FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Brown, ED Hopkins, MJG AF Brown, ED Hopkins, MJG TI How New Guinea rainforest flower resources vary in time and space: Implications for nectarivorous birds SO AUSTRALIAN JOURNAL OF ECOLOGY LA English DT Article DE flowering pattern; honeyeaters; lorikeets; nectarivory; phenology; rainforest; spatial pattern ID LOWLAND TROPICAL RAINFOREST; RAIN-FOREST; PHYLIDONYRIS-NOVAEHOLLANDIAE; AUSTRALIAN HONEYEATERS; HOLLAND HONEYEATER; BANKSIA-MENZIESII; SOUTH-AUSTRALIA; SCRUB JAYS; COMMUNITY; POLLINATION AB Variability in spatial and temporal patterning of flowering by populations of rainforest trees fed upon by honeyeaters and flower-visiting parrots was studied for 2 years in lowland tropical hill forest in Papua New Guinea. All 2200 trees in a 3 ha plot were tagged, identified, mapped and monitored monthly. Of 274 tree species present, 86 flowered during the course of the study; during any given month, approximately 20% of the species flowering that month were visited by nectarivorous birds. Results showed that overall flower resources (total number of species, and number of bird-pollinated species, individuals and flowers) fluctuated during the year, decreased during the dry season and increased during the wet season. In addition, there was a wide range of temporal variation within and among tree species in length and timing of flowering period, percentage of each conspecific population flowering from year to year, and degree of synchrony among flowering conspecifics. Spatial dispersion of tree populations also varied, from clumps to scattered single individuals. Resident bird species were correlated with synchronously flowering trees, whereas nomadic bird species were correlated with asynchronously flowering trees. Resident birds were also associated with smaller blooming displays per tree, whereas nomadic birds were associated with trees that bloomed massively. There was no correlation between avian nomadism and spatial dispersion of tree populations. Thus nomadic birds seem to range in search of rich but unpredictable resources; resident birds may rely more on predictable, but smaller resources. C1 UNIV PAPUA NEW GUINEA,DEPT BIOL,WAIGANI,PAPUA N GUINEA. RP Brown, ED (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DIV BIRDS,WASHINGTON,DC 20560, USA. NR 51 TC 16 Z9 17 U1 1 U2 10 PU BLACKWELL SCIENCE PI CARLTON PA 54 UNIVERSITY ST, P O BOX 378, CARLTON VICTORIA 3053, AUSTRALIA SN 0307-692X J9 AUST J ECOL JI Aust. J. Ecol. PD DEC PY 1996 VL 21 IS 4 BP 363 EP 378 DI 10.1111/j.1442-9993.1996.tb00623.x PG 16 WC Ecology SC Environmental Sciences & Ecology GA WF182 UT WOS:A1996WF18200002 ER PT J AU Krause, GH Winter, K AF Krause, GH Winter, K TI Photoinhibition of photosynthesis in plants growing in natural tropical forest gaps. A chlorophyll fluorescence study SO BOTANICA ACTA LA English DT Article DE chlorophyll fluorescence; photoinhibition; photosystem II; photosynthetic electron transport; tropical forest ID PHOTOSYSTEM-II; XANTHOPHYLL-CYCLE; LEAVES; CHLOROPLASTS; TURNOVER; CANOPY; LIGHT; COMPONENTS; MECHANISMS; RECOVERY AB Photoinhibition of photosynthesis was monitored by means of chlorophyll a fluorescence in leaves of plants growing in 60-80 m(2) light gaps in a moist tropical lowland forest located on Barro Colorado Island in central Panama. In these forest gaps, photon flux density was low (less than 100 mu mol photons m(-2) s(-1)) during most of the day, but increased on clear days to 1.7 - 1.8 mmol photons m(-2) s(-1) for 1 - 2 h during midday. Nine species representing different taxa and life-forms were examined. Leaves of all species exhibited substantial photoinhibition in situ during high light exposure, as manifested by a decrease in the ratio of variable to maximum fluorescence emission, F-V/F-M. Recovery (reversion of fluorescence quenching) took place in the shade following high light exposure. The major part of recovery occurred in a fast phase within about 1 h after the high light period. A slow phase of recovery proceeded for another 4-5 h until sunset. After 30-60 min of recovery in the shade, calculated rates of PSII electron transport remained significantly (5-15%) reduced in comparison to rates obtained prior to high light exposure; after about 2 h of recovery, inhibition was negligible. All species responded to the high light periods and following shade periods in a very similar manner. It is concluded that photoinhibition and recovery exhibited by these gap leaves reflect a dynamic regulatory mechanism of thermal energy dissipation that allows plants of different life-forms to cope with periods of high light in tropical forest gaps. C1 SMITHSONIAN TROP RES INST,PANAMA CITY,BALBOA,PANAMA. RP Krause, GH (reprint author), UNIV DUSSELDORF,INST PLANT BIOCHEM,UNIV STR 1,D-40225 DUSSELDORF,GERMANY. NR 28 TC 49 Z9 53 U1 0 U2 9 PU GEORG THIEME VERLAG PI STUTTGART PA P O BOX 30 11 20, D-70451 STUTTGART, GERMANY SN 0932-8629 J9 BOT ACTA JI Bot. Acta PD DEC PY 1996 VL 109 IS 6 BP 456 EP 462 PG 7 WC Plant Sciences SC Plant Sciences GA WB466 UT WOS:A1996WB46600003 ER PT J AU Stuart, J AF Stuart, J TI Fruitful sites: Garden culture in Ming dynasty China - Clunas,C SO CHINA QUARTERLY LA English DT Book Review RP Stuart, J (reprint author), SMITHSONIAN INST, FREER GALLERY ART, WASHINGTON, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0305-7410 J9 CHINA QUART JI China Q. PD DEC PY 1996 IS 148 BP 1393 EP 1395 PG 3 WC Area Studies SC Area Studies GA XE465 UT WOS:A1996XE46500040 ER PT J AU Ralls, K Demaster, DP Estes, JA AF Ralls, K Demaster, DP Estes, JA TI Developing a criterion for delisting the southern sea otter under the US endangered species act SO CONSERVATION BIOLOGY LA English DT Article ID POPULATION VIABILITY ANALYSIS; VALDEZ OIL-SPILL; EXXON-VALDEZ; RECOVERY PLANS; CONSERVATION AB Recent surveys of recovery plans indicate that criteria, such as population sizes, for delisting species from the U.S. Endangered Species Act (ESA) are often unrealistically low by scientific standards. We describe the delisting criterion for the threatened southern sea otter (Enhydra lutris nereis) developed by the Southern Sea Otter Recovery Team. A major oil spill is the most serious threat to this sea otter population. After extensive modeling of oil spills, the recovery team concluded that it was not scientifically defensible to develop a delisting criterion in terms of a single probability of extinction over a specified time period. Instead, the team decided to define a size at which it would consider the population endangered and to consider the population threatened as long as a major oil spill might reduce it to that size. The effective population size (N-e) for endangered status was set at 500, estimated to be about 1850 otters. Using a spill the size of the Exxon Valdez spill (250,000 bbl), the oil spill model was iterated to generate a frequency distribution of the number of sea otters contacted by oil, from which the team estimated that less than 800 otters would be killed by 90% of the simulated spills. Thus, the delisting criterion was set at 1850 + 800 = 2650 individuals. There have been several proposals to improve the Endangered Species Act by providing quantitative guidance, in the form of specific probabilities of extinction within some time frame or specific criteria like those used by the Wordl Conservation Union as to the levels of extinction risk represented by the terms ''threatened'' and ''endangered''. Experiences of the Sea Otter Recovery Team indicate that guidelines should not be overly rigid and should allow flexibility for dealing with specific situations. The most important consideration is to appoint a recovery team that is both technically well qualified and unconstrained by pressures from management agencies. C1 NATL MARINE MAMMAL LAB,SEATTLE,WA 98115. UNIV CALIF SANTA CRUZ,INST MARINE SCI,NATL BIOL SERV,SANTA CRUZ,CA 95064. RP Ralls, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 34 TC 18 Z9 19 U1 3 U2 22 PU BLACKWELL SCIENCE INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD DEC PY 1996 VL 10 IS 6 BP 1528 EP 1537 DI 10.1046/j.1523-1739.1996.10061528.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA VY245 UT WOS:A1996VY24500007 ER PT J AU Ryan, MJ Rand, AS Weigt, LA AF Ryan, MJ Rand, AS Weigt, LA TI Allozyme and advertisement call variation in the tungara frog, Physalaemus pustulosus SO EVOLUTION LA English DT Article DE advertisement calls; allozyme variation; genetic variation; geographical variation; Physalaemus pustulosus; sexual selection; tungara frog ID EPHIPPIGER-EPHIPPIGER ORTHOPTERA; FEMALE MATE CHOICE; SEXUAL SELECTION; SENSORY EXPLOITATION; GEOGRAPHIC-VARIATION; SPECIES RECOGNITION; POECILIA-RETICULATA; MATING PREFERENCES; NEOTROPICAL FROG; ACRIS-CREPITANS AB We analyzed variation in advertisement calls and allozymes in 30 populations along a 5000-km transect throughout most of the range of the tungara frog, Physalaemus pustulosus. All 12 call variables measured show significant differences among populations despite the importance of the advertisement call in species recognition. Some call variables exhibited clinal variation, whereas most others differed between the two major allozyme groups that have invaded Panama at different times, perhaps 4-4.5 million yr apart. Call variables that primarily affect discrimination among conspecifics tended to exhibit greater variation than call variables that are crucial for species recognition. The proximate mechanism of production underlying a call variable, however, is a better predictor of its variation. Contrary to predictions of some sexual selection models, carl Variation exhibits predictable patterns of geographical variation, although a substantial portion of variation among populations is not explained by geographic position. Although allozymes, calls, and geography usually covary, closer populations can have more similar calls independent of allozyme similarity. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP Ryan, MJ (reprint author), UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712, USA. NR 71 TC 93 Z9 96 U1 2 U2 12 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 SN 0014-3820 J9 EVOLUTION JI Evolution PD DEC PY 1996 VL 50 IS 6 BP 2435 EP 2453 DI 10.2307/2410711 PG 19 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA WB946 UT WOS:A1996WB94600028 ER PT J AU Stanley, DJ Chen, ZY AF Stanley, DJ Chen, ZY TI Neolithic settlement distributions as a function of sea level-controlled topography in the Yangtze delta, China SO GEOLOGY LA English DT Article ID EASTERN CHINA; SUBSIDENCE; INITIATION AB Combined geological and archaeological data sets indicate that sea level-controlled topography best explains the timing of Neolithic settlement onto the southern Yangtze delta plain, almost 1500 yr later than inland China, Information on settlement patterns of the three major Neolithic cultures (Ma-Jia-Bang, Song-Ze, Liang-Zhu), dated from ca. 5500 to 2200 B,C,, is provided by petrologic study of habitat bases of sites and of sediment cores recovered near the sites. In the early Holocene, rising sea level induced decreased relief and an aggrading silt mantle on the low-lying delta surface, Changes of sea level and climate from early to mid-Holocene initiated a fertile delta plain at ca. 6000-5500 B.C,, and settlement and cultivation, including rice, began within only 500 yr of delta formation, Rate of sea-level rise decelerated by mid-Holocene time, resulting in rising ground-water level and poor drainage, and a reduced delta plain area suitable for human occupation and agriculture, As a consequence, Neolithic settlements shifted progressively eastward toward higher, more restricted areas of the Yangtze delta chenier plain. C1 E CHINA NORMAL UNIV,DEPT GEOG,SHANGHAI 200062,PEOPLES R CHINA. RP Stanley, DJ (reprint author), SMITHSONIAN INST,NMNH E207,DELTAS GLOBAL CHANGE PROGRAM,WASHINGTON,DC 20560, USA. NR 21 TC 59 Z9 66 U1 2 U2 9 PU GEOLOGICAL SOC AMERICA PI BOULDER PA PO BOX 9140 3300 PENROSE PLACE, BOULDER, CO 80301 SN 0091-7613 J9 GEOLOGY JI Geology PD DEC PY 1996 VL 24 IS 12 BP 1083 EP 1086 DI 10.1130/0091-7613(1996)024<1083:NSDAAF>2.3.CO;2 PG 4 WC Geology SC Geology GA VZ942 UT WOS:A1996VZ94200007 ER PT J AU Herken, G AF Herken, G TI Impacts of the early cold war on the formulation of US science policy: Selected memoranda of William T. Golden, October 1950 April 1951 - Golden,WT SO ISIS LA English DT Book Review RP Herken, G (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,DEPT SPACE HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0021-1753 J9 ISIS JI Isis PD DEC PY 1996 VL 87 IS 4 BP 755 EP 755 DI 10.1086/357712 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA WE160 UT WOS:A1996WE16000088 ER PT J AU Rybicki, GB AF Rybicki, GB TI Radiative transfer SO JOURNAL OF ASTROPHYSICS AND ASTRONOMY LA English DT Article AB Chandrasekhar's work in radiative transfer theory began in 1944 and culminated with the publication of his influential treatise Radiative Transfer in 1950. In this review his major contributions to radiative transfer will be recounted and evaluated. These include his development of the discrete ordinates method, the invariance principles, and his formulation and solution of the transfer equation for polarized light. RP Rybicki, GB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 55 TC 5 Z9 5 U1 0 U2 0 PU INDIAN ACADEMY SCIENCES PI BANGALORE PA P B 8005 C V RAMAN AVENUE, BANGALORE 560 080, INDIA SN 0250-6335 J9 J ASTROPHYS ASTRON JI J. Astrophys. Astron. PD DEC PY 1996 VL 17 IS 3-4 BP 95 EP 112 DI 10.1007/BF02702299 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WM420 UT WOS:A1996WM42000005 ER PT J AU Chai, P Harrykissoon, R Dudley, R AF Chai, P Harrykissoon, R Dudley, R TI Hummingbird hovering performance in hyperoxic heliox: Effects of body mass and sex SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE air density; body mass; heliox; hovering flight; hummingbird; hyperoxia; muscle power; oxygen consumption; sexual dimorphism; Archilochus colubris ID INSECT FLIGHT; OXYGEN-CONSUMPTION; AERODYNAMICS; BIRDS; ENERGY; POWER; LIMITS; PHYSIOLOGY; ENERGETICS; METABOLISM AB Owing to their small size and hovering locomotion, hummingbirds are the most aerobically active vertebrate Can hyperoxia enhance the flight of this highly oxygen-dependent group? Hovering performance of ruby-throated hummingbirds (Archilochus colubris) was manipulated non-invasively using hyperoxic but hypodense gas mixtures of sea-level air combined with heliox containing 35 % O-2. This manipulation sheds light on the interplay among metabolic power input, mechanical power output and aerodynamic force production in limiting flight performance. No significant differences in flight mechanics and oxygen consumption were identified between hyperoxic and normoxic conditions. Thus, at least in the present experimental context, hyperoxia did not change the major metabolic and mechanical parameters; O-2 diffusive capacities of the respiratory system were probably not limiting to a significant extent. Compared with hummingbirds in our previous studies, the present experimental birds were heavier, had resultant shorter hover-feeding durations and experienced aerodynamic failure at higher air densities. Because hummingbirds have relatively stable wingbeat frequencies, modulation of power output was attained primarily through variation in stroke amplitude up to near 180 degrees. This result indicates that maximum hovering performance was constrained geometrically and that heavier birds with greater fat loads had less margin for enhancement of power production. Sexual dimorphism in flight adaptation also played a role, with males showing more limited hovering capacities, presumably as a trade-off for increased maneuverability. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RP Chai, P (reprint author), UNIV TEXAS, DEPT ZOOL, AUSTIN, TX 78712 USA. NR 67 TC 30 Z9 30 U1 1 U2 9 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 EI 1477-9145 J9 J EXP BIOL JI J. Exp. Biol. PD DEC PY 1996 VL 199 IS 12 BP 2745 EP 2755 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VX954 UT WOS:A1996VX95400020 PM 9110957 ER PT J AU Faust, MA Morton, SL Quod, JP AF Faust, MA Morton, SL Quod, JP TI Further SEM study of marine dinoflagellates: The genus Ostreopsis (Dinophyceae) SO JOURNAL OF PHYCOLOGY LA English DT Article DE Belize; benthic dinoflagellates; coral reef Dinophyceae; ecology; Japan; Mauritius, Mayotte Islands; morphology; Ostreopsis heptagona; Ostreopsis labens; Ostreopsis lenticularis; Ostreopsis mascarenensis; Ostreopsis ovata; Ostreopsis siamensis; Peridiniales; Puerto Rico; Reunion Island; scanning electron microscopy; taxonomy; toxicity ID SP-NOV DINOPHYCEAE; GAMBIERDISCUS-TOXICUS; CORAL-REEFS; MORPHOLOGY AB This paper presents a comprehensive examination of the taxonomy of the genus Ostreopsis Schmidt. The morphology of six species of marine dinoflagellates, Ostreopsis siamensis Schmidt 1902, Ostreopsis lenticularis Fukuyo 1981, Ostreopsis ovata Fukuyo 1981, Ostreopsis heptagona Norris, Bomber, et Balech 1985, Ostreopsis mascarenensis Quod 1994, and Ostreopsis labens Faust et Morton 1995 from three geographical regions (Japan, Southwest Indian Ocean, and the Caribbean) and three marine habitats (sand, water column, and macroalgal surfaces) are described from scanning electron micrographs. Differences in the following morphological characteristics differentiated the species: cell shape and size, and ornamentation of the epitheca, cingulum, and hypotheca. The thecal plate formula of the six Ostreopsis species is P-0, 3', 7'', 6C, 6S?, V-p, R(p), 5''', 1p, 2'''', with differences in thecal plate size and shape. The cingulum in ventral view has two prominent structures: a ventral plate (V-p) with a ventral pore (V-0) and a ridged plate (R(p)) that distinguishes Ostreopsis species from any other dinoflagellate taxa. This paper also includes ecological and toxicity information regarding the six Ostreopsis species. C1 SO ILLINOIS UNIV,DEPT PLANT BIOL,CARBONDALE,IL 62901. LAB ARVAM,F-97490 ST CLOTILDE,REUNION. RP Faust, MA (reprint author), SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT BOT,SUITLAND,MD 20746, USA. NR 43 TC 62 Z9 67 U1 0 U2 17 PU PHYCOLOGICAL SOC AMER INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD DEC PY 1996 VL 32 IS 6 BP 1053 EP 1065 DI 10.1111/j.0022-3646.1996.01053.x PG 13 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA WB441 UT WOS:A1996WB44100022 ER PT J AU BaileyGoldschmidt, J Kalfatovic, MC Kalfatovic, MR AF BaileyGoldschmidt, J Kalfatovic, MC Kalfatovic, MR TI ''I remember it well'': Paul Bern, Jean Harlow, and the negotiation of information SO JOURNAL OF POPULAR CULTURE LA English DT Article C1 SMITHSONIAN INST LIBRARIES,WASHINGTON,DC. RP BaileyGoldschmidt, J (reprint author), UNIV PENN,DEPT ANTHROPOL,PHILADELPHIA,PA 19104, USA. OI Kalfatovic, Martin/0000-0002-4563-4627 NR 15 TC 0 Z9 0 U1 0 U2 1 PU BOWLING GREEN POPULAR PRESS PI BOWLING GREEN PA C/O RAY B BROWNE, BOWLING GREEN STATE UNIV, BOWLING GREEN, OH 43403 SN 0022-3840 J9 J POP CULT JI J. Pop. Cult. PD WIN PY 1996 VL 30 IS 3 BP 223 EP 235 DI 10.1111/j.0022-3840.1996.00223.x PG 13 WC Humanities, Multidisciplinary; Cultural Studies SC Arts & Humanities - Other Topics; Cultural Studies GA XM895 UT WOS:A1996XM89500016 ER PT J AU Olson, SL Hasegawa, Y AF Olson, SL Hasegawa, Y TI A new genus and two new species of gigantic plotopteridae from Japan (Aves: Pelecaniformes) SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article AB The Plotopteridae are wing-propelled, penguin-like diving birds of the order Pelecaniformes Found in mid-Tertiary deposits of the North Pacific. Much new material representing a considerable radiation of genera and species has been discovered in Japan since the basic adaptations and characters of the family were revealed. A new genus and species, Copepteryx hexeris, is named here from previously known but underscribed material upon which much of our knowledge of the family had originally been based. A second new species, C. titan, is described from a single gigantic femur from a bird that was probably larger than any known diving bird, living or fossil. C1 GUNMA MUSEUM NAT HIST,TOMIOKA,GUNMA,JAPAN. RP Olson, SL (reprint author), NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 10 TC 22 Z9 24 U1 0 U2 1 PU SOC VERTEBRATE PALEONTOLOGY PI CHICAGO PA 401 NORTH MICHIGAN AVE, CHICAGO, IL 60611-4267 SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD DEC PY 1996 VL 16 IS 4 BP 742 EP 751 PG 10 WC Paleontology SC Paleontology GA WM073 UT WOS:A1996WM07300013 ER PT J AU Emry, RJ Korth, WW AF Emry, RJ Korth, WW TI The Chadronian squirrel ''Sciurus'' jeffersoni Douglass, 1901: A new generic name, new material, and its bearing on the early evolution of Sciuridae (Rodentia) SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID OLIGOCENE AB A new genus, Douglassia, is erected for the problematic Chadronian sciurid Sciurus jeffersoni Douglass, 1901. Previously undescribed material adds new morphologic information for the taxon. Douglassia differs from other sciurids in the retention of primitive dental and masseteric morphology. Based on postcranial anatomy, the genus is referred to the Tribe Sciurini (tree squirrels), which is regarded as the sister taxon to all other Sciurinae. The known fossil material of Tertiary flying squirrels is inadequate to determine whether they constitute a distinct family. C1 ROCHESTER INST VERTEBRATE PALEONTOL, PENFIELD, NY 14526 USA. RP Emry, RJ (reprint author), SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT PALEOBIOL, WASHINGTON, DC 20560 USA. NR 29 TC 19 Z9 21 U1 0 U2 4 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD DEC PY 1996 VL 16 IS 4 BP 775 EP 780 PG 6 WC Paleontology SC Paleontology GA WM073 UT WOS:A1996WM07300017 ER PT J AU Kennedy, MA Ramsay, E Diderrich, V Richman, L Allen, GP Potgieter, LND AF Kennedy, MA Ramsay, E Diderrich, V Richman, L Allen, GP Potgieter, LND TI Encephalitis associated with a variant of equine herpesvirus 1 in a Thomson's gazelle (Gazella thomsoni) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE equine herpesvirus 1; encephalitis; gazelle; Gazella thomsoni; case report ID TYPE-1; ABORTION; ZEBRA AB A captive Thomson's gazelle (Gazella thomsoni) died after an acute neurologic illness characterized by depression, recumbency, and seizures. Histopathologic changes in the brain consisted of mild subacute nonsuppurative perivascular meningoencephalitis. Equine herpesvirus 1 was isolated from pooled brain and lung tissue. The virus was genetically distinct from isolates recovered from domestic equids but was similar to isolates from an onager and a zebra herd. This is the first report of equine herpesvirus 1 infection associated with neurologic disease in a ruminant and may represent the isolation of a new equine herpesvirus 1 variant. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT PATHOL,WASHINGTON,DC 20008. UNIV KENTUCKY,DEPT VET SCI,LEXINGTON,KY 40546. RP Kennedy, MA (reprint author), UNIV TENNESSEE,DEPT COMPARAT MED,KNOXVILLE,TN 37901, USA. NR 13 TC 14 Z9 14 U1 0 U2 1 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD DEC PY 1996 VL 27 IS 4 BP 533 EP 538 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA WJ066 UT WOS:A1996WJ06600011 ER PT J AU Birchard, GF Marcellini, D AF Birchard, GF Marcellini, D TI Incubation time in reptilian eggs SO JOURNAL OF ZOOLOGY LA English DT Review ID CROCODYLUS-NILOTICUS; OXYGEN-CONSUMPTION; AVIAN EGG; TEMPERATURE; WATER; METABOLISM; MAMMALS; EMBRYOS; LIZARD; REPRODUCTION AB An allometric analysis of reptilian incubation time was performed. Incubation time increased with increasing egg mass (allometric exponent = 0.14, r(2) = 0.31). However, significant heterogeneity was found within the Reptilia for this character. If periods of developmental arrest are excluded the orders Crocodylia, Testudinata, and the suborder Serpentes have the shortest incubation times and the lizards the longest. Significant differences within lizard families were also observed (Iguanidae, Agamidae, Gekkonidae, and Lacertidae have shorter incubation times than the Varanidae and Teiidae). Preliminary analyses indicate the heterogeneity in incubation time observed within the Squamata is correlated with differences in brain mass; this is similar to findings for mammals. The variation in incubation time indicates the existence of differences in growth rates in reptilian groups and suggests a partial explanation for the observed distribution of viviparity within the Squamata. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT HERPETOL,WASHINGTON,DC 20008. RP Birchard, GF (reprint author), GEORGE MASON UNIV,DEPT BIOL,FAIRFAX,VA 22030, USA. NR 129 TC 14 Z9 14 U1 0 U2 9 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD, ENGLAND OX2 6DP SN 0952-8369 J9 J ZOOL JI J. Zool. PD DEC PY 1996 VL 240 BP 621 EP 635 PN 4 PG 15 WC Zoology SC Zoology GA VZ961 UT WOS:A1996VZ96100003 ER PT J AU Hoare, MG Drake, JJ Werner, K Dreizler, S AF Hoare, MG Drake, JJ Werner, K Dreizler, S TI The extreme-ultraviolet spectrum of the central star of the planetary nebula NGC 1360 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars, AGB and post-AGB; stars, atmospheres; stars, fundamental parameters; white dwarfs; planetary nebulae, individual, NGC 1360; X-rays, stars ID IRON-GROUP ELEMENTS AB We have used the Extreme Ultraviolet Explorer (EUVE) to obtain the first EUV spectrum of the central star of a planetary nebula, that of NGC 1360. The photospheric spectrum shows continuum absorption edges due to O4+ as well as absorption-line features. NLTE model atmospheres including line blanketing by iron-group elements can match the general level and shape of the spectrum, but are not capable of explaining all the observed features, precluding a detailed fit. Our solar abundance models require T-eff = 110000 K, log g=6.0 and N-H = 8.5 x 10(19) cm(-2). A new optical spectrum is presented and analysed with NLTE models. Stellar parameters in reasonable agreement with the EW results are derived. it is found that many optical lines need to be considered, otherwise the best fits are not necessarily unique. This data set will provide a stern test for future NLTE models, which will need to include still more Line blanketing before a totally satisfactory fit is obtained. C1 UNIV LEEDS,DEPT PHYS & ASTRON,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. UNIV CALIF BERKELEY,CTR EUV ASTROPHYS,BERKELEY,CA 94720. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV POTSDAM,LEHRSTUHL ASTROPHYS,D-14469 POTSDAM,GERMANY. CHRISTIAN ALBRECHTS UNIV KIEL,INST ASTRON & ASTROPHYS,D-24098 KIEL,GERMANY. RP Hoare, MG (reprint author), MAX PLANCK INST ASTRON,KONIGSTUHL 17,D-69117 HEIDELBERG,GERMANY. NR 25 TC 13 Z9 13 U1 1 U2 1 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 1996 VL 283 IS 3 BP 830 EP 836 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VY727 UT WOS:A1996VY72700019 ER PT J AU Schartel, N Green, PJ Anderson, SF Hewett, PC Foltz, CB Margon, B Brinkmann, W Fink, H Trumper, J AF Schartel, N Green, PJ Anderson, SF Hewett, PC Foltz, CB Margon, B Brinkmann, W Fink, H Trumper, J TI ROSAT soft X-ray properties of the Large Bright Quasar Survey: Modelling of stacked X-ray spectra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies, active; quasars, general; X-rays, galaxies ID OPTICALLY SELECTED QUASARS; HIGH-REDSHIFT QUASARS; ACTIVE GALACTIC NUCLEI; QSO SURVEY; EQUATORIAL FIELDS; RADIO PROPERTIES; ABSORPTION; CATALOG; OBJECTS AB We develop and apply a novel method of analysis to study the X-ray spectral properties of 908 QSOs in the Large Bright Quasar Survey (LBQS) that were observed during the soft X-ray ROSAT All-Sky Survey (RASS), Due to the relatively short (less than or equal to 600 s) RASS exposure times, only 10 per cent of the QSOs are detected in X-rays, so X-ray spectral model fits for individual QSOs are precluded by poor photon statistics. Spectral stacking provides effectively much more sensitive X-ray observations for an average QSO in bins of redshift, and for several classes of QSOs. We model the stacked X-ray spectra in st way that obviates both the distinction between detections and non-detections, and the need to stack together only those objects observed through similar Galactic column densities N-H. In application to the LBQS/RASS sample, we marginally confirm a flattening of the X-ray spectral index of QSOs toward higher redshifts. Radio-loud QSOs show flatter X-ray photon indices, in agreement with previous work. We show that the apparent flattening of the photon index with redshift is not due to an increasing fractional contribution from the radio-loud class of QSOs. C1 MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195. UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. UNIV ARIZONA,MULTIPLE MIRROR TELESCOPE OBSERV,TUCSON,AZ 85721. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Schartel, N (reprint author), IUE OBSERV,ESA,POB 50727,E-28080 MADRID,SPAIN. RI Margon, Bruce/B-5913-2012 NR 52 TC 28 Z9 28 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 1996 VL 283 IS 3 BP 1015 EP 1026 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VY727 UT WOS:A1996VY72700035 ER PT J AU Gallegos, CL Vant, WN Safi, KA AF Gallegos, CL Vant, WN Safi, KA TI Microzooplankton grazing of phytoplankton in Manukau Harbour, New Zealand SO NEW ZEALAND JOURNAL OF MARINE AND FRESHWATER RESEARCH LA English DT Article DE phytoplankton; microzooplankton; grazing; dilution experiments; Manukau Harbour ID GROWTH; DYNAMICS; PACIFIC; IMPACT; SEA; BAY AB Grazing by microzooplankton on phytoplankton in Manukau Harbour was measured by size-fractionated dilution experiments at monthly intervals from October 1994 to October 1995. Grazing rates were always highest on the < 5 mu m size fraction, the smallest size fraction measured. These rates ranged from 0.3 to 1.3 d(-1) and were highest in November and March; values did not appear to vary with grazer abundance. Grazing rates on the < 5 mu m phytoplankton exceeded growth rate by more than a factor of two in June when growth rate was seasonally depressed; but for most of the year the grazing rate averaged about 90% of growth rate. Grazing rates on the 5-22 mu m phytoplankton were lower in magnitude, and were a lower percentage of phytoplankton growth rate than those on the < 5 mu m size fraction. Grazing on the > 22 mu m phytoplankton was measurable only during the February bloom of the large diatom Odontella sinensis. The grazing rate was low, being a small percentage of phytoplankton growth rate in that size fraction. Mathematical simulation of the growth of the < 5 mu m phytoplankton in the harbour showed that the observed grazing rates were sufficient to prevent this size fraction from blooming. RP Gallegos, CL (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. OI Gallegos, Charles/0000-0001-5112-0166 NR 28 TC 34 Z9 34 U1 0 U2 2 PU SIR PUBLISHING PI WELLINGTON PA PO BOX 399, WELLINGTON, NEW ZEALAND SN 0028-8330 J9 NEW ZEAL J MAR FRESH JI N. Z. J. Mar. Freshw. Res. PD DEC PY 1996 VL 30 IS 4 BP 423 EP 434 PG 12 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA WC951 UT WOS:A1996WC95100002 ER PT J AU Maitra, NT Heller, EJ AF Maitra, NT Heller, EJ TI Semiclassical perturbation approach to quantum reflection SO PHYSICAL REVIEW A LA English DT Article AB We consider the problem of quantum ''reflection above the barrier,'' introducing a distorted-wave Born approximation based on the primitive semiclassical Wentzel-Kramers-Brillouin wave function. The idea generalizes to the concept of an unperturbed Hamiltonian defined as the exact Hamiltonian plus small parts which ''turn off'' nonclassical processes such as barrier reflection and barrier tunneling. C1 HARVARD UNIV,HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Maitra, NT (reprint author), HARVARD UNIV,DEPT PHYS,CAMBRIDGE,MA 02138, USA. NR 15 TC 28 Z9 29 U1 0 U2 2 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD DEC PY 1996 VL 54 IS 6 BP 4763 EP 4769 DI 10.1103/PhysRevA.54.4763 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA VX714 UT WOS:A1996VX71400026 ER PT J AU Yochelson, EL AF Yochelson, EL TI Discovery, collection, and description of the Middle Cambrian Burgess Shale Biota by Charles Doolittle Walcott SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Article ID CATHEDRAL ESCARPMENT; SHADOW RP Yochelson, EL (reprint author), SMITHSONIAN INST,NATL MUSEUM NATURAL HIST,DEPT PALEOBIOLOGY,WASHINGTON,DC, USA. NR 45 TC 4 Z9 4 U1 1 U2 3 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 SN 0003-049X J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD DEC PY 1996 VL 140 IS 4 BP 469 EP 545 PG 77 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA WB126 UT WOS:A1996WB12600004 ER PT J AU Kurin, R Hunt, M AF Kurin, R Hunt, M TI In the service of the presidency - Workers' culture at the White-House SO PROLOGUE-QUARTERLY OF THE NATIONAL ARCHIVES LA English DT Article RP Kurin, R (reprint author), SMITHSONIAN INST,CTR FOLKLIFE PROGRAMS & CULTURAL STUD,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ARCHIVES RECORDS ADMINISTRATION PI WASHINGTON PA TRUST FUND BOARD, WASHINGTON, DC 20408 SN 0033-1031 J9 PROLOGUE JI Prologue-Q. Natl. Archives PD WIN PY 1996 VL 28 IS 4 BP 271 EP & PG 0 WC History SC History GA WJ358 UT WOS:A1996WJ35800003 ER PT J AU COLLINS, MJ AF COLLINS, MJ TI NASA - A HISTORY OF THE UNITED-STATES-CIVIL-SPACE-PROGRAM - LAUNIUS,RD SO PUBLIC HISTORIAN LA English DT Book Review RP COLLINS, MJ (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD WIN PY 1996 VL 18 IS 1 BP 130 EP 132 PG 3 WC History SC History GA UA237 UT WOS:A1996UA23700033 ER PT J AU Bonnell, JT Nemiroff, RJ Goldstein, JJ AF Bonnell, JT Nemiroff, RJ Goldstein, JJ TI The Scale of the Universe debate in 1996 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB On April 21, 1996, Sidney van den Bergh and Gustav Tammann engaged in a public debate titled ''The Scale of the Universe.'' The arguments they presented focused on recently determined and still controversial values of the Hubble Constant. The program was moderated by John Bahcall, with lectures on the background and history behind humanity's quest for the scale of the Universe given by Owen Gingerich and Virginia Trimble. These introductory lectures along with the arguments presented by the 1996 debaters are recreated in the following papers. This debate was of the same title and held in the same auditorium as the ''Great Debate'' between Heber Curtis and Harlow Shapley in 1920. Here we discuss some of the issues surrounding the organization and inspiration for the 1996 debate, Like the 1920 debate, the 1996 debate was not intended to resolve a disagreement instantly. Instead it is hoped that this debate and the written contributions will stand as educational tools, summarizing the arguments behind today's Hubble Constant controversy, and will help provide a framework for evaluating progress in this field as the century which saw its creation draws to a close. Together with last year's debate, ''The Distance Scale to Gamma Ray Bursts'' (Nemiroff, R. J. 1995, PASP, 107, 1131), these papers may also provide a clue as to how scientists think. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. NR 4 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 1996 VL 108 IS 730 BP 1065 EP 1067 DI 10.1086/133835 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VY121 UT WOS:A1996VY12100001 ER PT J AU Gingerich, O AF Gingerich, O TI The scale of the universe: A curtain raiser in four acts and four morals SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB This concise and highly selective introduction to the distance-scale debate, from antiquity to Hubble's paper of 1924 on the distance to M31, provides some key quotations and references. The first section describes the early Creek determinations of the distances of the Sun and Moon. The second part discusses the distances to the stars, from Copernicus to Huygens. Section 3 skips to the early twentieth-century ideas on the scale of the Milky Way, especially the work of Shapley. The final section describes how Hubble's discovery of distances to galaxies was first announced. RP Gingerich, O (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 35 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 1996 VL 108 IS 730 BP 1068 EP 1072 DI 10.1086/133836 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VY121 UT WOS:A1996VY12100002 ER PT J AU Robinson, H AF Robinson, H TI The Paralychnophora group of Eremanthus (Vernonieae: Asteraceae) SO RHODORA LA English DT Article DE Asteraceae; Compositae; Vernonieae; Eremanthus; Paralychnophora ID COMPOSITAE; REVISION AB The species placed in Paralychnophora by MacLeish are returned to the genus Eremanthus, and two related species, E. harleyi and E. santosii, are described as new. RP Robinson, H (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 8 TC 8 Z9 11 U1 0 U2 0 PU NEW ENGLAND BOTANICAL CLUB INC PI LAWRENCE PA P.O. BOX 368, LAWRENCE, KS 66044 SN 0035-4902 J9 RHODORA JI Rhodora PD WIN PY 1996 VL 98 IS 893 BP 85 EP 93 PG 9 WC Plant Sciences SC Plant Sciences GA WW027 UT WOS:A1996WW02700003 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI DISCovering multicultural America SO RQ LA English DT Database Review RP Kalfatovic, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER LIBRARY ASSN PI CHICAGO PA 50 E HURON ST, CHICAGO, IL 60611 SN 0033-7072 J9 RQ JI RQ PD WIN PY 1996 VL 36 IS 2 BP 282 EP 283 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA WH286 UT WOS:A1996WH28600014 ER PT J AU Heyman, IM AF Heyman, IM TI Smithsonian perspectives + 'Red, Hot & Blue', a new exhibition saluting the American musical, is an invigorating example of the Smithsonian's mission to illuminate our past SO SMITHSONIAN LA English DT Editorial Material RP Heyman, IM (reprint author), SMITHSONIAN INST,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD DEC PY 1996 VL 27 IS 9 BP 18 EP 18 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA VX736 UT WOS:A1996VX73600001 ER PT J AU Burke, K AF Burke, K TI Ruined by reading: A life in books - Schwartz,LS SO SMITHSONIAN LA English DT Book Review RP Burke, K (reprint author), SMITHSONIAN INST,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD DEC PY 1996 VL 27 IS 9 BP 137 EP 137 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA VX736 UT WOS:A1996VX73600017 ER PT J AU Swofford, DL Thorne, JL Felsenstein, J Wiegmann, BM AF Swofford, DL Thorne, JL Felsenstein, J Wiegmann, BM TI The topology-dependent permutation test for monophyly does not test for monophyly SO SYSTEMATIC BIOLOGY LA English DT Editorial Material ID SEQUENCE DATA; PHYLOGENIES; PROBABILITY; PARSIMONY; LIMITS; CHANCE C1 N CAROLINA STATE UNIV,DEPT STAT,PROGRAM STAT GENET,RALEIGH,NC 27695. UNIV WASHINGTON,DEPT GENET,SEATTLE,WA 98195. N CAROLINA STATE UNIV,DEPT ENTOMOL,RALEIGH,NC 27695. RP Swofford, DL (reprint author), SMITHSONIAN INST,LAB MOL SYSTEMAT,MRC-534,WASHINGTON,DC 20560, USA. NR 17 TC 46 Z9 47 U1 0 U2 2 PU SOC SYSTEMATIC BIOLOGISTS PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY NHB 163, WASHINGTON, DC 20560 SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD DEC PY 1996 VL 45 IS 4 BP 575 EP 579 DI 10.2307/2413533 PG 5 WC Evolutionary Biology SC Evolutionary Biology GA WK350 UT WOS:A1996WK35000011 ER PT J AU Lefebvre, G Poulin, B AF Lefebvre, G Poulin, B TI Seasonal abundance of migrant birds and food resources in Panamanian mangrove forests SO WILSON BULLETIN LA English DT Article ID OVERWINTERING NEARCTIC MIGRANTS; VENEZUELAN MANGROVES; LAND BIRDS; WARBLERS; BEHAVIOR; DIETS AB We studied temporal variation in abundance of Nearctic-Neotropical migrants, particularly the Northern Waterthrush (Seiurus noveboracensis), Prothonotary Warbler (Protonotaria citrea), and American Redstart (Setophaga ruticilla) in two black mangrove sites of central Panama from September 1993 through May 1995. The two sites, on the Caribbean and the Pacific coasts, differ importantly in annual rainfall, tide amplitude, and seasonal invertebrate abundance. Most migrant species varied temporally in abundance with the opposite pattern at each site, suggesting mid-winter movements correlated with abundance of food resources. Because of their wide geographic distribution and their particular response to hydrographic factors, mangroves are likely to have a temporally complementary role in sustaining migrant populations throughout the Neotropics. However, variations in migrant numbers reported in other Neotropical habitats could also reflect large-scale movements by migrants. Occurrence of mid-winter (facultative) migration has been documented mostly for the Palearctic-African migratory system, and needs to be investigated in the Nearctic-Neotropical realm for proper conservation of migratory species. C1 SMITHSONIAN TROP RES INST,ANCON,PANAMA. NR 40 TC 23 Z9 25 U1 1 U2 11 PU WILSON ORNITHOLOGICAL SOC PI ANN ARBOR PA MUSEUM OF ZOOLOGY UNIV MICHIGAN, ANN ARBOR, MI 48109 SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD DEC PY 1996 VL 108 IS 4 BP 748 EP 759 PG 12 WC Ornithology SC Zoology GA WC226 UT WOS:A1996WC22600012 ER PT J AU Mueller, UG AF Mueller, UG TI Evolution of social insect colonies. Sex allocation and kin selection - Crozier,RH, Pamilo,P SO SCIENCE LA English DT Book Review C1 UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742. RP Mueller, UG (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 1 TC 0 Z9 0 U1 3 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD NOV 29 PY 1996 VL 274 IS 5292 BP 1477 EP 1478 DI 10.1126/science.274.5292.1477 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VV775 UT WOS:A1996VV77500028 ER PT J AU Rosenthal, ED Gurwell, MA Ho, PTP AF Rosenthal, ED Gurwell, MA Ho, PTP TI Efficient detection of brown dwarfs using methane-band imaging SO NATURE LA English DT Article AB BROWN dwarfs lie in the mass range between the most massive Jupiter-like planets and the least massive stars, They are much less luminous than stars, and so may provide a fraction of the baryonic dark matter in our Galaxy, Only one unambiguous detection of a brown dwarf has been made to date(1-6)-Gl229B, a low-mass companion to the nearby star Gl229A, The detection(4) of strong methane-band absorption in the spectrum of Gl229B, a feature restricted to cool substellar objects(5-9), lends weight to the idea(7) that differential methane-band imaging (the subtraction of an image taken in the methane band from a continuum-light image taken in the same spectral region) should provide an efficient method for detecting brown dwarfs. Here we demonstrate the potential of this approach by obtaining an image of Gl229B with less than two minutes of integration time. This technique promises efficient detection of both isolated brown dwarfs in crowded regions, and brown dwarfs orbiting close to their primary stars. RP Rosenthal, ED (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 34 Z9 34 U1 0 U2 1 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD NOV 21 PY 1996 VL 384 IS 6606 BP 243 EP 244 DI 10.1038/384243a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VU381 UT WOS:A1996VU38100043 ER PT J AU Zhao, JH Anantharamaiah, KR Goss, WM Viallefond, F AF Zhao, JH Anantharamaiah, KR Goss, WM Viallefond, F TI Radio recombination lines from the nuclear regions of starburst galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, nuclei; galaxies, starburst; galaxies, stellar content; radio lines, galaxies ID INFRARED-LUMINOUS GALAXIES; MOLECULAR CLOUDS; STAR-FORMATION; NEUTRAL HYDROGEN; SPIRAL GALAXIES; BRIGHT GALAXIES; BRACKETT-ALPHA; OH-MEGAMASER; IC 4553; ARP 220 AB Using the Very Large Array (VLA) with an angular resolution of 3 '', we have detected the hydrogen recombination line H92 alpha from the galaxies Arp 220, M83, and NGC 2146. The line emission arises from the nuclear regions with a line-to-continuum ratio of 1% or less. In order to fit both the observed H92 alpha line and continuum data in the nuclear regions, we have considered two types of models. First, we utilize a model with a collection of H rr regions. A large number of compact H II regions are required in this model. With electron temperatures in the range 5 x 10(3)-1 x 10(4) K and a range of electron densities, this model can account for both the line intensity and the continuum spectrum. In most cases, the H92 alpha line is dominated by internal stimulated emission due to free-free continuum arising within the H II regions. In a low-density case (n(e) = 50 cm(-3)) for Arp 220, about half the line emission comes from external stimulated emission due to the background nonthermal source. Typical rates of ionizing photons predicted from these models are similar to 5 x 10(52) S-1 for M83, similar to 4 x 10(53) S-1 for NGC 2146, and 5 x 10(54) S-1 for Arp 220. We infer that 10(5) O5 stars are required in Arp 220, which is an order of magnitude greater than in NGC 2146 and 2 orders of magnitude greater than in M83. Alternatively, several uniform slab models with T-e greater than or equal to 5 x 10(3) and n, in the range of 50-1 x 10(4) cm(-3) appear to fit both the H92 alpha line and continuum data of Arp 220 and M83. In the low-density models, stimulated emission by the background nonthermal radiation appears to be dominant at low frequencies, and the lines at higher frequencies arise primarily from spontaneous emission. The uniform slab model requires a higher ionizing photon rate than the H n region model. No slab models with reasonable T-e can fit the data observed in M83 and NGC 2146. Combining previous published data with these new observations, a sample of 13 galaxies has been observed for radio recombination lines (RRLs) with the VLA. Nine out of the 13 galaxies have been detected in the H92 alpha line. While the H92 alpha line luminosity appears to be correlated with the Bra line luminosity, we find that nearly all the RRL galaxies show a significant excess in H92 alpha line compared to the expected LTE value. The excess in the H92 alpha line flux suggests that non-LTE effects are important for the H92 alpha line in these starburst nuclei. A strong correlation between H92 alpha and the molecular lines of HCN/HCO+ is also found, indicating that the RRL emitters may be spatially associated with the dense molecular cores. The inferred high electron density also suggests an intimate relation between the RRLs and the dense molecular medium in these galaxies. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RAMAN RES INST, BANGALORE 560080, KARNATAKA, INDIA. NATL RADIO ASTRON OBSERV, SOCORRO, NM 87801 USA. OBSERV MEUDON, DEMIRM, F-92190 MEUDON, FRANCE. RP Zhao, JH (reprint author), ACAD SINICA, INST ASTRON & ASTROPHYS, POB 1-87, TAIPEI 115, TAIWAN. RI Anantharamaiah , K. R./E-5369-2012; M, Manjunath/N-4000-2014 OI M, Manjunath/0000-0001-8710-0730 NR 54 TC 39 Z9 39 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1996 VL 472 IS 1 BP 54 EP 72 DI 10.1086/178041 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU065 UT WOS:A1996VU06500006 ER PT J AU Laming, JM Raymond, JC McLaughlin, BM Blair, WP AF Laming, JM Raymond, JC McLaughlin, BM Blair, WP TI Electron-ion equilibration in nonradiative shocks associated with SN 1006 SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; ISM, individual (SN 1006); shock waves; supernova remnants ID HOPKINS-ULTRAVIOLET-TELESCOPE; RESOLVED LAYER; CYGNUS LOOP; HIGH-BETA; COLLISIONLESS DISSIPATION; IMPACT EXCITATION; SUPERNOVA REMNANT; CHARGE-EXCHANGE; IA SUPERNOVAE; X-RAY AB The ultraviolet spectrum of SN 1006 observed by the Hopkins Ultraviolet Telescope (HUT) is modeled to infer the degree of electron-ion equilibration at the nonradiative shocks in the remnant. Such an approach is possible since the spectrum has lines (He II lambda 1640) whose excitation is dominated by electrons, and others (C IV lambda 1550, N V lambda 1240, O VI lambda 1036) in which protons and other ions are more important, and the intensity ratio between these is sensitive to the electron-ion temperature ratio. We find substantially less than full equilibration, marginally consistent with existing plasma simulations but rather more suggestive of even lower equilibration than these studies would predict. The more stringent limits on the electron temperature resulting from this allow a more accurate determination of the distance to SN 1006. Our result is 1.8 +/- 0.3 kpc. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. USN,RES LAB,WASHINGTON,DC 20375. RP Laming, JM (reprint author), SFA INC,1401 MCCORMICK DR,LANDOVER,MD 20785, USA. NR 50 TC 107 Z9 108 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1996 VL 472 IS 1 BP 267 EP 274 DI 10.1086/178061 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU065 UT WOS:A1996VU06500026 ER PT J AU Buckley, JH Akerlof, CW Biller, S CarterLewis, DA Catanese, M Cawley, MF Connaughton, V Fegan, DJ Finley, JP Gaidos, J Hillas, AM Kartje, JF Konigl, A Krennrich, F Lamb, RC Lessard, R Macomb, DJ Mattox, JR McEnery, JE Mohanty, G Quinn, J Rodgers, AJ Rose, HJ Schubnel, MS Sembroski, GL Smith, PS Weekes, TC Wilson, C Zweerink, J AF Buckley, JH Akerlof, CW Biller, S CarterLewis, DA Catanese, M Cawley, MF Connaughton, V Fegan, DJ Finley, JP Gaidos, J Hillas, AM Kartje, JF Konigl, A Krennrich, F Lamb, RC Lessard, R Macomb, DJ Mattox, JR McEnery, JE Mohanty, G Quinn, J Rodgers, AJ Rose, HJ Schubnel, MS Sembroski, GL Smith, PS Weekes, TC Wilson, C Zweerink, J TI Gamma-ray variability of the BL Lacertae object markarian 421 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays, observations; BL Lacertae objects, individual (markarian 421) ID ACTIVE GALACTIC NUCLEI; X-RAY; RADIATION; EMISSION; BLAZARS; JETS AB We report on the gamma-ray variability of Mrk 421 at E(gamma) > 300 GeV during the 1995 season, and concentrate on the results of an intense multiwavelength observing campaign in the period April 20 to May 5, which included > 100 MeV gamma-ray, X-ray, extreme-ultraviolet, optical, and radio observations, some of which show evidence for correlated behavior. Rapid variations in the TeV gamma-ray light curve with doubling and decay times of less than or similar to 1 day require a compact emission region and significant Doppler boosting. The TeV data reveal that the gamma-ray emission is best characterized by a succession of rapid flares with a relatively low baseline level of steady emission. C1 UNIV MICHIGAN,RANDALL LAB PHYS,ANN ARBOR,MI 48109. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. IOWA STATE UNIV,DEPT PHYS & ASTRON,AMES,IA 50011. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. PURDUE UNIV,DEPT PHYS,W LAFAYETTE,IN 47907. UNIV CHICAGO,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637. NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. UNIV SPACE RES ASSOC,ASTROPHYS PROGRAM,GREENBELT,MD. UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. RP Buckley, JH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,FRED LAWRENCE WHIPPLE OBSERV,POB 97,AMADO,AZ 85645, USA. NR 44 TC 98 Z9 98 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1996 VL 472 IS 1 BP L9 EP L12 DI 10.1086/310352 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU067 UT WOS:A1996VU06700003 ER PT J AU Greenhill, LJ Gwinn, CR Antonucci, R Barvainis, R AF Greenhill, LJ Gwinn, CR Antonucci, R Barvainis, R TI VLBI imaging of water maser emission from the nuclear torus of NGC 1068 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, individual (NGC 1068); galaxies, kinematics and dynamics; galaxies, nuclei; masers ID ACTIVE GALACTIC NUCLEI; OBSCURING DUST TORI; INFRARED-SPECTRA; NGC-1068; GALAXIES; DISK; ACCELERATION; NGC-4258; QUASARS; REGION AB We have made the first VLBI synthesis images of the H2O maser emission associated with the central engine of the Seyfert galaxy NGC 1068. Emission extends about +/- 300 km s(-1) from the systemic velocity. Images with sub-milliarcsecond angular resolution show that the redshifted emission lies along an are to the northwest of the systemic emission. (The blueshifted emission has not yet been imaged with VLBI.) Based on the maser velocities and the relative orientation of the known radio jet, we propose that the maser emission arises on the surface of a nearly edge-on torus, where physical conditions are conducive to maser action. The visible part of the torus is axially thick, with comparable height and radius. The velocity field indicates sub-Keplerian differential rotation around a central mass of similar to 1 x 10(7) M. that lies within a cylindrical radius of about 0.65 pc. The estimated luminosity of the central engine is about 0.5 of the Eddington limit. There is no detectable compact radio continuum emission near the proposed center of the torus (T-B < 5 x 10(6) K on size scales of similar to 0.1 pc), so that the observed flat-spectrum core cannot be direct self-absorbed synchrotron radiation. C1 UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106. NEROC,HAYSTACK OBSERV,WESTFORD,MA 01886. RP Greenhill, LJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 36 TC 93 Z9 95 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1996 VL 472 IS 1 BP L21 EP & DI 10.1086/310346 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU067 UT WOS:A1996VU06700006 ER PT J AU Travers, MJ McCarthy, MC Kalmus, P Gottlieb, CA Thaddeus, P AF Travers, MJ McCarthy, MC Kalmus, P Gottlieb, CA Thaddeus, P TI Laboratory detection of the cyanopolyyne HC13N SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, molecules; line, identification; molecular data; molecular processes; radio lines, ISM ID HC9N AB The cyanopolyyne HC13N has been detected in the laboratory, and the frequency of 21 rotational transitions in the band 5-12 GHz has been measured to a few parts in 10(7); correspondingly precise values for the rotational constant and centrifugal distortion constant have been obtained from a least-squares fit to the data: B-0 = 106.97258(4) MHz, D-0 = 0.092(10) Hz (uncertainties in parentheses are la in the last significant digit). The best lines for astronomical detection of this carbon chain, longer than any yet detected in space, probably lie in the band 5-30 GHz and can be calculated from B-0 and D-0 to better than 0.1 km s(-1) in equivalent radial velocity. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Travers, MJ (reprint author), HARVARD UNIV,DIV APPL SCI,29 OXFORD ST,CAMBRIDGE,MA 02138, USA. NR 6 TC 9 Z9 9 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1996 VL 472 IS 1 BP L61 EP L62 DI 10.1086/310359 PN 2 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU067 UT WOS:A1996VU06700016 ER PT J AU Williams, HL Korona, T Bukowski, R Jeziorski, B Szalewicz, K AF Williams, HL Korona, T Bukowski, R Jeziorski, B Szalewicz, K TI Helium dimer potential from symmetry-adapted perturbation theory SO CHEMICAL PHYSICS LETTERS LA English DT Article ID CONFIGURATION-INTERACTION CALCULATIONS; HE-HE; DISPERSION COEFFICIENTS; MOLECULAR INTERACTIONS; INTERACTION ENERGIES; WEAKEST BOND; CONVERGENCE; DIPOLE; MODEL; ATOMS AB The intermolecular potential for the helium dimer has been computed using infinite-order symmetry-adapted perturbation theory and very large orbital and explicitly correlated basis sets. Our potential is significantly deeper than recent literature potentials, After adding the relativistic retardation correction, it accurately reproduces bulk properties of helium, the inclusion of retardation being essential for this agreement. Transport properties and virial coefficients are expected to be accurate enough to calibrate measuring apparatus. C1 ARMY RES LAB,WEAPONS TECHNOL DIRECTORATE,ABERDEEN PROVING GROUND,MD 21005. WARSAW UNIV,DEPT CHEM,PL-02093 WARSAW,POLAND. UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716. UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Williams, HL (reprint author), UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716, USA. RI Korona, Tatiana/E-8290-2011 OI Korona, Tatiana/0000-0001-7169-3412 NR 36 TC 50 Z9 51 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD NOV 15 PY 1996 VL 262 IS 3-4 BP 431 EP 436 DI 10.1016/0009-2614(96)01078-0 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA VT117 UT WOS:A1996VT11700041 ER PT J AU Janetzky, W Arbizu, PM Reid, JW AF Janetzky, W Arbizu, PM Reid, JW TI Attheyella (Canthosella) mervini sp n (Canthocamptidae, Harpacticoida) from Jamaican bromeliads SO HYDROBIOLOGIA LA English DT Article DE Attheyella (Canthosella) mervini; taxonomy; new species; Jamaica; phytotelmata ID COPEPODA AB In phytotelmata of Jamaican bromeliads the harpacticoid copepods Epactophanes richardi Mrazek, 1893, Phyllognathopus viguieri (Maupas, 1892) and Attheyella (Canthosella) mervini sp. n. occurred. The new species conforms to the diagnosis of the subgenus, despite the fact that the endopods of legs 2-4 have retained more setae than in the species known for the Asian region. Attheyella (Canthosella) mervini lacks setae on the baseoendopod of leg 5, which is characteristic for neotropical Canthosella-species. We propose that Attheyella (Chappuisiella) kalima (Delachaux, 1924), Attheyella (Ch.) aliena Noodt, 1956, Elaphoidella siolii Kiefer, 1967, and Canthocamptus (Elaphoidella) striblingi Reid, 1990 be included in the subgenus Attheyella (Canthosella). Additionally, Attheyella (Chappuisiella) kalima of Dussart & Frutos, 1986 is included in this subgenus, but we propose the name Attheyella (Canthosella) pilagaensis sp.n., because the species as described differs from the original description of A. (C.) kalima (Delachaux, 1924). C1 UNIV OLDENBURG,ICBM,AG AQUAT OKOL,D-26111 OLDENBURG,GERMANY. SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. OI Martinez-Arbizu, Pedro/0000-0002-0891-1154 NR 17 TC 11 Z9 11 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD NOV 15 PY 1996 VL 339 IS 1-3 BP 123 EP 135 DI 10.1007/BF00008920 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA WC904 UT WOS:A1996WC90400015 ER PT J AU Heller, EJ AF Heller, EJ TI Quantum proximity resonances SO PHYSICAL REVIEW LETTERS LA English DT Article ID CLASSICALLY CHAOTIC REPELLOR; SCATTERING; SYSTEMS; QUANTIZATION AB It is well known that at long wavelengths lambda an s-wave scatterer can have a scattering cross section sigma on the order of lambda(2), much larger than its physical size, as measured by the range of its potential. Very interesting phenomena can arise when two or more identical scatterers are placed close together, well within one wavelength. We show that, for a pair of identical scatterers, an extremely narrow p-wave ''proximity'' resonance develops from a broader s-wave resonance of the individual scatterers. A new s-wave resonance of the pair also appears. The relation of these proximity resonances (so called because they appear when the scatterers are close together) to the Thomas and Efimov effects is discussed. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. RP Heller, EJ (reprint author), HARVARD UNIV,DEPT PHYS,CAMBRIDGE,MA 02138, USA. NR 19 TC 31 Z9 31 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD NOV 11 PY 1996 VL 77 IS 20 BP 4122 EP 4125 DI 10.1103/PhysRevLett.77.4122 PG 4 WC Physics, Multidisciplinary SC Physics GA VR556 UT WOS:A1996VR55600004 ER PT J AU Lin, H Kirshner, RP Schectman, SA Landy, SD Oemler, A Tucker, DL Schechter, PL AF Lin, H Kirshner, RP Schectman, SA Landy, SD Oemler, A Tucker, DL Schechter, PL TI The power spectrum of galaxy clustering in the Las Campanas Redshift Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology-observations; galaxies-clusters-general; galaxies-distances and redshifts; large-scale structure of universe; methods-numerical ID LARGE-SCALE STRUCTURE; COLD DARK-MATTER; BACKGROUND-RADIATION ANISOTROPIES; IRAS GALAXIES; DENSITY PERTURBATIONS; LUMINOSITY FUNCTION; UNIVERSE; COBE; EVOLUTION; DISTANCES AB The Las Campanas Redshift Survey (LCRS) contains 23,697 galaxies, with an average redshift z = 0.1, distributed over six 1.degrees 5 x 80 degrees slices in the north and south galactic caps. We have computed the power spectrum P(k) for magnitude-limited samples of LCRS galaxies over wavelengths lambda = 2 pi/k = 5-400 h(-1) Mpc. The LCRS P(k) may be approximated as proportional to k(-1.8+/-0.1) for small scales lambda = 5-30 h(-1) Mpc, changing to proportional to k(1+/-1) for large scales lambda approximate to 200-400 h(-1) Mpc. The overall amplitude corresponds to sigma(8) = 1.0 +/- 0.1 in redshift space. Comparisons to the power spectra of other redshift surveys will be presented; the LCRS results agree best with those from the combined Center for Astrophysics (CfA2) and Southern Sky redshift surveys (SSRS2). For lambda greater than or similar to 100 h(-1) Mpc, the LCRS results are consistent with those of other surveys, given the large errors among all the surveys on these scales. For lambda less than or similar to 100 h(-1) Mpc, the LCRS P(k) is well determined and similar in shape to the P(k) of other surveys, but with an amplitude differing from some of the other samples, possibly because of inherent clustering differences among different types of galaxies. In particular, power spectrum measurements for volume-limited LCRS samples show that galaxies brighter than about M*-1 appear about 50% more strongly clustered than those fainter. Also, a sample of LCRS emission galaxies shows 30% weaker clustering than the full LCRS sample. Comparisons to N-body models show that the LCRS power spectrum lies intermediate between that of a standard flat Omega(0) h = 0.5 cold dark matter (CDM) model and an open Omega(0) h = 0.2 model, both normalized to sigma(8) = 1 for galaxies. On large scales lambda greater than or similar to h 40 h(-1) Mpc, we have fit the LCRS results to various linear CDM models, and find that a number of them could meet the constraints set by the LCRS power spectrum, the Hubble constant range 0.5 less than or similar to h less than or similar to 0.8, the abundance of galaxy clusters, and the reasonable assumption that LCRS galaxies are roughly unbiased tracers of the mass, relative to the normalization provided by the 4 year COBE DMR data. The possibilities include open CDM or flat nonzero cosmological-constant CDM models with Omega(0) approximate to 0.4-0.6 and shape parameter Gamma approximate to Omega(0) h approximate to 0.2-0.3, as well as flat Omega(0) = 1 models with massive neutrino density Omega(v) approximate to 0.2-0.3 or a spectral tilt n approximate to 0.7-0.8. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. CARNEGIE OBSERV, PASADENA, CA 91101 USA. YALE UNIV, DEPT ASTRON, NEW HAVEN, CT 06520 USA. INST ASTROPHYS, D-14482 POTSDAM, GERMANY. MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. NR 74 TC 109 Z9 109 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1996 VL 471 IS 2 BP 617 EP 635 DI 10.1086/177993 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VR611 UT WOS:A1996VR61100006 ER PT J AU Churazov, E Gilfanov, M Forman, W Jones, C AF Churazov, E Gilfanov, M Forman, W Jones, C TI Mapping the gas temperature distribution in extended X-ray sources and spectral analysis in the case of low statistics: Application to ASCA observations of clusters of galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies-clusters-general; methods-data analysis; methods-statistical; X-rays-galaxies ID ASTRONOMY AB A simple method for mapping the temperature distribution in extended sources is developed for application to ASCA observations of galaxy clusters. Unlike the conventional approach to spatially resolved spectral analysis, this method does not require nonlinear minimization and is computationally fast and stable. Therefore, it can be implemented for a large number of regions or on a fine spatial grid. Although based on a Taylor expansion over the nonlinear parameter, the method is found to be accurate in many practical situations, the relative error for the temperature estimate being less than 2%-4% when the plasma temperature exceeds similar to 2 keV. This method is not intended to replace conventional spectral analysis but to supplement it, providing relatively fast and easy construction of temperature maps, which may be used as a guide to further detailed analysis of particularly interesting regions using conventional spectral fitting. Conventional spectral analysis in the case of moderate and low numbers of counts is discussed. A practical recipe for unbiased parameter estimation is suggested and verified in Monte Carlo simulations for commonly used spectral models. A simple modification of the chi(2) statistic (calculation of weights based on the smoothed observed spectrum) yields nearly unbiased parameter estimates and correct confidence interval determination with no need for regrouping (binning) the energy channels even in the case of low statistics (similar to 50-100 counts in the observed spectrum with several hundred channels). C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP Churazov, E (reprint author), SPACE RES INST,PROFSOUZNAYA 84-32,MOSCOW 117810,RUSSIA. RI Churazov, Eugene/A-7783-2013 NR 4 TC 79 Z9 80 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1996 VL 471 IS 2 BP 673 EP 682 DI 10.1086/177997 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VR611 UT WOS:A1996VR61100010 ER PT J AU Carone, TE Peterson, BM Bechtold, J Bertram, R Bischoff, K Dietrich, M Filippenko, AV Ho, LC Huchra, JP Kollatschny, W Korista, KT Matheson, T Pogge, RW Shields, JC Smith, PS Wagner, RM Wilkes, BJ AF Carone, TE Peterson, BM Bechtold, J Bertram, R Bischoff, K Dietrich, M Filippenko, AV Ho, LC Huchra, JP Kollatschny, W Korista, KT Matheson, T Pogge, RW Shields, JC Smith, PS Wagner, RM Wilkes, BJ TI Optical continuum and emission-line variability of the Seyfert 1 galaxy Markarian 509 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, individual (Markarian 509); galaxies, Seyfert ID ACTIVE GALACTIC NUCLEI; REGION; SIZE; STEPS; NGC-5548; NGC-4151; WAVELENGTHS; EVOLUTION; ACCURACY; NGC-3227 AB We report on the results of a 5 year coordinated program of spectroscopic monitoring of the luminous Seyfert 1 galaxy Markarian 509. The H beta and He II lambda 4686 emission lines are found to respond to continuum variations with time lags of similar to 80 and similar to 60 days, respectively, considerably longer than the emission-line lags measured for other Seyfert galaxies. C1 UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. OHIO STATE UNIV, DEPT ASTRON, COLUMBUS, OH 43210 USA. UNIV STERNWARTE GOTTINGEN, D-37083 GOTTINGEN, GERMANY. UNIV CALIF BERKELEY, DEPT ASTRON, BERKELEY, CA 94720 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. CARNEGIE INST WASHINGTON OBSERV, PASADENA, CA 91101 USA. UNIV KENTUCKY, DEPT PHYS & ASTRON, LEXINGTON, KY 40506 USA. KONIGSTUHL, LANDESSTERNWARTE, D-69117 HEIDELBERG, GERMANY. OI Wilkes, Belinda/0000-0003-1809-2364 NR 36 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1996 VL 471 IS 2 BP 737 EP 747 DI 10.1086/178002 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VR611 UT WOS:A1996VR61100015 ER PT J AU Seward, FD Kearns, KE Rhode, KL AF Seward, FD Kearns, KE Rhode, KL TI ROSAT observations of two southern supernova remnants SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual (Kesteven 27, G327.4+0.4, G327.1-1.1); supernovae remnants; X-rays, ISM AB The supernova remnants G327.1-1.1 and G327.4+0.4 (Kes 27) are located 1.degrees 5 apart in the constellation Norma. In 1980, Einstein IPC observations discovered that both were irregular filled-center X-ray sources with possible point sources superposed. This paper describes new ROSAT PSPC observations which both map the diffuse structure and clearly show several unresolved sources in each held. Both remnants have bright emitting regions inside the limb which might indicate the presence of high-energy electrons accelerated by a pulsar. The interior region is more prominent in G327.1-1.1 than in Kes 27. The spectra are relatively strongly absorbed, as expected from distant remnants close to the Galactic plane. Comparison of the X-ray and radio maps of each remnant allows us to attribute some emission to a shell and some to the interior. With this information, a blast-wave model is used to derive approximate ages and energy release. Indications are that the Kes 27 supernova deposited similar to 10(51) ergs in the surrounding medium. The G327.1-1.1 event probably deposited a factor of 3-10 less. C1 WESLEYAN UNIV,DEPT ASTRON,MIDDLETOWN,CT 06459. RP Seward, FD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 17 TC 13 Z9 13 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1996 VL 471 IS 2 BP 887 EP 896 DI 10.1086/178015 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VR611 UT WOS:A1996VR61100028 ER PT J AU Proga, D Kenyon, SJ Raymond, JC Mikolajewska, J AF Proga, D Kenyon, SJ Raymond, JC Mikolajewska, J TI Illumination in symbiotic binary stars: Non-LTE photoionization models .1. Hydrostatic case SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, symbiotic; radiative transfer; stars, emission-line, Be; stars, late-type ID EMISSION-LINE SPECTRUM; NOVA AG-PEGASI; X-RAY; MASS-LOSS; STELLAR ATMOSPHERES; COOL COMPONENTS; URSAE-MAJORIS; EG-ANDROMEDAE; RADIO SURVEY; GIANT STARS AB We describe a non-LTE photoionization code that calculates the atmospheric structure and emergent spectrum of a red giant illuminated by the hot component of a symbiotic binary system. The model assumes hydrostatic, radiative, and statistical equilibrium for the red giant atmosphere and solves the radiative transfer equation with a local escape probability method. We compute non-LTE level populations for a variety of ions and predict the variation of emission-line fluxes as function of the temperature and luminosity of the hot component. Our models produce strong emission lines only when the hot component has a high effective temperature, T-h greater than or similar to 100,000 K, for hot component luminosities, L(h) greater than or similar to 630 L.. Predicted electron densities and temperatures for the photoionized atmosphere agree with observations. The models also produce reasonably large continuum variations that are consistent with the light curves of some symbiotic stars. However, predictions for most optical and ultraviolet emission-line fluxes fall well below those observed in typical symbiotic stars. We conclude that the hot component must illuminate a red giant wind to reproduce observed line fluxes. Hydrostatic red giant atmospheres simply do not have enough material beyond the photosphere to account for the emission features observed in most symbiotics. Illumination can modify the structure of a red giant atmosphere even when the emitted spectrum changes very little. Energetic photons from the hot component cause the atmosphere to expand by several percent for large hot component luminosities. This expansion is insufficient to increase the red giant mass-loss rate, except in systems where the giant already fills or nearly fills its Roche lobe. C1 COPERNICUS ASTRON CTR,PL-00716 WARSAW,POLAND. RP Proga, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 79 TC 29 Z9 29 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1996 VL 471 IS 2 BP 930 EP 948 DI 10.1086/178020 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VR611 UT WOS:A1996VR61100033 ER PT J AU Zaccheo, TS Karovska, M Cook, JW Howard, RA Brueckner, GE Korendyke, CM Schwenn, R AF Zaccheo, TS Karovska, M Cook, JW Howard, RA Brueckner, GE Korendyke, CM Schwenn, R TI Enhancing the spatial resolution of solar coronagraph observations using dynamic imaging SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation, miscellaneous; space vehicles; Sun, corona; techniques, image processing AB The Large Angle Spectrometric Coronagraph (LASCO) C1 coronagraph on board the Solar and Heliospheric Observatory (SOHO) is designed to image the corona from 1.1 to 3.0 R.. The resolution of C1 is defined by the size of its CCD pixels, which correspond to 5''.6, and not by the diffraction limit of the optical system, which may be as small as 3''. The resolution of C1 can be improved using the technique of ''dynamic imaging''-the process of acquiring successive images of the same scene using sub-pixel displacements of the steerable primary mirror. We developed a technique we call the fractional pixel restoration (FPR) algorithm that utilizes these observations to construct an image with improved resolution. Simulations were used to test this algorithm and to explore its limitations. We also applied the direct co-addition and FPR algorithms to laboratory preflight images of a wire mesh grid. These results show that the resolution of the C1 coronagraph can be significantly enhanced, even in the presence of noise and modest differences between successive images. In some cases, the results can even reach the diffraction limit of the telescope. C1 USN,RES LAB,EO HULBURT CTR SPACE RES,WASHINGTON,DC 20375. MAX PLANCK INST AERON,D-37189 KATLENBURG DUHM,GERMANY. RP Zaccheo, TS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 11 TC 1 Z9 1 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1996 VL 471 IS 2 BP 1058 EP & DI 10.1086/178033 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VR611 UT WOS:A1996VR61100046 ER PT J AU Stoner, RE Rosenberry, MA Wright, JT Chupp, TE Oteiza, ER Walsworth, RL AF Stoner, RE Rosenberry, MA Wright, JT Chupp, TE Oteiza, ER Walsworth, RL TI Demonstration of a two species noble gas maser SO PHYSICAL REVIEW LETTERS LA English DT Article ID ELECTRIC-DIPOLE MOMENT; SPIN-EXCHANGE; VIOLATION; NEUTRON; ATOMS; HE-3 AB We have demonstrated the first two species maser. Ensembles of He-3 and Xe-129 gas, co-located in a double-chamber glass cell, performed simultaneous maser oscillations on their nuclear spin-1/2 Zeeman transitions. This new device may be used for experiments requiring precision magnetometry combined with frequency measurement of a second free-running species operating in the same volume. For example, the He-3 maser may serve as a magnetometer, while the Xe-129 maser may be used to search for a permanent electric dipole moment of the Xe-129 atom as a test of time reversal symmetry. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV MICHIGAN,DEPT PHYS,ANN ARBOR,MI 48109. OI Stoner, Richard/0000-0001-7949-6747 NR 19 TC 31 Z9 32 U1 0 U2 4 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD NOV 4 PY 1996 VL 77 IS 19 BP 3971 EP 3974 DI 10.1103/PhysRevLett.77.3971 PG 4 WC Physics, Multidisciplinary SC Physics GA VQ147 UT WOS:A1996VQ14700008 ER PT J AU DellAntonio, IP Bothun, GD Geller, MJ AF DellAntonio, IP Bothun, GD Geller, MJ TI Peculiar velocities for galaxies in the Great Wall .1. The data SO ASTRONOMICAL JOURNAL LA English DT Article ID TULLY-FISHER RELATION; SPIRAL GALAXIES; DISTANCE SCALE; H-I; SUPERCLUSTER; CLUSTERS; SCATTER; CATALOG; SAMPLE; WIDTH AB We construct the I-band Tully-Fisher relation (IRTF) for a sample of galaxies in the redshift space vicinity of the Great Wall. We measure isophotal and total I-band magnitudes for the galaxies and use the Arecibo 305 m to obtain 20% and 50% linewidths for the galaxies. We construct TF relations from these data. The derived TF zero point for this relation is M(0)=-19.73, and the TF slope is b=8.34, with scatter sigma similar to 0.30-0.32. We use the 20% linewidth relation for a study of the peculiar velocity field in a separate paper [Dell'Antonio er al. 1996, ApJ, submitted (Paper II)]. We also investigate the effects of extinction on the IRTF. The data are consistent with a moderate internal extinction (Bothun et al. 1992, ApJ, 395, 347), and are inconsistent with the strong internal extinction correction proposed by Bernstein ct al. (1994, AJ, 107, 1962). (C) 1996 American Astronomical Society. C1 UNIV OREGON,DEPT PHYS,EUGENE,OR 97403. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP DellAntonio, IP (reprint author), AT&T BELL LABS,LUCENT TECHNOL,700 MT AVE,MURRAY HILL,NJ 07974, USA. NR 35 TC 8 Z9 8 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 1759 EP 1779 DI 10.1086/118139 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600001 ER PT J AU DellAntonio, IP Geller, MJ Bothun, GD AF DellAntonio, IP Geller, MJ Bothun, GD TI Peculiar velocities for galaxies in the Great Wall .2. Analysis SO ASTRONOMICAL JOURNAL LA English DT Article ID ASTROPHYSICS REDSHIFT SURVEY; LOCAL GROUP; ELLIPTICAL GALAXIES; LUMINOSITY FUNCTION; DISTANCE SCALE; WIDTH RELATION; IRAS GALAXIES; COMA CLUSTER; MOTION; SUPERCLUSTER AB We analyze the peculiar velocity field in the vicinity of the Great Wall (GW) using a sample of 172 spiral galaxies with reliable IRTF distance estimates (Dell'Antonio et nl. 1996). We examine three main issues: (1) the infall onto the GW, (2) large-scale flow, and (3) shear. We use a Monte Carlo method to remove selection-based biases from the peculiar velocity sample. For the GW sample, the velocity bias is small (less than or similar to 150 km s(-1)). We use the bias-corrected velocities to constrain the infall towards the Great Wall. We thus have the first limits on the true spatial thickness of this structure. The data are best fit by an infall velocity less than or equal to 150 km s(-1). The 90% upper limit on the mean infall velocity is similar to 500 km s(-1). Consequently, the upper limit on the real-space full width of the GW is d<11.2h(-1) Mpc. Thus, the Great Wall is a thin, two-dimensional structure in real space as well as in redshift space. We calculate the best-fit estimate of the motion of the Local Group with respect to the galaxy distribution: upsilon(flow)similar to 725+/-400 km s(-1) towards alpha=11.7+/-1.5 hr, delta=36.8 degrees+/-55 degrees. Because our delta constraints are quite weak, this flow is consistent with the CMB dipole (Smoot ef al. 1992) and with the flow vector of Riess et al. (1995). The data are also consistent at the 25% confidence level with the direction of large-scale flow reported by Lauer & Postman (1994). We calculate the improvement in sensitivity expected for a sample extending over the full declination range of the GW. We also calculate the shear across the right ascension range of the GW. The GW region is quiet: the detected the shear across the range of the GW is -70+/-210 km s(-1). The absence of large shear constrains the amplitude of large-scale density fluctuations (Feldman & Watkins 1995). (C) 1996 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV OREGON,DEPT PHYS,EUGENE,OR 97403. RP DellAntonio, IP (reprint author), AT&T BELL LABS,LUCENT TECHNOL,700 MT AVE,MURRAY HILL,NJ 07974, USA. NR 37 TC 8 Z9 8 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 1780 EP 1793 DI 10.1086/118140 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600002 ER PT J AU Marzke, RO Huchra, JP Geller, MJ AF Marzke, RO Huchra, JP Geller, MJ TI Large-scale structure at low galactic latitude SO ASTRONOMICAL JOURNAL LA English DT Review ID SURFACE-BRIGHTNESS GALAXIES; 8000 KM S(-1); PISCES-PERSEUS SUPERCLUSTER; GREAT-ATTRACTOR REGION; SKY REDSHIFT SURVEY; H-I OBSERVATIONS; IRAS GALAXIES; MILKY-WAY; NEUTRAL HYDROGEN; OPTICAL GALAXIES AB We have extended the CfA Redshift Survey to low galactic latitudes to investigate the relation between the Great Wall in the North Galactic Cap and the Perseus-Pisces chain in the South Galactic Cap. We present redshifts for 2020 galaxies in the Catalogue of Galaxies and of Clusters of Galaxies (Zwicky et al. 1961-68, CGCG) in the following regions: 4(h) less than or equal to alpha less than or equal to 8(h), 17(h) less than or equal to alpha less than or equal to 20(h), 0 degrees less than or equal to delta less than or equal to 45 degrees. In these regions, the redshift catalogue includes 1664 galaxies with B(0)less than or equal to 15.5 (of which 820 are newly measured) and is 97% complete. We also include redshifts for an additional 356 galaxies in these regions with B(0)>15.5; of these, 148 were previously unmeasured. The CGCG samples the galaxy distribution down to b(II)similar or equal to 10 degrees. In this paper, we discuss the acquisition and reduction of the spectra, and we examine the qualitative features of the redshift distribution. The Great Wall and the Perseus-Pisces chain are not simply connected across the Zone of Avoidance. These structures, which at first appear to be coherent on scales of similar to 100h(-1) Mpc or more, actually form the boundaries of neighboring voids of considerably smaller scale, approximately 50h(-1) Mpc. The structures delineated by our optically-selected sample are qualitatively similar to those detected by the far-infrared-selected IRAS 1.2 Jansky Survey (Fisher ct al. 1995). Although the IRAS survey probes more deeply into the Zone of Avoidance, our optically-selected survey provides better sampling of structures at b(II)greater than or equal to 10 degrees. (C) 1996 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Marzke, RO (reprint author), NATL RES COUNCIL CANADA,HERZBERG INST ASTROPHYS,DOMINION ASTROPHYS OBSERV,5071 W SAANICH RD,VICTORIA,BC V8X 4M6,CANADA. NR 112 TC 40 Z9 40 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 1803 EP & DI 10.1086/118142 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600004 ER PT J AU Mohr, JJ Geller, MJ Wegner, G AF Mohr, JJ Geller, MJ Wegner, G TI A dynamical analysis of the poor galaxy clusters Abell 2626 and Abell 2440 SO ASTRONOMICAL JOURNAL LA English DT Article ID X-RAY; RICH CLUSTERS; LUMINOSITY FUNCTIONS; COMA CLUSTER; MASS; GAS; SUBSTRUCTURE; CENTAURUS; PERSEUS; CATALOG AB We use 189 new radial velocities and R band CCD photometry to study the galaxy clusters Abell 2626 and Abell 2440. By combining these new optical constraints with archival x-ray images and gas temperature measurements, we investigate the dynamical nature of both systems. We derive masses, luminosity functions, and mass-to-light ratios. The symmetric x-ray emission from A2626 suggests a relaxed, single-component system; however, our sample of 159 redshifts reveals a complex, three-component cluster at cz similar to 17 500 km/s. One of these components is a typical x-ray bright cluster, a second has a cluster-like galaxy population with a much lower central galaxy and gas density, and the third is a background structure with field galaxy composition. A comparison of the magnitude distributions within the two subclusters suggests that A2626 is a merger in progress (at 93% confidence). Virial masses and a composite luminosity function for a region with projected radius r=1.5h(-1) Mpc yield a mass-to-light ratio M/L(R) similar to 610h. Analysis of the x-ray emission from the primary component yields a gas mass function of similar to 2.2h(-3/2)% and a baryon fraction of similar to 3.4%. A radial infall model indicates that the virial mass may be an underestimate. The bimodal x-ray emission and elongated galaxy distribution of A2440 have been studied before (Baler 1979; Beers et nl. 1991). With deeper, CCD R band photometry we demonstrate a striking correspondence between the galaxy and cluster gas distributions. The galaxy distribution has three main components, each associated with a giant elliptical galaxy. The two larger peaks in the galaxy distribution coincide with the primary peaks in the x-ray emission, and the third is associated with a significant x-ray surface brightness enhancement. We use this galaxy-gas correspondence, 48 redshifts, and the structure of the x-ray emission to argue that the subclusters are bound within a single system, and that the two primary components are beginning to merge. The composite luminosity function and estimates of the subcluster virial masses indicate a mass-to-light ratio in the range M/L(R)=660h to 880h. (C) 1996 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. DARTMOUTH COLL,DEPT PHYS & ASTRON,HANOVER,NH 03755. RP Mohr, JJ (reprint author), UNIV MICHIGAN,DEPT PHYS & ASTRON,ANN ARBOR,MI 48109, USA. NR 60 TC 23 Z9 23 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 1816 EP 1828 DI 10.1086/118144 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600006 ER PT J AU Barth, AJ Reichert, GA Filippenko, AV Ho, LC Shields, JC Mushotzky, RF Puchnarewicz, EM AF Barth, AJ Reichert, GA Filippenko, AV Ho, LC Shields, JC Mushotzky, RF Puchnarewicz, EM TI The ultraviolet spectrum of the liner NGC 4579 SO ASTRONOMICAL JOURNAL LA English DT Article ID ACTIVE GALACTIC NUCLEI; X-RAY; GALAXIES; EMISSION; QUASARS; ORIGIN; HYPOTHESIS; CONTINUUM; SHOCKS; MODELS AB We present a Hubble Space Telescope ultraviolet spectrum of the LINER nucleus of NGC 4579, spanning the wavelength range 1160-3270 Angstrom. The data reveal a low-excitation spectrum of narrow (FWHM approximate to 1200 km s(-1)) and broad (FWHM approximate to 6600 km s(-1)) emission lines, which provide new diagnostics of the physical conditions within the emission-line regions, A featureless ultraviolet continuum is detected unambiguously, with f(n)u proportional to nu(-1.0) over the range 1300-2200 Angstrom and nu(-2.4) over 2200-3000 Angstrom. The 2200 Angstrom continuum flux is a factor of 3.3 lower than the value reported by Maoz et al, (1995) based on an HST image taken 19 months earlier; this is the first time that UV variability has been discovered in a LINER. The predictions of fast shock models are incompatible with the narrow-line spectrum, because the high-excitation lines produced in fast shocks are weak or absent in NGC 4579, Models of a single slab of gas photoionized by a power-law spectrum do not reproduce the observed line ratios well either, and it appears that the narrow-line region cannot be characterized by a unique value of the ionization parameter, We argue that the narrow-line region is photoionized by the central UV/X-ray source, and that more sophisticated photoionization calculations, incorporating the effects of density and/or ionization stratification and different continuum shapes, can yield results in better agreement with the data. (C) 1996 American Astronomical Society. C1 NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD 20771 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UCL, MULLARD SPACE SCI LAB, DORKING RH5 6NT, SURREY, ENGLAND. RP Barth, AJ (reprint author), UNIV CALIF BERKELEY, DEPT ASTRON, 601 CAMPBELL HALL, BERKELEY, CA 94720 USA. OI Barth, Aaron/0000-0002-3026-0562 NR 49 TC 42 Z9 42 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 1829 EP 1838 DI 10.1086/118145 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600007 ER PT J AU Hora, JL Deutsch, LK Hoffmann, WF Fazio, GG AF Hora, JL Deutsch, LK Hoffmann, WF Fazio, GG TI Mid-infrared imaging of the bipolar nebulae AFGL 618, AFGL 2688, and AFGL 915 SO ASTRONOMICAL JOURNAL LA English DT Article ID PROTO-PLANETARY-NEBULAE; MICRON EMISSION FEATURES; RADIO-CONTINUUM; RED RECTANGLE; REFLECTION NEBULAE; EVOLVED STARS; ARRAY CAMERA; CRL-2688; EVOLUTION; SPECTRA AB We have obtained nearly diffraction-limited images of three bipolar proto-planetary nebulae: AFGL 618, AFGL 2688 (the ''Egg nebula''), and AFGL 915 (the ''Red Rectangle''), Images were taken at unidentified infrared (UIR) emission feature wavelengths and at several continuum wavelengths in the 10 and 20 mu m atmospheric windows. In all three nebulae the emission is dominated by a central point source, In AFGL 618, evidence for a slight (0.1 ''-0.2 '') extension of the core in the E-W direction is seen. In AFGL 2688 and AFGL 915, the cores are extended and fainter emission is detected several arcsec from the central peaks. In AFGL 2688, the mid-IR emission is extended in the same direction as the main optical and near-IR lobes, In AFGL 915, the nebula is seen to follow the optical and near-IR bicone morphology. The ''spikes'' that have been observed at 2 mu m and give the nebula its rectangular appearance are also visible at 10 mu m. The UIR feature emission is spatially separate from the central source and is enhanced along the walls of the bicone. In all three nebulae, the direction of largest spatial extension is along the major axis as defined by the optical and near-infrared morphology. Therefore the mid-infrared emission appears to be tracing material in the bipolar outflow regions, rather than detecting structure related to an equatorial density enhancement that presumably is collimating the flow. (C) 1996 American Astronomical Society. C1 BOSTON UNIV, DEPT ASTRON, BOSTON, MA 02215 USA. UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. RP Hora, JL (reprint author), UNIV HAWAII, INST ASTRON, 2680 WOODLAWN DR, HONOLULU, HI 96822 USA. OI Hora, Joseph/0000-0002-5599-4650 NR 65 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 2064 EP 2075 DI 10.1086/118163 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600025 ER PT J AU Tamura, M Ohashi, N Hirano, N Itoh, Y MoriartySchieven, GH AF Tamura, M Ohashi, N Hirano, N Itoh, Y MoriartySchieven, GH TI Interferometric observations of outflows from low-mass protostars in Taurus SO ASTRONOMICAL JOURNAL LA English DT Article ID SUBMILLIMETER-WAVELENGTH OBSERVATIONS; L1551 MOLECULAR OUTFLOW; FORMING DENSE CORES; CIRCUMPROTOSTELLAR ENVIRONMENTS; CONTINUUM OBSERVATIONS; IRAS SOURCES; DARK CLOUDS; STARS; IMAGES; EVOLUTION AB We have mapped CO J=1-0 outflows from two low-mass protostar candidates in Taurus, IRAS 04365+2535 (TMC1-A) and IRAS 04368+2557 (L1527), using the Nobeyama Millimeter Array. The outflow structure is compared with deep near-infrared images obtained by IR array detectors. The molecular outflow from IRAS 043651+2535 (TMC1-A) shows a clear bipolar structure whose blueshifted lobe extends to the north-west and redshifted one to the south-east. The extension of the blueshifted lobe is consistent with that of the cometary infrared reflection nebula, suggesting the presence of a large (similar to 2500 AU) tilted dust disk or elongated envelope which obscures the other side of the nebula, i.e., the redshifted lobe. The outflow associated with IRAS 04368+2557 (L1527) appears to be almost perfectly in the plane of the sky with blueshifted and redshifted lobes significantly overlapped with each other, Both lobes show clear bow-tie shaped, shell-like structure whose geometrical center is coincident with a millimeter continuum point-like source. Deep near-infrared images have revealed that a faint bipolar infrared nebulosity is associated with the ''edge-on'' molecular outflow. The central source, totally invisible even at near-infrared wavelengths, might be heavily obscured by a disk or an elongated envelope whose size is comparable to the IR nebula (similar to 10 000 AU). These two IRAS sources show large difference in their near-infrared appearance even though they have similar physical properties including bolometric luminosity, association of CO outflows, and submillimeter/millimeter flux. This difference might be due to the inclination effect: the central part of IRAS 04368+2557 is more heavily obscured (A(upsilon)similar to 70 mag) along the line of sight than that of IRAS 04365+2535 by the envelope of a disk-like structure with almost edge-on geometry. The difference of the appearance of CO outflow between these two sources is consistent with this interpretation. Although IRAS 04368+2557 is regarded as a Class 0 source, our observations suggest that this source could be similar to IRAS 04365+2535, a Class 1 source, in nature, except for the geometry of the circumstellar envelope. (C) 1996 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. HITOTSUBASHI UNIV,KUNITACHI,TOKYO 186,JAPAN. JOINT ASTRON CTR,HILO,HI 96720. RP Tamura, M (reprint author), NATL ASTRON OBSERV,OSAWA 2-21-1,MITAKA,TOKYO 181,JAPAN. NR 37 TC 37 Z9 37 U1 0 U2 2 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 2076 EP & DI 10.1086/118164 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600026 ER PT J AU vanBelle, GT Dyck, HM Benson, JA Lacasse, MG AF vanBelle, GT Dyck, HM Benson, JA Lacasse, MG TI Angular size measurements of 18 Mira variable stars at 2.2 mu m SO ASTRONOMICAL JOURNAL LA English DT Article ID LONG-PERIOD VARIABLES; MASS-LOSS RATES; IOTA INTERFEROMETER; INFRARED PHOTOMETRY; TIME-SERIES; MODELS; TEMPERATURES; ATMOSPHERES; PARAMETERS; EVOLUTION AB We present angular size measurements of 18 oxygen-rich Mira variable stars. These data are part of a long term observational program using the Infrared Optical Telescope Array (IOTA) to characterize the observable behavior of these stars. Complementing the infrared angular size measurements, values for variable star phase, spectral type, bolometric flux, and distance were established for stars in the sample; flux and distance led to values for effective temperature (T-EFF), and linear radius, respectively. We are able to define an effective temperature versus spectral type scale for Mira variables that we compare to the temperature scales for K and M giants and supergiants. T-EFF's and linear radii for these stars are shown to lie between approximately 2100 and 3200 K, and 200 and 600 R(.), respectively. Relationships among the Mira variable parameters are explored for significant trends. Notably, the phase dependence of T-EFF is shown to follow simple expectations, and examination of the radius-T-EFF relationship yields a plausible description of the V and K band light curves of these stars. A simple examination of the oscillation mode of the stars in the sample does not strongly suggest either fundamental or first-overtone oscillation as the primary mode of oscillation. This conclusion differs from that recently presented by Haniff et al. (1995), who argue that Mira variables are all first-overtone pulsators. We discuss some possible reasons for the different conclusions between the two studies. (C) 1996 American Astronomical Society. C1 USNO,FLAGSTAFF STN,FLAGSTAFF,AZ 86002. FLWO,SMITHSONIAN INST,AMADO,AZ 85645. RP vanBelle, GT (reprint author), UNIV WYOMING,DEPT PHYS & ASTRON,LARAMIE,WY 82071, USA. NR 68 TC 96 Z9 96 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 2147 EP 2158 DI 10.1086/118170 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600032 ER PT J AU Greene, TP Lada, CJ AF Greene, TP Lada, CJ TI Near-infrared spectra and the evolutionary status of young stellar objects: Results of a 1.1-2.4 mu m survey SO ASTRONOMICAL JOURNAL LA English DT Article ID T-TAURI STARS; AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE STARS; LOW-MASS; CO; DISKS; SPECTROSCOPY; CLUSTER; MICRONS; MODELS AB We present the results of a moderate resolution (R similar to 500) 1.15-2.42 mu m near-IR spectroscopic survey of young stellar objects (YSOs), EU Ori type stars, and MK spectral standards. The survey sample includes approximately 100 mostly low-mass YSOs characterized by a wide range of spectral energy distributions (SEDs) and evolutionary states which are drawn from the Ophiuchus, Taurus, and other nearby star forming regions. As part of this study we also present the first systematic, flux-limited spectroscopic survey of an entire population of YSOs embedded within a single molecular cloud (Ophiuchus), In general we find the shapes of YSO spectra to be correlated with SED class such that the most embedded objects generally have the steepest IR spectra. Many YSOs also show absorption features similar to those of (mostly late-type) MK standard stars. For sources in the flux-limited sample, we find that the strengths of atomic and CO absorption features are closely related to SED class and evolutionary state. In particular, these line strengths generally decrease from the revealed Class III phase to the Class II phase to the self-embedded Class I phase where absorption features are typically absent at the resolution of our survey, confirming trends found in earlier studies. This correlation of absorption strength with SED class can be explained by a systematic increase in the veiling of an underlying stellar photosphere from Class III to Class I objects, The likely source of this veiling is continuum emission from increasing amounts of luminous circumstellar material surrounding these objects. Moreover, it appears that the absence of absorption features and the resulting large veilings of Class I sources are likely related to significantly increased levels of accretion/infall compared to Class II and III sources, Most YSOs in our study appear to have surface gravities which range between those of giant and dwarf stars. Flat-spectrum YSOs have the lowest surface gravities of all objects in our flux-limited Ophiuchus sample. FU Ori stars have even lower surface gravities, similar to those of giant or supergiant stars, suggestive of line formation in disks rather than stellar photospheres. The FU Ori type stars and a few other YSOs show deep and broad H2O absorptions, indicative of cool (T less than or equal to 3000 K) disks or stellar photospheres. Many Class I and Class II objects show relatively strong H I emission lines which probably originate in a partially ionized circumstellar region. However, mostly Class I objects show detectable H-2 emission lines. (C) 1996 American Astronomical Society. C1 SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. RP Greene, TP (reprint author), UNIV HAWAII, INST ASTRON, 1680 WOODLAWN DR, HONOLULU, HI 96822 USA. NR 36 TC 142 Z9 142 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 2184 EP 2221 DI 10.1086/118173 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600035 ER PT J AU Morse, JA Blair, WP Dopita, MA Hughes, JP Kirshner, RP Long, KS Raymond, JC Sutherland, RS Winkler, PF AF Morse, JA Blair, WP Dopita, MA Hughes, JP Kirshner, RP Long, KS Raymond, JC Sutherland, RS Winkler, PF TI Hubble Space Telescope observations of oxygen-rich supernova remnants in the magellanic clouds .1. Narrowband imaging of N132D in the lmc (vol 112, pg 509, 1996) SO ASTRONOMICAL JOURNAL LA English DT Correction, Addition C1 UNIV COLORADO,DEPT ASTROPHYS PLANETARY & ATMOSPHER SCI,CTR ASTROPHYS & SPACE ASTRON,BOULDER,CO 80309. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,CANBERRA,ACT 2611,AUSTRALIA. HARVARD UNIV,HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV COLORADO,JILA,BOULDER,CO 80309. NIST,BOULDER,CO 80309. MIDDLEBURY COLL,DEPT PHYS,MIDDLEBURY,VT 05753. RP Morse, JA (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. RI Dopita, Michael/P-5413-2014 OI Dopita, Michael/0000-0003-0922-4986 NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 1996 VL 112 IS 5 BP 2350 EP 2351 DI 10.1086/118189 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VQ496 UT WOS:A1996VQ49600051 ER PT J AU Oliver, RJ Masheder, MRW Thaddeus, P AF Oliver, RJ Masheder, MRW Thaddeus, P TI A new CO survey of the Monoceros OB1 region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM clouds; surveys, Galaxy, structure; radio lines, ISM; ISM, molecules; ISM, bubbles ID MOLECULAR CLOUDS; OUTER GALAXY; SOLAR CIRCLE; IRAS SOURCES; RADIAL-DISTRIBUTION; SUPERNOVA-REMNANTS; MILKY-WAY; CLUSTERS; MOTIONS; IMAGES AB A new, fully sampled, sensitive CO survey of 52.5 square degrees towards the Monoceros OB 1 (Mon OB 1) region has been completed using the CfA 1.2 m millimeter-wave radio telescope. This survey extends from b = -1.5 degrees to b = +3.5 degrees and from l = 196.0 degrees to l = 206.5 degrees on a uniformly spaced grid of 3.75' in l and b, and has substantially better sensitivity than previous surveys of the region. CO is detected in 80% of the area, 60% of which is weak with integrated intensities less than 5 K km s(-1). The large-scale kinematics are dominated by the Perseus and Local spiral arms. Within the Local arm the molecular gas appears to have been strongly influenced by supernova remnants and expanding H II regions with the strongest emission at velocities ranging from -17 to +10 km s(-1), and a total mass of 1.3 x 10(5) M.. Weak CO emission from Perseus arm clouds shows that they have a mean kinematic distance of 3.5 kpc and are comparable in size and mass to local molecular clouds. The coincident positions of colour selected IRAS point sources indicates that these distant clouds are undergoing massive star formation. C1 UNIV BRISTOL, HH WILLS PHYS LAB, ASTROPHYS GRP, BRISTOL BS8 1TL, AVON, ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NR 67 TC 35 Z9 35 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 3 BP 578 EP 590 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VW764 UT WOS:A1996VW76400034 ER PT J AU Barlow, MJ NguyenQRieu TruongBach Cernicharo, J GonzalezAlfonso, E Liu, XW Cox, P Sylvester, RJ Clegg, PE Griffin, MJ Swinyard, BM Unger, SJ Baluteau, JP Caux, E Cohen, M Cohen, RJ Emery, RJ Fischer, J Furniss, I Glencross, WM Greenhouse, MA Gry, C Joubert, M Lim, T Lorenzetti, D Nisini, B Omont, A Orfei, R Pequignot, D Saraceno, P Serra, G Skinner, CJ Smith, HA Walker, HJ Armand, C Burgdorf, M Ewart, D DiGiorgio, A Molinari, S Price, M Sidher, S Texier, D Trams, N AF Barlow, MJ NguyenQRieu TruongBach Cernicharo, J GonzalezAlfonso, E Liu, XW Cox, P Sylvester, RJ Clegg, PE Griffin, MJ Swinyard, BM Unger, SJ Baluteau, JP Caux, E Cohen, M Cohen, RJ Emery, RJ Fischer, J Furniss, I Glencross, WM Greenhouse, MA Gry, C Joubert, M Lim, T Lorenzetti, D Nisini, B Omont, A Orfei, R Pequignot, D Saraceno, P Serra, G Skinner, CJ Smith, HA Walker, HJ Armand, C Burgdorf, M Ewart, D DiGiorgio, A Molinari, S Price, M Sidher, S Texier, D Trams, N TI The rich far-infrared water vapour spectrum of W Hya SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars, general; stars, individual, W Hya; stars, mass loss; stars, AGE and post-AGE ID OH-IR STARS; EVOLVED STARS; CIRCUMSTELLAR ENVELOPES; EMISSION; MASERS; SIO AB We present an ISO Long Wavelength Spectrometer (LWS) grating spectrum of the oxygen-rich AGE star W Hya from 43-197 mu m. The spectrum is dominated by a forest of water vapour emission lines, confirming that H2O molecules are the dominant coolants of the winds of these stars. We have constructed an outflow model for the H2O spectrum of W Hya, which successfully matches the fluxes of most of the observed H2O lines, using an adopted wind temperature profile. These fits are sensitive to the mass loss rate, to the H2O abundance and to the inner radius of the H2O emitting region. The best fit parameters correspond to a mass loss rate of 6 x 10(-7) M. yr(-1) inner and outer radii for the emitting region of 1.5 x 10(14) and 1 x 10(16) cm, and a H2O/H-2 abundance of 8 x 10(-4) for r less than or equal to 4.5 x 10(14) cm and 3 x 10(-4) at large radii. A decrease of the H2O/H-2 abundance in the outer envelope is consistent with the predictions of photochemical models. The availability for the first time of observations of the line fluxes from the dominant coolant species should enable improved models of the wind temperature distribution to be produced. C1 OBSERV PARIS, F-75014 PARIS, FRANCE. CSIC, IEM, DEPT FIS MOL, E-28006 MADRID, SPAIN. OAN, E-28800 ALCALA DE HENARES, SPAIN. UNIV ALCALA DE HENARES, DEPT FIS, E-28871 ALCALA DE HENARES, MADRID, SPAIN. UNIV PARIS 11, INST ASTROPHYS SPATIALE, F-91405 ORSAY, FRANCE. UNIV LONDON QUEEN MARY & WESTFIELD COLL, DEPT PHYS, LONDON E1 4NS, ENGLAND. RUTHERFORD APPLETON LAB, DEPT SPACE SCI, CHILTON OX11 0QX, OXON, ENGLAND. CNRS, ASTRON SPATIALE LAB, F-13376 MARSEILLE 12, FRANCE. UPS, CNRS, CTR ETUD SPATIALE RAYONNEMENTS, F-31029 TOULOUSE, FRANCE. UNIV CALIF BERKELEY, RADIO ASTRON LAB, BERKELEY, CA 94720 USA. UNIV MANCHESTER, NUFFIELD RADIO ASTRON LABS, MACCLESFIELD SK11 9DL, CHESHIRE, ENGLAND. USN, RES LAB, REMOTE SENSING DIV, WASHINGTON, DC 20375 USA. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, WASHINGTON, DC 20560 USA. OSSERV ASTRON ROMA, I-00040 MONTE PORZIO CATO, ITALY. CNES, F-75001 PARIS, FRANCE. CNR, IST FIS SPAZIO INTERPLANETARIO, I-00044 FRASCATI, ITALY. INST ASTROPHYS, F-75014 PARIS, FRANCE. OBSERV PARIS, F-92190 MEUDON, FRANCE. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. ISO, SCI OPERAT CTR, LWS INSTRUMENT DEDICATED TEAM, E-28080 MADRID, SPAIN. RP Barlow, MJ (reprint author), UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, GOWER ST, LONDON WC1E 6BT, ENGLAND. RI Barlow, Michael/A-5638-2009 OI Barlow, Michael/0000-0002-3875-1171 NR 13 TC 61 Z9 61 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L241 EP L244 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600052 ER PT J AU Cernicharo, J Barlow, MJ GonzalezAlfonso, E Cox, P Clegg, PE NguyenQRieu Omont, A Guelin, M Liu, XW Sylvester, RJ Lim, T Griffin, MJ Swinyard, BM Unger, SJ Ade, PAR Baluteau, JP Caux, E Cohen, M Emery, RJ Fischer, J Furniss, I Glencross, WM Greenhouse, MA Gry, C Joubert, M Lorenzetti, D Nisini, B Orfei, R Pequignot, D Saraceno, P Serra, G Skinner, CJ Smith, HA Towlson, WA Walker, HJ Armand, C Burgdorf, M Ewart, D DiGiorgio, A Molinari, S Price, M Sidher, S Texier, D Trams, N AF Cernicharo, J Barlow, MJ GonzalezAlfonso, E Cox, P Clegg, PE NguyenQRieu Omont, A Guelin, M Liu, XW Sylvester, RJ Lim, T Griffin, MJ Swinyard, BM Unger, SJ Ade, PAR Baluteau, JP Caux, E Cohen, M Emery, RJ Fischer, J Furniss, I Glencross, WM Greenhouse, MA Gry, C Joubert, M Lorenzetti, D Nisini, B Orfei, R Pequignot, D Saraceno, P Serra, G Skinner, CJ Smith, HA Towlson, WA Walker, HJ Armand, C Burgdorf, M Ewart, D DiGiorgio, A Molinari, S Price, M Sidher, S Texier, D Trams, N TI The ISO/LWS far infrared spectrum of IRC+10216 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars, AGE and post AGE; stars, individual, IRC+10216; stars, circumstellar matter; infrared, stars ID HCN AB We present an ISO Long Wavelength Spectrometer (LWS) grating spectrum of the carbon-rich circumstellar envelope -CSE- of IRC+10216 between 43 and 197 mu m. The spectrum consists of strong dust emission plus a forest of emission lines from CO, HCN, (HCN)-C-13 and vibrationally excited HCN (nu(2)=1(1),2(0,2) and nu(1,3)=1) All the CO lines between J=14-13 and J=39-38 have been detected while lines of HCN with J(u) as high as 48 have also been observed. The molecular emission arises from the warm and dense gas located in the innermost zone of the CSE. The CO and HCN emission can be easily explained if the vibrational and rotational temperatures are around 700-1500 K. We also report the tentative detection of the bending mode of the C-3 molecule around 62 cm(-1) (157.2 mu m). C1 OAN, E-28800 A DE HENARES, SPAIN. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. UNIV ALCALA DE HENARES, DEPT FIS, E-28871 ALCALA DE HENARES, SPAIN. UNIV PARIS 11, INST ASTROPHYS SPATIALE, F-91405 ORSAY, FRANCE. UNIV LONDON QUEEN MARY & WESTFIELD COLL, LONDON E1 4NS, ENGLAND. OBSERV PARIS, F-75014 PARIS, FRANCE. INST ASTROPHYS, F-75014 PARIS, FRANCE. INST RADIO ASTRON MILLIMETR, F-38406 ST MARTIN DHERES, FRANCE. ISO, SCI OPERAT CTR, LWS INSTRUMENT DEDICATED TEAM, E-28080 MADRID, SPAIN. RUTHERFORD APPLETON LAB, DIDCOT OX11 0QX, OXON, ENGLAND. ASTRON SPATIALE LAB, F-13376 MARSEILLE, FRANCE. UPS, CNRS, CTR ETUD SPATIALE RAYONNEMENTS, F-31029 TOULOUSE, FRANCE. UNIV CALIF BERKELEY, RADIO ASTRON LAB, BERKELEY, CA 94720 USA. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, WASHINGTON, DC 20560 USA. USN, RES LAB, REMOTE SENSING DIV, WASHINGTON, DC 20375 USA. OBSERV ASTRON ROMA, I-00040 MONTE PORZIO CATO, ITALY. CNES, F-75001 PARIS, FRANCE. CNR, IST FIS SPAZIO INTERPLANETARIO, I-00044 FRASCATI, ITALY. OBSERV PARIS, SECT ASTROPHYS, F-92190 PARIS, FRANCE. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. RP Cernicharo, J (reprint author), CSIC, IEM, DEPT FIS MOL, SERRANO 123, E-28006 MADRID, SPAIN. RI Barlow, Michael/A-5638-2009; Molinari, Sergio/O-4095-2016 OI Barlow, Michael/0000-0002-3875-1171; Molinari, Sergio/0000-0002-9826-7525 NR 11 TC 71 Z9 71 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L201 EP L204 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600042 ER PT J AU Clegg, PE Ade, PAR Armand, C Baluteau, JP Barlow, MJ Buckley, MA Berges, JC Burgdorf, M Caux, E Ceccarelli, C Cerulli, R Church, SE Cotin, F Cox, P Cruvellier, P Culhane, JL Davis, GR DiGiorgio, A Diplock, BR Drummond, DL Emery, RJ Ewart, JD Fischer, J Furniss, I Glencross, WM Greenhouse, MA Griffin, MJ Gry, C Harwood, AS Hazell, AS Joubert, M King, KJ Lim, T Liseau, R Long, JA Lorenzetti, D Molinari, S Murray, AG Naylor, DA Nisini, B Norman, K Omont, A Orfei, R Patrick, TJ Pequignot, D Pouliquen, D Price, MC NguyenQRieu Rogers, AJ Robinson, FD Saisse, M Saraceno, P Serra, G Sidher, SD Smith, AF Smith, HA Spinoglio, L Swinyard, BM Texier, D Towlson, WA Trams, NR Unger, SJ White, GJ AF Clegg, PE Ade, PAR Armand, C Baluteau, JP Barlow, MJ Buckley, MA Berges, JC Burgdorf, M Caux, E Ceccarelli, C Cerulli, R Church, SE Cotin, F Cox, P Cruvellier, P Culhane, JL Davis, GR DiGiorgio, A Diplock, BR Drummond, DL Emery, RJ Ewart, JD Fischer, J Furniss, I Glencross, WM Greenhouse, MA Griffin, MJ Gry, C Harwood, AS Hazell, AS Joubert, M King, KJ Lim, T Liseau, R Long, JA Lorenzetti, D Molinari, S Murray, AG Naylor, DA Nisini, B Norman, K Omont, A Orfei, R Patrick, TJ Pequignot, D Pouliquen, D Price, MC NguyenQRieu Rogers, AJ Robinson, FD Saisse, M Saraceno, P Serra, G Sidher, SD Smith, AF Smith, HA Spinoglio, L Swinyard, BM Texier, D Towlson, WA Trams, NR Unger, SJ White, GJ TI The ISO long-wavelength spectrometer SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE artificial satellites, space probes; instrumentation, spectrographs; infrared, general AB The Long-Wavelength Spectrometer (LWS) is one of two complementary spectrometers aboard the European Space Agency's Infrared Space Observatory(1) (ISO) (Kessler et al., 1996). It operates over the wavelength range 43 - 196.9 mu m at either medium (about 150 to 200) or high (6800 to 9700) spectral resolving power. This Letter describes the instrument and its modes of operation. a companion paper (Swinyard et al, 1996) describes its performance and calibration. C1 ISO SCI OPERAT CTR, LWS INSTRUMENT DEDICATED TEAM, E-28080 MADRID, SPAIN. ASTRON SPATIALE LAB, CNRS, F-13376 MARSEILLE 12, FRANCE. OBSERV MARSEILLE, F-13248 MARSEILLE, FRANCE. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. RUTHERFORD APPLETON LAB, DIDCOT OX11 0QX, OXON, ENGLAND. CTR ETUD SPATIALE RAYONNEMENTS, CNRS, F-31029 TOULOUSE, FRANCE. CNR, IST FIS SPAZIO INTERPLANETARIO, I-00044 FRASCATI, ITALY. CALTECH, PASADENA, CA 91125 USA. UNIV PARIS 11, INST ASTROPHYS SPATIALE, F-91405 ORSAY, FRANCE. UCL, MULLARD SPACE SCI LAB, DORKING RH5 6NT, SURREY, ENGLAND. UNIV SASKATCHEWAN, INST SPACE & ATMOSPHER STUDIES, SASKATOON, SK S7N 5E2, CANADA. SMITHSONIAN INST, ASTROPHYS LAB, NATL AIR & SPACE MUSEUM, WASHINGTON, DC 20560 USA. CNES, F-75001 PARIS, FRANCE. NAVAL RES LAB, REMOTE SENSING DIV, WASHINGTON, DC 20375 USA. STOCKHOLM OBSERV, S-13336 SALTSJOBADEN, SWEDEN. OSSERV ASTRON ROMA, I-00040 MONTE PORZIO CATO, ITALY. UNIV LETHBRIDGE, DEPT PHYS, LETHBRIDGE, AB T1K 3M4, CANADA. INST ASTROPHYS, CNRS, F-75014 PARIS, FRANCE. OBSERV PARIS, F-92190 MEUDON, FRANCE. OBSERV PARIS, F-75014 PARIS, FRANCE. NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD 20771 USA. RP UNIV LONDON QUEEN MARY & WESTFIELD COLL, MILE END RD, LONDON E1 4NS, ENGLAND. RI Barlow, Michael/A-5638-2009; Molinari, Sergio/O-4095-2016 OI Barlow, Michael/0000-0002-3875-1171; Molinari, Sergio/0000-0002-9826-7525 NR 5 TC 286 Z9 287 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L38 EP L42 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600003 ER PT J AU Emery, R Aannestad, P Minchin, N Unger, SJ Baluteau, JP Barlow, MJ Caux, E Serra, G Joubert, M Lorenzetti, D Pequignot, D Armand, C Burgdorf, M diGiorgio, A Gry, C Molinari, S Texier, D Sidher, SD Trams, N Swinyard, B King, K Smith, H Furniss, I Ewart, D Price, M Smith, A AF Emery, R Aannestad, P Minchin, N Unger, SJ Baluteau, JP Barlow, MJ Caux, E Serra, G Joubert, M Lorenzetti, D Pequignot, D Armand, C Burgdorf, M diGiorgio, A Gry, C Molinari, S Texier, D Sidher, SD Trams, N Swinyard, B King, K Smith, H Furniss, I Ewart, D Price, M Smith, A TI Extended fine structure and continuum emission from S140/L1204 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM, S140; I-III regions; ISM, clouds; infrared, interstellar, lines; infrared, interstellar, continuum ID MOLECULAR CLOUDS; PHOTODISSOCIATION REGIONS; S140; S-140/L-1204; OUTFLOW; CARBON; LINE AB Grating spectra, covering the wavelength range 45 to 187 mu m have been taken with the ISO Long Wavelength Spectrometer (LWS) at a series of pointing positions over the S140 region, centred on the cluster of embedded young stellar objects at the south-west corner of the L1204 molecular cloud. Extended emission from [CII] 158 mu m and [Or]63 mu m is seen, peaking near the position of the embedded stars. The measurements of the fine structure lines are interpreted in terms of PDR models for the emission, as well as the underlying thermal continuum for the heated gas and dust. C1 ARIZONA STATE UNIV, DEPT PHYS & ASTRON, TEMPE, AZ 85287 USA. UNIV LONDON QUEEN MARY & WESTFIELD COLL, DEPT PHYS, LONDON E1 4NS, ENGLAND. CNRS, ASTRON SPATIALE LAB, F-13012 MARSEILLE, FRANCE. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. CTR ETUD SPATIALE RAYONNEMENTS, F-31029 TOULOUSE, FRANCE. CNES, F-75001 PARIS, FRANCE. ASTRON OBSERV, MONTE PORZIO CATO, ITALY. OBSERV PARIS, SECT ASTROPHYS, F-75014 PARIS, FRANCE. VILSPA, LWS INSTRUMENT DEDICATED TEAM, E-28080 MADRID, SPAIN. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. RP RUTHERFORD APPLETON LAB, DEPT SPACE SCI, CHILTON OX11 0QX, OXON, ENGLAND. RI Barlow, Michael/A-5638-2009; Molinari, Sergio/O-4095-2016 OI Barlow, Michael/0000-0002-3875-1171; Molinari, Sergio/0000-0002-9826-7525 NR 18 TC 7 Z9 7 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L285 EP L288 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600063 ER PT J AU Fischer, J Shier, LM Luhman, ML Satyapal, S Smith, HA Stacey, GJ Unger, SJ Greenhouse, MA Spinoglio, L Malkan, MA Lord, SD Miles, JW Shure, MA Clegg, PE Ade, PAR Armand, C Burgdorf, M Church, SE Davis, GR DiGiorgio, A Ewart, D Furniss, I Glencross, WM Gry, C Lim, T Molinari, S NguyenRieu, Q Price, MC Sidher, SD Smith, A Swinyard, BM Texier, D Trams, NR Wolfire, MG AF Fischer, J Shier, LM Luhman, ML Satyapal, S Smith, HA Stacey, GJ Unger, SJ Greenhouse, MA Spinoglio, L Malkan, MA Lord, SD Miles, JW Shure, MA Clegg, PE Ade, PAR Armand, C Burgdorf, M Church, SE Davis, GR DiGiorgio, A Ewart, D Furniss, I Glencross, WM Gry, C Lim, T Molinari, S NguyenRieu, Q Price, MC Sidher, SD Smith, A Swinyard, BM Texier, D Trams, NR Wolfire, MG TI LWS observations of the colliding galaxies NGC 4038/39 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared, galaxies; galaxies, interactions; galaxies, starburst; galaxies, evolution; galaxies, nuclei; galaxies, individual NGC 4038/39 ID MOLECULAR CLOUDS; ANTENNAE; EMISSION AB Infrared Space Observatory (ISO) Long Wavelength Spectrometer (LWS) and ground-based Fabry-Perot imaging spectroscopic observations are used to penetrate the extinction to the powerful burst of star formation that has occurred in the extranuclear molecular cloud complex in the galaxy overlap region of the galaxies NGC 4038/39 (''The Antennae''). Parameters of the starburst and typical molecular cloud core characteristics are derived. It is found that the starburst can power the infrared luminosity of this galaxy system. C1 SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. CORNELL UNIV, DEPT ASTRON, ITHACA, NY 14853 USA. RUTHERFORD APPLETON LAB, DIV S&A, DIDCOT OX11 0QX, OXON, ENGLAND. CNR, IST FIS SPAZIO INTERPLANETARIO, I-00044 FRASCATI, ITALY. UNIV CALIF LOS ANGELES, DEPT ASTRON, LOS ANGELES, CA 90024 USA. CALTECH, IPAC, PASADENA, CA 91125 USA. GEORGIA STATE UNIV, CTR HIGH ANGULAR RES ASTRO, ATLANTA, GA 30303 USA. UNIV LONDON QUEEN MARY & WESTFIELD COLL, DEPT PHYS, LONDON E1 4NS, ENGLAND. ISO, SCI OPERAT CTR, LWS INSTRUMENT DEDICATED TEAM, MADRID 50727, SPAIN. CALTECH, DIV PHYS MATH & ASTRON, PASADENA, CA 91125 USA. UNIV SASKATCHEWAN, INST SPACE & ATMOSPHER STUDIES, SASKATOON, SK S7N 5E2, CANADA. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. ASTRON SPATIALE LAB, CNRS, F-13248 MARSEILLE 12, FRANCE. OBSERV PARIS, F-75014 PARIS, FRANCE. RP Fischer, J (reprint author), USN, RES LAB, REMOTE SENSING DIV, 4555 OVERLOOOK AVE SW, WASHINGTON, DC 20375 USA. RI Molinari, Sergio/O-4095-2016 OI Molinari, Sergio/0000-0002-9826-7525 NR 15 TC 37 Z9 37 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L97 EP L100 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600016 ER PT J AU Griffin, MJ Naylor, DA Davis, GR Ade, PAR Oldham, PG Swinyard, BM Gautier, D Lellouch, E Orton, GS Encrenaz, T deGraauw, T Furniss, I Smith, H Armand, C Burgdorf, M DiGiorgio, A Eward, D Gry, C King, KJ Lim, T Molinari, S Price, M Sidher, S Smith, A Texier, D Trams, N Unger, SJ Salama, A AF Griffin, MJ Naylor, DA Davis, GR Ade, PAR Oldham, PG Swinyard, BM Gautier, D Lellouch, E Orton, GS Encrenaz, T deGraauw, T Furniss, I Smith, H Armand, C Burgdorf, M DiGiorgio, A Eward, D Gry, C King, KJ Lim, T Molinari, S Price, M Sidher, S Smith, A Texier, D Trams, N Unger, SJ Salama, A TI First detection of the 56-mu m rotational line of HD in Saturn's atmosphere SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites, individual, Saturn; infrared, solar system ID COLLISIONAL INTERFERENCE; SPECTRUM; PLANETS; RATIO AB The R(1) rotational line of HD at 56.23 mu m has been detected for the first time on Saturn using the Long Wavelength Spectrometer (LWS) on board the Infrared Space Observatory (ISO). The measurements were made using the LWS in Fabry-Perot mode in January 1996 during the ISO performance verification phase. The measured spectrum has been compared with atmospheric models to determine the HD/H-2 abundance ratio. The best model fit to the measured spectrum was obtained with a D/H ratio in hydrogen of 2.3x10(-5); D/H values between 1.5x10(-5) and 3.5x10(-5) are however also compatible with the data. This result is intermediate between the saturnian value derived from ground-based observations of methane and its deuterated isotope, and the preliminary determination of the jovian D/H ratio measured by the mass spectrometer in the Galileo probe. The initial Saturn measurements reported here will be repeated to improve the signal-to-noise ratio, and LWS observations of HD on Jupiter, Uranus and Neptune will also be made. C1 UNIV LETHBRIDGE, DEPT PHYS, LETHBRIDGE, AB T1K 3M4, CANADA. UNIV SASKATCHEWAN, INST SPACE & ATMOSPHER STUDIES, SASKATOON, SK S7N 5E2, CANADA. RUTHERFORD APPLETON LAB, DIDCOT OX11 0QX, OXON, ENGLAND. OBSERV PARIS, F-92195 MEUDON, FRANCE. CALTECH, JET PROP LAB, PASADENA, CA 91109 USA. SRON, GRONINGEN, NETHERLANDS. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. LWS, INSTRUMENT DEDICATED TEAM, E-28080 MADRID, SPAIN. ISO, SCI OPERAT CTR, E-28080 MADRID, SPAIN. RP Griffin, MJ (reprint author), UNIV LONDON QUEEN MARY & WESTFIELD COLL, DEPT PHYS, MILE END RD, LONDON E1 4NS, ENGLAND. RI Molinari, Sergio/O-4095-2016 OI Molinari, Sergio/0000-0002-9826-7525 NR 17 TC 34 Z9 34 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L389 EP L392 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600089 ER PT J AU Liu, XW Barlow, MJ NguyenQRieu TruongBach Cox, P Pequignot, D Clegg, PE Swinyard, BM Griffin, MJ Baluteau, JP Lim, T Skinner, CJ Smith, HA Ade, PAR Furniss, I Towlson, WA Unger, SJ King, KJ Davis, GR Cohen, M Emery, RJ Fischer, J Glencross, WM Caux, E Greenhouse, MA Gry, C Joubert, M Lorenzetti, D Nisini, B Omont, A Orfei, R Saraceno, P Serra, G Walker, HJ Armand, C Burgdorf, M DiGiorgio, A Molinari, S Price, M Texier, D Sidher, S Trams, N AF Liu, XW Barlow, MJ NguyenQRieu TruongBach Cox, P Pequignot, D Clegg, PE Swinyard, BM Griffin, MJ Baluteau, JP Lim, T Skinner, CJ Smith, HA Ade, PAR Furniss, I Towlson, WA Unger, SJ King, KJ Davis, GR Cohen, M Emery, RJ Fischer, J Glencross, WM Caux, E Greenhouse, MA Gry, C Joubert, M Lorenzetti, D Nisini, B Omont, A Orfei, R Saraceno, P Serra, G Walker, HJ Armand, C Burgdorf, M DiGiorgio, A Molinari, S Price, M Texier, D Sidher, S Trams, N TI The ISO LWS grating spectrum of NGC 7027 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary nebulae, general; planetary nebulae, individual, NGC 7027; ISM, atoms; ISM, molecules ID PLANETARY-NEBULAE; NGC-7027; EMISSION AB We present a high signal-to-noise ISO Long Wavelength Spectrometer (LWS) grating spectrum of the planetary nebula NGC7027 from 43-194 mu m. In total 40 emission lines have been detected, with 30 identified. From the ionized region, we observe fine-structure lines from [N Il], [N III] and [O III]. The [O I] and [C II] fine-structure lines from the photodissociation region are the strongest features observed in this spectral region. Amongst the molecular lines, 11 pure rotation CO lines from J=14-13 up to J=24-23 have been detected. The most striking result, however, is the detection in this carbon-rich nebula of the o-H2O 179.53 mu m and the OH 119.3 mu m fundamental lines. Astrophysical implications are briefly discussed. C1 OBSERV PARIS, F-75014 PARIS, FRANCE. UNIV PARIS 11, INST ASTROPHYS SPATIALE, F-91405 ORSAY, FRANCE. OBSERV PARIS, F-92190 MEUDON, FRANCE. UNIV LONDON QUEEN MARY & WESTFIELD COLL, DEPT PHYS, LONDON E1 4NS, ENGLAND. RUTHERFORD APPLETON LAB, DEPT SPACE SCI, CHILTON OX11 0QX, OXON, ENGLAND. ASTRON SPATIALE LAB, CNRS, F-13376 MARSEILLE 12, FRANCE. ISO, SCI OPERAT CTR, LWS INSTRUMENT DEDICATED TEAM, E-28080 MADRID, SPAIN. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. UNIV SASKATCHEWAN, INST SPACE & ATMOSPHERE STUDIES, SASKATOON, SK S7N 5E2, CANADA. UNIV CALIF BERKELEY, RADIO ASTRON LAB, BERKELEY, CA 94720 USA. USN, RES LAB, REMOTE SENSING DIV, WASHINGTON, DC 20375 USA. UNIV TOULOUSE 3, CTR ETUD SPATIALE RAYONNEMENTS, CNRS, F-31029 TOULOUSE, FRANCE. CNES, F-75001 PARIS, FRANCE. OSSERV ASTRON ROMA, I-00040 MONTE PORZIO CATO, ITALY. CNR, IST FIS SPAZIO INTERPLANETARIO, I-00044 FRASCATI, ITALY. INST ASTROPHYS, F-75014 PARIS, FRANCE. RP UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, GOWER ST, LONDON WC1E 6BT, ENGLAND. RI Barlow, Michael/A-5638-2009 OI Barlow, Michael/0000-0002-3875-1171 NR 14 TC 55 Z9 57 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L257 EP L260 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600056 ER PT J AU Neufeld, DA Chen, W Melnick, GJ deGraauw, T Feuchtgruber, H Haser, L Lutz, D Harwit, M AF Neufeld, DA Chen, W Melnick, GJ deGraauw, T Feuchtgruber, H Haser, L Lutz, D Harwit, M TI Detection of far-infrared rotational lines of water vapour toward W Hydrae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars, circumstellar matter; stars, late-type; infrared, stars; molecular processes ID MASS-LOSS RATES; CIRCUMSTELLAR ENVELOPES; EVOLVED STARS; DUST; GRAINS; GIANT; CO AB We report the first detection of thermal water vapour emission from a circumstellar outflow. We have observed four far-infrared rotational emission lines of water vapour and one water absorption feature toward the evolved star W Hydrae, using the Short Wavelength Spectrometer (SWS) of the Infrared Space Observatory (ISO). Three of the emission lines were observed in the instrument's Fabry-Perot mode at a resolving power lambda/Delta lambda of approximately 30 000: the 7(25) - 6(16) line at 29.84 mu m, the 4(41) - 3(12) line at 31.77 mu m, and the 4(32) - 3(03) line at 40.69 mu m One additional emission line, the 4(41) - 4(14) line at 37.98 mu m, and one absorption feature at 38.08 mu m that we attribute to a blend of the 13(13,0) - 13(12,1) and the 13(13,1) - 13(12,2) water lines were observed in grating mode at a resolving power of about 2 000. The observed emission line fluxes were 3.2 x 10(-19) 6.3 x 10(-19), 2.3 x 10(-19) and 2.8 x 10(-19) W cm(-2) respectively, and the equivalent width of the absorption feature was similar to 10 km s(-1). To within the possible errors in the flux calibration, the observed emission line fluxes can be accounted for simultaneously by a model similar to that of Chen & Neufeld (1995), given a mass-loss rate in the range (0.5 - 3) x 10(-5) M. yr(-1) This range lies at least a factor similar to 2 above an independent estimate of the mass-loss rate that may be derived from dynamical considerations, and at least a factor similar to 30 above previous estimates based upon the interpretation of CO observations. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV GRONINGEN, SRON, SPACE RES LAB, GRONINGEN, NETHERLANDS. ESA, ISO, SCI OPERAT CTR, VILLAFRANCA, SPAIN. MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. RP Neufeld, DA (reprint author), JOHNS HOPKINS UNIV, DEPT PHYS & ASTRON, 3400 N CHARLES ST, BALTIMORE, MD 21218 USA. NR 19 TC 36 Z9 36 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L237 EP L240 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600051 ER PT J AU Nisini, B Lorenzetti, D Cohen, M Ceccarelli, C Giannini, T Liseau, R Molinari, S Radicchi, A Saraceno, P Spinoglio, L Tommasi, E Clegg, PE Ade, PAR Armand, C Barlow, MJ Burgdorf, M Caux, E Cerulli, P Church, SE DiGiorgio, A Fischer, J Furniss, I Glencross, WM Griffin, MJ Gry, C King, KJ Lim, T Naylor, DA Texier, D Orfei, R NguyenQRieu Sidher, S Smith, BM Swinyard, BM Trams, N Unger, SJ White, GJ AF Nisini, B Lorenzetti, D Cohen, M Ceccarelli, C Giannini, T Liseau, R Molinari, S Radicchi, A Saraceno, P Spinoglio, L Tommasi, E Clegg, PE Ade, PAR Armand, C Barlow, MJ Burgdorf, M Caux, E Cerulli, P Church, SE DiGiorgio, A Fischer, J Furniss, I Glencross, WM Griffin, MJ Gry, C King, KJ Lim, T Naylor, DA Texier, D Orfei, R NguyenQRieu Sidher, S Smith, BM Swinyard, BM Trams, N Unger, SJ White, GJ TI LWS-spectroscopy of Herbig Haro objects and molecular outflows in the Cha II dark cloud SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars, formation; stars, individual, IRAS 12496-7650; ISM, jets and outflows; ISRI, individual objects, HH52,53,54; infrared, ISM, lines ID PHOTODISSOCIATION REGIONS; EXCITING STARS; AE STAR; EMISSION AB We present the first far infrared spectra of the Herbig Hare objects HH 52-53-54 and of IRAS 12496-7650, all located in the nearby star forming region known as Chamaleon II dark cloud, obtained with the Long Wavelength Spectrometer (LWS) onboard the Infrared Space Observatory (ISO). The richest spectrum is found in HH54, showing molecular transitions (CO with J(u) from 19 to 14, water vapour mainly in its ortho form and OH) and low excitation fine structure lines ([OI]63, 145 mu m, [CII]158 mu m). In HH52 and HH53, only the [OI] and [CII] lines are detected. The LWS spectrum of IRAS 12496-7650 shows both fine structure and CO lines. The [CII]158 mu m line is ubiquitous in the region, as proved by its presence in all ISO pointings, including the raster scan maps. The fine structure lines are used to evaluate the physical parameters of the emitting regions. In particular, the mass loss rates of each outflow present in the region, are derived from the [OI]63 mu m line luminosity. C1 OSSERV ASTRON ROMA, I-00040 MONTE PORZIO CATO, ITALY. UNIV CALIF BERKELEY, RADIO ASTRON LAB, BERKELEY, CA 94720 USA. OBSERV GRENOBLE, ASTROPHYS LAB, F-38041 GRENOBLE, FRANCE. STOCKHOLM OBSERV, S-13336 SALTSJOBADEN, SWEDEN. ISO, SCI OPERAT CTR, LWS INSTRUMENT DEDICATED TEAM, VILLAFRANCA, SPAIN. UNIV LONDON QUEEN MARY & WESTFIELD COLL, DEPT PHYS, LONDON E1 4NS, ENGLAND. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. UNIV TOULOUSE 3, CESR, CNRS, F-31029 TOULOUSE, FRANCE. CALTECH, PASADENA, CA 91125 USA. USN, RES LAB, REMOTE SENSING DIV, WASHINGTON, DC 20375 USA. RUTHERFORD APPLETON LAB, DEPT SPACE SCI, CHILTON OX11 0QX, OXON, ENGLAND. UNIV LETHBRIDGE, DEPT PHYS, LETHBRIDGE, AB T1K 3M4, CANADA. OBSERV PARIS, F-75014 PARIS, FRANCE. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. RP Nisini, B (reprint author), CNR, IST FIS SPAZIO INTERPLANETARIO, CASELLA POSTALE 27, I-00044 FRASCATI, ITALY. RI Barlow, Michael/A-5638-2009; Molinari, Sergio/O-4095-2016 OI Barlow, Michael/0000-0002-3875-1171; Molinari, Sergio/0000-0002-9826-7525 NR 17 TC 24 Z9 24 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L321 EP L324 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600072 ER PT J AU Saraceno, P Ceccarelli, C Clegg, P Correia, C DiGiorgio, A Giannini, T Griffin, M Lorenzetti, D Molinari, S NguyenQRieu Nisini, B Radicchi, A Spinoglio, L Tommasi, E White, GJ Ade, PAR Andre, P Armand, C Barlow, MJ Burgdorf, M Caux, E Cerulli, P Fischer, J Furniss, I Glencross, B Gry, C King, KJ Lim, T Liseau, R Minchin, N Naylor, D Texier, D Orfei, R Palla, F Sidher, S Smith, HA Swinyard, B Trams, N Unger, S AF Saraceno, P Ceccarelli, C Clegg, P Correia, C DiGiorgio, A Giannini, T Griffin, M Lorenzetti, D Molinari, S NguyenQRieu Nisini, B Radicchi, A Spinoglio, L Tommasi, E White, GJ Ade, PAR Andre, P Armand, C Barlow, MJ Burgdorf, M Caux, E Cerulli, P Fischer, J Furniss, I Glencross, B Gry, C King, KJ Lim, T Liseau, R Minchin, N Naylor, D Texier, D Orfei, R Palla, F Sidher, S Smith, HA Swinyard, B Trams, N Unger, S TI LWS observations of the bright rimmed globule IC1396N SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars, formation; ISM, jets and outflows; ISM, individual objects, 1C1396N; infrared, ISM, lines ID EMISSION; DENSITY AB We present the first far-infrared spectrum of the IRAS source associated with IC1396N, located in the HII region IC1396 together with submillimeter and millimeter photometry. A rich spectrum of CO, OH, and H2O lines are detected in the ISO-LWS spectrum, indicative of a warm, dense region, probably shock excited, around the source. Among the fine structure lines, [OIII] and [NIII] are also detected and can be explained by the presence of the O6 star HD206267 approximately 16 pc away. The far infrared and submillimeter spectral energy distribution is fitted with a model assuming spherical grey-bodies with a radial power law of density and temperature. An accurate measure of the bolometric luminosity and an estimate of the total envelope mass are obtained. C1 OBSERV GRENOBLE, ASTROPHYS LAB, F-38041 GRENOBLE, FRANCE. UNIV LONDON QUEEN MARY & WESTFIELD COLL, DEPT PHYS, LONDON E1 4NS, ENGLAND. ISO, SCI OPERAT CTR, LWS INSTUMENT DEDICATED TEAM, VILLAFRANCA, SPAIN. OSSERV ASTRON ROMA, I-00040 MONTE PORZIO CATO, ITALY. OBSERV PARIS, F-75014 PARIS, FRANCE. CENS, CEA, SERV ASTROPHYS, F-91191 GIF SUR YVETTE, FRANCE. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. UNIV TOULOUSE 3, CESR, CNRS, F-31029 TOULOUSE, FRANCE. USN, RES LAB, REMOTE SENSING DIV, WASHINGTON, DC 20375 USA. STOCKHOLM OBSERV, S-13336 SALTSJOBADEN, SWEDEN. UNIV LETHBRIDGE, DEPT PHYS, LETHBRIDGE, AB T1K 3M4, CANADA. OSSERV ASTROFIS ARCETRI, I-50125 FLORENCE, ITALY. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. RUTHERFORD APPLETON LAB, DEPT SPACE SCI, CHILTON OX11 0QX, OXON, ENGLAND. RP Saraceno, P (reprint author), CNR, IST FIS SPAZIO INTERPLANETARIO, CP 27, I-00044 FRASCATI, ITALY. RI Barlow, Michael/A-5638-2009; Molinari, Sergio/O-4095-2016 OI Barlow, Michael/0000-0002-3875-1171; Molinari, Sergio/0000-0002-9826-7525 NR 15 TC 34 Z9 34 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L293 EP L296 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600065 ER PT J AU Swinyard, BM Clegg, PE Ade, PAR Armand, C Balteau, JP Barlow, MJ Berges, JC Burgdorf, M Caux, E Ceccarelli, C Cerulli, R Church, SE Colgan, S Cotin, F Cox, P Cruvellier, P Davis, GR DiGiorgio, A Emery, RJ Ewart, D Fischer, J Furniss, I Glencrossi, WM Greenhouse, M Griffin, MJ Gry, C Haas, MR Joubert, M King, KJ Lim, T Liseau, R Lord, S Lorenzetti, D Molinari, S Naylor, DA Nisini, B Omont, A Orfei, R Patrick, T Pequignot, D Pouliquen, D Price, MC NguyenQRieu Robinson, FD Saisse, M Saraceno, P Serra, G Sidher, SD Smith, HA Spinoglio, L Texier, D Towlson, WA Trams, N Unger, SJ White, GJ AF Swinyard, BM Clegg, PE Ade, PAR Armand, C Balteau, JP Barlow, MJ Berges, JC Burgdorf, M Caux, E Ceccarelli, C Cerulli, R Church, SE Colgan, S Cotin, F Cox, P Cruvellier, P Davis, GR DiGiorgio, A Emery, RJ Ewart, D Fischer, J Furniss, I Glencrossi, WM Greenhouse, M Griffin, MJ Gry, C Haas, MR Joubert, M King, KJ Lim, T Liseau, R Lord, S Lorenzetti, D Molinari, S Naylor, DA Nisini, B Omont, A Orfei, R Patrick, T Pequignot, D Pouliquen, D Price, MC NguyenQRieu Robinson, FD Saisse, M Saraceno, P Serra, G Sidher, SD Smith, HA Spinoglio, L Texier, D Towlson, WA Trams, N Unger, SJ White, GJ TI Calibration and performance of the ISO Long-Wavelength Spectrometer SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE artificial satellites; instrumentation, spectrographs; infrared, general AB The wavelength and flux calibration, and the in-orbit performance of the Infrared Space Observatory Long-Wavelength Spectrometer (LWS) are described. The LWS calibration is mostly complete and the instrument's performance in orbit is largely as expected before launch. The effects of ionising radiation on the detectors, and the techniques used to minimise them are outlined. The overall sensitivity figures achieved in practice are summarised. The standard processing of LWS data is described. C1 UNIV LONDON QUEEN MARY & WESTFIELD COLL, LONDON E1 4NS, ENGLAND. ISO, SCI OPERAT CTR, LWS INSTRUMENT DEDICATED TEAM, VILLAFRANCA, SPAIN. OBSERV MARSEILLE, F-13248 MARSEILLE, FRANCE. UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. ASTRON SPATIALE LAB, F-13376 MARSEILLE, FRANCE. CTR ETUD SPATIALE RAYONNEMENTS, F-31029 TOULOUSE, FRANCE. CNR, IST FIS SPAZIO INTERPLANETARIO, I-00044 FRASCATI, ITALY. CALTECH, PASADENA, CA 91125 USA. NASA, AMES RES CTR, ASTROPHYS BRANCH 2456, DIV SPACE SCI, MOFFETT FIELD, CA 94035 USA. UNIV PARIS 11, F-91405 ORSAY, FRANCE. UNIV SASKATCHEWAN, INST SPACE & ATMOSPHER STUDIES, SASKATOON, SK S7N 5E2, CANADA. USN, RES LAB, REMOTE SENSING DIV, WASHINGTON, DC 20375 USA. SMITHSONIAN INST, ASTROPHYS LAB, NATL AIR & SPACE MUSEUM, WASHINGTON, DC 20560 USA. CNES, F-75001 PARIS, FRANCE. STOCKHOLM OBSERV, S-13336 SALTSJOBADEN, SWEDEN. CALTECH, IPAC, PASADENA, CA 91125 USA. OSSERV ASTRON ROMA, I-00040 MONTE PORZIO CATO, ITALY. UNIV LETHBRIDGE, DEPT PHYS, LETHBRIDGE, AB T1K 3M4, CANADA. INST ASTROPHYS, F-75014 PARIS, FRANCE. MULLARD SPACE SCI LAB, DORKING RH5 6NT, SURREY, ENGLAND. OBSERV PARIS, SECT ASTROPHYS, F-92190 PARIS, FRANCE. OBSERV PARIS, F-75014 PARIS, FRANCE. NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD 20771 USA. RP Swinyard, BM (reprint author), RUTHERFORD APPLETON LAB, DIDCOT OX11 0QX, OXON, ENGLAND. RI Barlow, Michael/A-5638-2009; Colgan, Sean/M-4742-2014; Molinari, Sergio/O-4095-2016 OI Barlow, Michael/0000-0002-3875-1171; Molinari, Sergio/0000-0002-9826-7525 NR 6 TC 107 Z9 107 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1996 VL 315 IS 2 BP L43 EP L48 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU266 UT WOS:A1996VU26600004 ER PT J AU Troland, TH Crutcher, RM Goodman, AA Heiles, C Kazes, I Myers, PC AF Troland, TH Crutcher, RM Goodman, AA Heiles, C Kazes, I Myers, PC TI The magnetic fields in the Ophiuchus and Taurus molecular clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, clouds; ISM, individual (rho Ophiuchi, Taurus); ISM, magnetic fields; ISM, molecules; polarization; stars, formation ID DENSE INTERSTELLAR CLOUDS; RHO-OPHIUCHI; DARK CLOUD; STAR FORMATION; AMBIPOLAR DIFFUSION; CORES; GAS; COMPLEX; BARNARD-1; CHEMISTRY AB We discuss the significance of previously published OH Zeeman effect measurements of the magnetic field in the rho Oph cloud (L1688) and also a new OH Zeeman effect measurement for the dark cloud core TMC-1C, the latter obtained with the Arecibo telescope. Results for both of these clouds, like previously published OH Zeeman results for other dark clouds, show that the line-of-sight field strength /B-parallel to/ less than or equal to 10 mu G. The rho Oph cloud is significantly higher in column density than other clouds studied, and recent H I Zeeman effect observations have revealed B-parallel to approximate to +10 mu G in the H I self-absorption region in front of the II derived from the OH Zeeman effect may indicate that OH poorly samples cloud. The low values of B-parallel to derived from the OH Zeeman effect may indicate that OH poorly samples the dense gas in the rho Oph cloud, or else that the cloud is in a state of supercritical collapse. The TMC-IC cloud core may have formed via ambipolar diffusion in a manner similar to recent modeling of dark cloud Barnard 1. C1 UNIV ILLINOIS, DEPT ASTRON, URBANA, IL 61801 USA. HARVARD UNIV, DEPT ASTRON, CAMBRIDGE, MA 02138 USA. UNIV CALIF BERKELEY, DEPT ASTRON, BERKELEY, CA 94720 USA. OBSERV PARIS, MEUDON SECT, F-92195 MEUDON, FRANCE. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV KENTUCKY, DEPT PHYS & ASTRON, LEXINGTON, KY 40506 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 38 TC 41 Z9 41 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 1996 VL 471 IS 1 BP 302 EP 307 DI 10.1086/177970 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VP223 UT WOS:A1996VP22300023 ER PT J AU Liu, WH Dalgarno, A AF Liu, WH Dalgarno, A TI Formation and destruction of silicon monoxide in SN 1987A SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular processes; supernovae, individual (SN 1987A) ID RADIATIVE ASSOCIATION; CARBON-MONOXIDE; CROSS-SECTIONS; SN-1987A; ATOMS; IONS; HE+; C+; CO AB We present a new chemistry model for the silicon monoxide molecules in SN 1987A. It incorporates an enhanced rate of formation by radiative association and an enhanced rate of destruction through charge transfer between SiO and Ar+ and Ne+, which is more efficient than the energetic electron impact ionization and dissociation in a previous model. The conclusion is unchanged that the 10(-4) - 10(-3) M(Theta) of SiO observed in SN 1987A can be produced by chemistry models in which there is no microscopic mixing of helium into the silicon-oxygen region of the ejecta. RP Liu, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 26 TC 22 Z9 22 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 1996 VL 471 IS 1 BP 480 EP 484 DI 10.1086/177982 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VP223 UT WOS:A1996VP22300035 ER PT J AU Tennyson, J AF Tennyson, J TI Resonance parameters and quantum defects for superexcited H-2 SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID ELECTRON-SCATTERING; RYDBERG STATES; MOLECULES; PHOTOIONIZATION; COLLISIONS; EXCITATION; HYDROGEN AB The results of R-matrix calculations on electron collisions with H-2(+) are presented. These calculations include the three lowest states of H-2(+) ((2) Sigma(g)(+), (2) Sigma(u)(+) and (2) Pi(u)). Positions and widths of the Feshbach resonances converging to both the (2) Sigma(u)(+) and (2) Pi(u) states are given, as are autoionization branching ratios for resonances lying above the (2) Sigma(u)(+): state. Complex quantum defects, calculated by performing scattering calculations above threshold, are presented for all three states considered. Results are tabulated for 12 symmetries ((1) Sigma(g)(+), (1) Sigma(u)(+), (1) Pi(u), (1) Pi(g), (1) Delta(g), (1) Delta(u), (3) Sigma(g)(+), (3) Sigma(u)(+), (3) Pi(u), (3) Pi(g), (3) Delta(g), (3) Delta(u)) and 13 internuclear separations from 1 to 4 a(0). (C) 1996 Academic Press, Inc. C1 UNIV LONDON UNIV COLL,DEPT PHYS & ASTRON,LONDON WC1E 6BT,ENGLAND. RP Tennyson, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Tennyson, Jonathan/I-2222-2012 OI Tennyson, Jonathan/0000-0002-4994-5238 NR 20 TC 87 Z9 87 U1 0 U2 3 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD NOV PY 1996 VL 64 IS 2 BP 253 EP 277 DI 10.1006/adnd.1996.0023 PG 25 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA VZ367 UT WOS:A1996VZ36700004 ER PT J AU Kensley, B AF Kensley, B TI New thalassinidean shrimp from the Pacific Ocean (Crustacea: Decapoda: Axiidae and Calocarididae) SO BULLETIN OF MARINE SCIENCE LA English DT Article AB One new genus (Marianaxius) and seven new species of axiid shrimps, and one new calocaridid species are recorded from scattered sites around the Pacific Ocean. The axiid species include Axiopsis bythos from the Philippines; Bouvieraxius springeri from the Sulu Sea; Eiconaxius albatrossae from Pacific Panama; Eiconaxius baja from Baja California; Eiconaxius kimbla from Queensland, Australia; and Marianaxius kroppi from Guam. Eiconaxius cristagalli (Faxon), originally described from Pacific Panama, is recorded from the Galapagos Islands. The new species of calocaridid, Ambiaxius japonicus, is recorded from Japan. RP Kensley, B (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 23 TC 21 Z9 24 U1 0 U2 1 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD NOV PY 1996 VL 59 IS 3 BP 469 EP 489 PG 21 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA VW934 UT WOS:A1996VW93400002 ER PT J AU Sadeghpour, HR AF Sadeghpour, HR TI Theory of double photoionization in ''two-electron'' systems SO CANADIAN JOURNAL OF PHYSICS LA English DT Article; Proceedings Paper CT International Symposium on (e,2e) Collisions, Double Photoionization, and Related Topics CY AUG 03-05, 1995 CL UNIV BRITISH COLUMBIA, VANCOUVER, CANADA HO UNIV BRITISH COLUMBIA ID HIGH-ENERGY PHOTON; DIFFERENTIAL CROSS-SECTIONS; DOUBLE-IONIZATION; ANGULAR-DISTRIBUTIONS; COMPTON-SCATTERING; MOLECULAR-HYDROGEN; ATOM IONIZATION; THRESHOLD LAW; 2 ELECTRONS; RARE-GASES AB Theory of double photoionization of atoms and molecules with two active electrons is reviewed. The emphasis is on advances toward theoretical understanding of new developments in laboratory observations. RP Sadeghpour, HR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 61 TC 9 Z9 9 U1 1 U2 1 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD NOV-DEC PY 1996 VL 74 IS 11-12 BP 727 EP 735 PG 9 WC Physics, Multidisciplinary SC Physics GA WA940 UT WOS:A1996WA94000005 ER PT J AU Yoshino, K Esmond, JR Parkinson, WH Ito, K Matsui, T AF Yoshino, K Esmond, JR Parkinson, WH Ito, K Matsui, T TI Absorption cross section measurements of water vapor in the wavelength region 120 to 188 nm SO CHEMICAL PHYSICS LA English DT Article ID AERONOMIC DISSOCIATION; PHOTOABSORPTION; MESOSPHERE; BANDS AB Laboratory measurements of the relative absorption cross sections of H2O at the temperature 295 K have been made throughout the wavelength region 120 to 188 nm. Laboratory measurements of the absolute absorption cross sections of H2O at 295 K have been made at 19 different wavelengths in the region 120 to 188 nm, and these absolute values have been used to put the relative cross section measurements of H2O at 295 K on an absolute basis. C1 NATL LAB HIGH ENERGY PHYS,PHOTON FACTORY,TSUKUBA,IBARAKI 305,JAPAN. RP Yoshino, K (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 17 TC 49 Z9 50 U1 4 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD NOV 1 PY 1996 VL 211 IS 1-3 BP 387 EP 391 DI 10.1016/0301-0104(96)00210-8 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA VR360 UT WOS:A1996VR36000034 ER PT J AU Shulman, MJ Robertson, DR AF Shulman, MJ Robertson, DR TI Changes in the coral reefs of San Blas, Caribbean Panama: 1983 to 1990 SO CORAL REEFS LA English DT Article ID DIADEMA-ANTILLARUM PHILIPPI; MASS MORTALITY; SEA-URCHIN; COMMUNITY STRUCTURE; ECHINODERMATA; ECHINOIDEA; RESPONSES; JAMAICA; COAST AB Between 1983-1990 large changes in abundances of corals and macroalgae occurred on shallow (1-5 m) lagoonal reefs in the San Bias Islands of Panama. In 1983 these reefs were dominated by the vertical plate forms of the coral genera Agaricia and Millepora. By 1990 we observed the following major changes: (1) loss of approximately one-half of the initial live coral cover, primarily during 1983-1986, and almost completely due to a decline in the abundance of Agaricia. Corals only occupied 12-26% of the reef area by 1990. (2) Macroalgae (mostly Dictyota and Halimeda) increased from similar to 2% cover in 1983 to 28% cover in 1990. (3) Microalgal cover increased two to ten-fold between 1983 and 1986, then declined to 50% greater than the initial values by 1990. There are at least three contributors to these changes in the benthic community: (1) a coral bleaching event in 1983, which disproportionately affected Agaricia; (2) the mass mortality of Diadema antillarum in 1983, which led to decreases in grazing pressure on algae; and (3) possible increases in sediment and nutrient loads due to runoff from deforested mountainsides. Temporal patterns and observations of interactions suggest that the decrease in Diadema herbivory is a major factor in this shift in coral and algal populations. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 35 TC 69 Z9 71 U1 2 U2 13 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD NOV PY 1996 VL 15 IS 4 BP 231 EP 236 DI 10.1007/s003380050048 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA VW920 UT WOS:A1996VW92000008 ER PT J AU Adey, WH Luckett, C Smith, M AF Adey, WH Luckett, C Smith, M TI Purification of industrially contaminated groundwaters using controlled ecosystems SO ECOLOGICAL ENGINEERING LA English DT Article DE ecotoxicology; microcosmology; algal turf scrubber; chemical pollution ID AQUATIC ENVIRONMENT; ORGANIC CONTAMINANTS; DRINKING-WATER; TETRACHLOROETHYLENE; TRICHLOROETHYLENE; DECOMPOSITION; FATE AB Pollution of ground and surface waters by industrial processes is a widespread and very serious environmental issue. While solutions exist to many of these problems, they frequently remain unused because of high costs often related to the broad spectrum of chemistry involved at individual sites. This paper presents, at bench scale, an amelioration procedure involving miniature ecosystems controlled by algal turf scrubbing (ATS) as applied to contaminated groundwater from a New Jersey (USA) industrial site. The groundwater, with a COD of 1300 mg/l and a TSS of 2000 mg/l, presented a broad array of inorganic elements including magnesium, iron and manganese and minor heavy metals with a suite of twenty synthetic organic compounds. The organic compounds included trichloroethylene, vinyl chloride and acetone, among others, for a concentration averaging 1071 mg/l. On the first experimental run, using metal halide lighting for driving algal photosynthesis, the ATS/microcosm process described herein purified the contaminated water to drinking water standards for all inorganic elements and organic compounds except trichloroethylene and dichloroethylene. Subsequent runs, with low levels of W-B applied to the ATS, achieved full drinking water standards. An examination of losses due to volatilization showed that minor losses of chlorinated hydrocarbons were also largely avoided with the addition of UV-B. Vinyl chloride was not detected in significant quantities in the volatile suite taken from air over the ATS unit either before or after the supplemental addition of UV-B. ATS is a low-cost ecotechnology that combines metabolic and adsorptive uptake by algae, precipitation at high pH and degradation under a saturated oxygen/UV radiation regime to ameliorate complex industrial wastewaters. RP Adey, WH (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,MARINE SYST LAB,WASHINGTON,DC 20560, USA. NR 36 TC 28 Z9 30 U1 3 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 J9 ECOL ENG JI Ecol. Eng. PD NOV PY 1996 VL 7 IS 3 BP 191 EP 212 DI 10.1016/0925-8574(96)00008-0 PG 22 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA VT624 UT WOS:A1996VT62400003 ER PT J AU Wing, SL Greenwood, D AF Wing, SL Greenwood, D TI Eocene continental climates and latitudinal temperature gradients: Reply SO GEOLOGY LA English DT Article C1 VICTORIA UNIV TECHNOL,DEPT ENVIRONM MANAGEMENT,MELBOURNE,VIC 3000,AUSTRALIA. RP Wing, SL (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,NHB121,WASHINGTON,DC 20560, USA. RI Greenwood, David/C-2758-2008; OI Greenwood, David/0000-0002-8569-9695; Wing, Scott/0000-0002-2954-8905 NR 4 TC 6 Z9 6 U1 0 U2 5 PU GEOLOGICAL SOC AMERICA PI BOULDER PA PO BOX 9140 3300 PENROSE PLACE, BOULDER, CO 80301 SN 0091-7613 J9 GEOLOGY JI Geology PD NOV PY 1996 VL 24 IS 11 BP 1054 EP 1055 PG 2 WC Geology SC Geology GA VW098 UT WOS:A1996VW09800025 ER PT J AU Mitchell, DL Ostro, SJ Hudson, RS Rosema, KD Campbell, DB Velez, R Chandler, JF Shapiro, II Giorgini, JD Yeomans, DK AF Mitchell, DL Ostro, SJ Hudson, RS Rosema, KD Campbell, DB Velez, R Chandler, JF Shapiro, II Giorgini, JD Yeomans, DK TI Radar observations of asteroids 1 Ceres, 2 Pallas, and 4 Vestal SO ICARUS LA English DT Article ID SPECKLE INTERFEROMETRY; IMAGES; SHAPE; POLE; SURFACE; SCATTERING; ALBEDO; SIZE; MARS; METEORITES AB Asteroids 1 Ceres, 2 Pallas, and 4 Vesta were observed with the 13-cm Arecibo radar and the 3.5-cm Goldstone radar during several apparitions between 1981 and 1995, These observations help to characterize the objects' surface properties. Echoes from Cere;: and Pallas are similar to 95% polarized (mu(C) = sigma(SC/)sigma(OC) approximate to 0.05) in the sense expected for specular (mirror) reflection yet broadly distributed in Doppler frequency, thus revealing surfaces that are smoother than the Moon at decimeter scales but much rougher (rms slopes > 20 degrees) on larger scales. Slopes on Ceres appear to be somewhat higher when viewed with the 3.5-cm wavelength, a trend that is observed for the terrestrial planets and the Moon, In contrast, echoes from Vesta are significantly depolarized, indicating substantial near-surface complexity at scales near 13 cm (mu(C) = 0.24 +/- 0.04) and 3.5 cm (mu(C) = 0.32 +/- 0.04), which is probably a consequence of Vesta's relatively strong basaltic surface material and may be a signature of large impact features inferred to be present on the surface. The low radar albedos of Ceres (<(sigma)over cap>(OC) = 0.042 +/- 0.006) and Pallas (<(sigma)over cap>(OC) = 0.075 +/- 0.011) are in the range expected for surfaces with a carbonaceous chondrite mineralogy. Pallas' distinctly higher albedo implies a similar to 35% higher surface density, which could result from a lower regolith porosity and/or a higher specific gravity (zero-porosity density), Given a porosity of 45%, the specific gravities of the surface materials on Ceres and Pallas would be similar to 2.3 and similar to 3.0 g cm(-3), respectively, which would be consistent with (1) the presence of an additional silicate component on Pallas' surface (as inferred from spectroscopic observations) and (2) recent mass estimates, which suggest a higher mean (volume-averaged) density for Pallas than for Ceres. (C) 1996 Academic Press, Inc. C1 WASHINGTON STATE UNIV,SCH ELECT ENGN & COMP SCI,PULLMAN,WA 99164. CORNELL UNIV,NATL ASTRON & IONOSPHERE CTR,ITHACA,NY 14853. NATL ASTRON & IONOSPHERE CTR,ARECIBO OBSERV,ARECIBO,PR 00613. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Mitchell, DL (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 78 TC 34 Z9 34 U1 1 U2 6 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 1996 VL 124 IS 1 BP 113 EP 133 DI 10.1006/icar.1996.0193 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE896 UT WOS:A1996WE89600008 ER PT J AU DiMichele, WA Eble, CF Chaney, DS AF DiMichele, WA Eble, CF Chaney, DS TI A drowned lycopsid forest above the Mahoning coal (Conemaugh Group, Upper Pennsylvanian) in eastern Ohio, USA SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Article ID SWAMP VEGETATION; PALEOECOLOGY; EURAMERICA; REPRODUCTION; ENVIRONMENT; ILLINOIS; LYCOPODS; HISTORY; BED AB Over 800 mud-filled casts of upright lycopsid tree stumps have been documented immediately above the Mahoning coal in an active underground mine located in northwestern Jefferson County, Ohio. The coal body originated as a pod-shaped peat body of similar to 60 km(2). Trees are rooted at several levels within a thin (15-40 cm) bone coal directly above the banded coal; they extend upward up to 15 cm into overlying, flat-bedded, carbonaceous mudstones that coarsen up. From a maximum basal diameter of 1.2 m, stumps taper upward to diameters no less than 0.3 m. Within single-entry transects, < 6 m wide that total 2585 m in length, stumps are randomly distributed. The trees are identified as lepidodendrids on the basis of gross morphology, external stem patterns, and attached stigmarian root systems, and provisionally as Lepidophloios or Lepidodendron by associated palynology of the enclosing matrix. Palynological analyses of incremental seam samples indicate an initial dominance of lycopsid spores with lepidodendracean affinities (Lycospora granulata from Lepidophloios hallii), replaced upwards by tree-fern spores, with a reoccurrence of lepidodendracean spores in the upper benches; spores of Sigillaria (Crassispora) are abundant only at the base of the coal. Petrographic analyses indicate a parallel trend from vitrinite-rich to inertinite- and liptinite-rich upward in the coal body. All data indicate that the peat represented by the Mahoning coal was drowned slowly. During the earliest stages of inundation, a lycopsid forest was re-established, only to be subsequently drowned. C1 UNIV KENTUCKY,KENTUCKY GEOL SURVEY,LEXINGTON,KY 40506. RP DiMichele, WA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL MRC 121,WASHINGTON,DC 20560, USA. RI DiMichele, William/K-4301-2012 NR 41 TC 31 Z9 31 U1 1 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD NOV PY 1996 VL 31 IS 1-4 BP 249 EP 276 DI 10.1016/S0166-5162(96)00019-5 PG 28 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA VV654 UT WOS:A1996VV65400012 ER PT J AU Kensley, B AF Kensley, B TI The genus Ptilanthura in the western Atlantic: Evidence for primary males and description of a new species (Isopoda: Anthuridae) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB The genus Ptilanthura is redefined. The type species, P. tenuis is redescribed, with the aid of more than 500 specimens. Ptilanthura tricarina Menzies and Frankenburg, 1966, is synonymized with the earlier P. tenuis Harger, 1878. Size-frequency distributions indicate the presence of primary and secondary males in this species. A second species of the genus, P. colpos, described from the eastern Gulf of Mexico, differs from P. tenuis in body proportions, shape of the pleotelson, and in several features of the appendages. RP Kensley, B (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 16 TC 4 Z9 4 U1 0 U2 0 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD NOV PY 1996 VL 16 IS 4 BP 763 EP 781 DI 10.2307/1549195 PG 19 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA VR912 UT WOS:A1996VR91200013 ER PT J AU Zhao, L Mulkern, R Tseng, CH Williamson, D Patz, S Kraft, R Walsworth, RL Jolesz, FA Albert, MS AF Zhao, L Mulkern, R Tseng, CH Williamson, D Patz, S Kraft, R Walsworth, RL Jolesz, FA Albert, MS TI Gradient-echo imaging considerations for hyperpolarized Xe-129 MR SO JOURNAL OF MAGNETIC RESONANCE SERIES B LA English DT Article ID LASER-POLARIZED XE-129; VARIABLE FLIP ANGLES; SPIN RELAXATION; RARE SEQUENCES; NMR; DIFFUSION; CONTRAST; ARTIFACT; SIGNAL; FLASH C1 BRIGHAM & WOMENS HOSP,DEPT RADIOL,BOSTON,MA 02115. HARVARD UNIV,SCH MED,BOSTON,MA 02115. BOSTON UNIV,DEPT BIOMED ENGN,BOSTON,MA 02215. CHILDRENS HOSP,DEPT RADIOL,BOSTON,MA 02215. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RI Patz, Samuel/I-2879-2012 NR 25 TC 138 Z9 140 U1 3 U2 22 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 1064-1866 J9 J MAGN RESON SER B JI J. Magn. Reson. Ser. B PD NOV PY 1996 VL 113 IS 2 BP 179 EP 183 DI 10.1006/jmrb.1996.0173 PG 5 WC Physics, Atomic, Molecular & Chemical SC Physics GA VX448 UT WOS:A1996VX44800011 PM 11543610 ER PT J AU Travers, MJ Chen, W Novick, SE Vrtilek, JM Gottlieb, CA Thaddeus, P AF Travers, MJ Chen, W Novick, SE Vrtilek, JM Gottlieb, CA Thaddeus, P TI Structure of the cumulene carbene butatrienylidene: H2CCCC SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID ASTRONOMICAL DETECTION; EQUILIBRIUM GEOMETRY; LABORATORY DETECTION; SPECTROSCOPY; PROPADIENYLIDENE AB The microwave rotational spectra of the J = 1 <-- 0 and 2 <-- 1 transitions of six isotopic species of the singlet carbene butatrienylidene (H2CCCC, (H2CCCC)-C-13, (H2CCCC)-C-13, (H2CCCC)-C-13, (H2CCCC)-C-13, and D2CCCC) were measured with a Fourier-transform microwave spectrometer and the r(o) and r(s) structures were determined. Both structures are consistent with a cumulenic carbon-chain backbone. Our empirical structure is r(s)(HC(1)) = 1.079 +/- 0.002 Angstrom, r(s)(C-(1)C-(2)) = 1.306 +/- 0.004 Angstrom, r(s)(C-(2)C-(3)) = 1.294 +/- 0.004 Angstrom, r(s)(C-(3)C-(4)) = 1.278 +/- 0.004 Angstrom, and angle(s)HC((1))H = 119.4 +/- 0.4 degrees. Except for the CC bond closest to the carbene carbon, r(s)(C-(3)C-(4)), an equilibrium geometry determined in a high-level ab initio calculation (M. Oswald and P. Botschwina, J. Mol. Spectrosc. 169, 181 (1995)) is in very good agreement with the experimental structure. (C) 1996 Academic Press, Inc. C1 HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. WESLEYAN UNIV,DEPT CHEM,MIDDLETOWN,CT 06459. RP Travers, MJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 TC 20 Z9 20 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD NOV PY 1996 VL 180 IS 1 BP 75 EP 80 DI 10.1006/jmsp.1996.0225 PG 6 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA VP270 UT WOS:A1996VP27000008 ER PT J AU Thorington, RW Darrow, K AF Thorington, RW Darrow, K TI Jaw muscles of old world squirrels SO JOURNAL OF MORPHOLOGY LA English DT Article ID MECHANICS; RAT AB The jaw, suprahyoid, and extrinsic tongue muscles were studied in 11 genera, belonging to five tribes, of Old World squirrels. Significant variation in most of the adductor muscles is evident. The most primitive state of sciuromorphy is seen in the African tree squirrels Paraxerus and Funisciurus, especially as reflected in the anterior deep masseter. A derived state of sciuromorphy is found in five genera of Old World squirrels and perhaps evolved independently in each. Reduction of the temporalis muscle was observed in three genera, distantly related to one another. A unique arrangement of the superficial masseter is reported in the Asian giant tree squirrels, Ratufa. The arrangement of the masseter in the African pygmy squirrel, Myosciurus, is very similar to that of the South American pygmy squirrel, Sciurillus. We present hypotheses about the functional significance of these differences. In the derived state of sciuromorphy, which is found in three cases in squirrels that feed extensively on hard fruits, the anterior deep masseter is well positioned to increase the strength of the power stroke of the incisor bite. Among the pygmy squirrels, the position of the anterior deep masseter suggests that it plays a more significant role in molar chewing. (C) 1996 Wiley-Liss, Inc. RP Thorington, RW (reprint author), SMITHSONIAN INST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 32 TC 36 Z9 39 U1 0 U2 4 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD NOV PY 1996 VL 230 IS 2 BP 145 EP 165 DI 10.1002/(SICI)1097-4687(199611)230:2<145::AID-JMOR3>3.0.CO;2-G PG 21 WC Anatomy & Morphology SC Anatomy & Morphology GA VR405 UT WOS:A1996VR40500003 PM 8921609 ER PT J AU Waller, TR AF Waller, TR TI Bridging the gap between the eastern Atlantic and eastern Pacific: A new species of Crassadoma (Bivalvia: Pectinidae) in the Pliocene of Florida SO JOURNAL OF PALEONTOLOGY LA English DT Article ID CHLAMYS MOLLUSCA; MARINE; AGE AB Crassadoma monroensis new species (Mollusca: Bivalvia: Pectinidae), from the lower upper Pliocene Ochopee Limestone Member of the Tamiami Formation of southern Florida, is the first undoubted member of the genus Crassadoma Bernard, 1986, to be discovered in the Neogene on the eastern side of the Americas. The new species was likely byssate, not cemented, and fills the geographic gap between ancestral members of the tribe Crassadomini in the eastern Atlantic and Crassadoma gigantea, the giant cemented species that lives along the western shores of North America. RP Waller, TR (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 60 TC 5 Z9 5 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI ITHACA PA 1259 TRUMANSBURG ROAD, ITHACA, NY 14850 SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD NOV PY 1996 VL 70 IS 6 BP 941 EP 946 PG 6 WC Paleontology SC Paleontology GA VV631 UT WOS:A1996VV63100007 ER PT J AU Windsor, DM Jolivet, P AF Windsor, DM Jolivet, P TI Aspects of the morphology and ecology of two Panamanian ant-plants, Hoffmannia vesciculifera (Rubiaceae) and Besleria formicaria (Gesneriaceae) SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE ant-plants; Besleria formicaria; Hoffmannia vesciculifera; Panama; Pheidole sp; Solenopsis sp AB Two formicarial ant-plants endemic to Panama and adjacent areas of Costa Rica co-occur in mid-elevation cloud forest yet have distinctive modifications to house and feed small, retiring ants. Besleria formicaria (Gesneriaceae) hosts only Pheidole sp, which harvest the oil-rich seeds of its host and other plants and insect parts. Hoffmannia vesciculifera (Rubiaceae) hosts only Solenopsis sp. ants which obtain lipid and possibly other nutrients from vescicular tissues. Judging by their abundance in refuse deposits, fern sporangia appear to be a plentiful and evenly distributed resource exploited by both ant species. RP Windsor, DM (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA ANCON,PANAMA. NR 21 TC 2 Z9 2 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD NOV PY 1996 VL 12 BP 835 EP 842 PN 6 PG 8 WC Ecology SC Environmental Sciences & Ecology GA VW924 UT WOS:A1996VW92400007 ER PT J AU Jordan, HL Howard, J Sellon, RK Wildt, DE Tompkins, WA KennedyStoskopf, S AF Jordan, HL Howard, J Sellon, RK Wildt, DE Tompkins, WA KennedyStoskopf, S TI Transmission of feline immunodeficiency virus in domestic cats via artificial insemination SO JOURNAL OF VIROLOGY LA English DT Article ID HTLV-III; INFECTION; SEMEN; MODEL; PREVALENCE; DISEASE; EMBRYO; AIDS AB The objective of this study was to determine whether semen from male domestic cats infected with feline immunodeficiency virus (FIV) can transmit virus to females, Twelve inseminations were pel formed by an intrauterine laparoscopic technique with fresh or cryopreserved electroejaculates from asymptomatic males chronically infected with the NCSU1 strain of FIV. Of sis inseminations performed with fresh semen, three resulted in infection of queens, as indicated by seroconversion, expression of FIV gag provirus in peripheral blood leukocytes, and reduced peripheral CD4(+)/CD8(+) T-lymphocyte ratios. None of the six inseminates with thawed cryopreserved semen resulted in infection. Two infected queens and one uninfected queen became pregnant. Virus was not evident in the seven offspring. We conclude that FIV can be transmitted horizontally by artificial insemination with fresh semen. C1 N CAROLINA STATE UNIV, COLL VET MED, DEPT MICROBIOL PATHOL & PARASITOL, RALEIGH, NC 27606 USA. N CAROLINA STATE UNIV, COLL VET MED, DEPT COMPAN ANIM & SPECIAL SPECIES MED, RALEIGH, NC 27606 USA. SMITHSONIAN INST, NATL ZOOL PK, WASHINGTON, DC 20008 USA. SMITHSONIAN INST, CONSERVAT & RES CTR, WASHINGTON, DC 20560 USA. FU NCRR NIH HHS [1 K01 RR00109-01A1]; NIAID NIH HHS [R01 AI32310-02, K11 AI01122-01A1] NR 39 TC 21 Z9 21 U1 0 U2 2 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0022-538X J9 J VIROL JI J. Virol. PD NOV PY 1996 VL 70 IS 11 BP 8224 EP 8228 PG 5 WC Virology SC Virology GA VL792 UT WOS:A1996VL79200106 PM 8892958 ER PT J AU ArandaGomez, JJ Luhr, JF AF ArandaGomez, JJ Luhr, JF TI Origin of the Joya Honda maar, San Luis Potosi, Mexico SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE maars; phreatomagmatism; Mexico; pyroclastic surges; volcanic breccia; San Luis Potosi, Mexico; aquifers ID QUATERNARY VOLCANIC CENTERS; EVOLUTION; PETROLOGY; MAGMA AB Joya Honda is a Quaternary maar of unusual type from the Mexican Basin and Range Province. Its similar to 300-m-deep crater is excavated in Cretaceous limestones. The surrounding tephra deposit, which in places is > 100 m thick, begins with a series of weakly indurated pyroclastic-surge and -fall layers that we interpret as dry-surge deposits. These are overlain by the main sequence of strongly indurated, massive tuff breccias that we interpret as wet-surge deposits. Joya Honda formed subaerially from the interaction of groundwater with rapidly ascending intraplate-type basanitic magma carrying peridotitic mantle xenoliths. Local aquifer characteristics controlled the style of eruption and the nature of the deposits. Groundwater in the limestone-hosted aquifer beneath Joya Honda was apparently contained within solution-enhanced fractures. At the onset of the eruption, magma began to interact with a moderate amount of groundwater, producing the dry-surge deposits, which are typical of deposits found at many maars and tuff rings. As the eruption continued, the crater grew and the hydromagmatic blasts fractured the limestones around the explosion foci. A marked increase in the water/magma ratio of the system followed when a large fracture or a portion of the limestone with enhanced secondary permeability was intersected by the expanding crater. Subsequent phreatomagmatic explosions occurred in a system with groundwater flow rates several orders of magnitude larger than in the initial dry-surge stage. At the maar rim these wet eruptions led to the emplacement of massive tuff breccias through a combination of fallout, steeply dipping tuff breccias are similar to deposits found at many tuff cones. Juvenile clasts in the near-vent deposits show marked upward increases in both hydration (palagonitization) and vesicularity. The increased palagonitization with height in the section appears to be a consequence of the overall increased wetness of the eruption with time, correlating with greater carbonate cementation and lithification in the upper part of the deposit. The transition toward higher vesicularity is interpreted as evidence of a gradual reduction in the confining pressure for the ascending magma prior to explosive fragmentation, perhaps related to unroofing during progressive excavation of the overlying maar crater. Thus, Joya Honda does not support maar-formation models that invoke downward displacement of explosion foci, caused by formation of a cone of depression in the aquifer, in order to maintain the confining pressure for the hydromagmatic blasts. C1 SMITHSONIAN INST, DEPT MINERAL SCI, WASHINGTON, DC 20560 USA. RP ArandaGomez, JJ (reprint author), UNIV NACL AUTONOMA MEXICO, INST GEOL, ESTAC REG CTR, GUANAJUATO 36000, GTO, MEXICO. NR 48 TC 53 Z9 53 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD NOV PY 1996 VL 74 IS 1-2 BP 1 EP 18 DI 10.1016/S0377-0273(96)00044-3 PG 18 WC Geosciences, Multidisciplinary SC Geology GA VV200 UT WOS:A1996VV20000001 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI A critic writes: Selected essays - Banham,R SO LIBRARY JOURNAL LA English DT Book Review RP Kalfatovic, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 1 PY 1996 VL 121 IS 18 BP 63 EP 63 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VT170 UT WOS:A1996VT17000045 ER PT J AU Petaev, MI AF Petaev, MI TI The search for exsolved ferromagnesian olivines: A meteoritic survey SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DIVNOE METEORITE; PETROLOGY AB Olivine grains from selected meteorites (the Springwater pallasite, the Lowicz mesosiderite, the ALH 84025 brachinite, the Krymka LL3 chondrite, and the Calcalong Creek lunar meteorite) and terrestrial rocks (San Carlos forsterite and Rockport fayalite) were studied by optical microscopy and high-precision electron microprobe analysis. Detailed microprobe traverses revealed regular igneous zoning in the Krymka and Calcalong Creek olivines. Traverses across the San Carlos forsterite grain are flat and display no chemical variations larger than the 2 sigma range of counting error (+/- 0.2 mol% Fa). Traverses across olivine grains in the ALH 84025, Lowicz, and Springwater meteorites show regular patterns of periodic or wavy chemical variations well exceeding the 20 uncertainty range. However, no lamellar structure was seen in backscattered electron images. It is suggested that the periodic chemical variations may be due to spinodal decomposition of primary, more or less homogeneous grains. I conclude that the absence of earlier reports of such variations simply means that olivine grains in equilibrated meteorites have not been examined closely enough to detect them. RP Petaev, MI (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 20 TC 5 Z9 6 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 1996 VL 31 IS 6 BP 807 EP 815 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA VY468 UT WOS:A1996VY46800012 ER PT J AU Hershkovitz, MA Lewis, LA AF Hershkovitz, MA Lewis, LA TI Deep-level diagnostic value of the rDNA-ITS region SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE ITS; 5.8S; rDNA evolution; eukaryotes; maximum-likelihood; among-site rate variation ID RIBOSOMAL-RNA SEQUENCE; INTERNAL TRANSCRIBED SPACER-2; PHYLOGENETIC ANALYSIS; NUCLEOTIDE-SEQUENCES; STRUCTURAL ELEMENTS; GREEN-ALGAE; DNA; ORIGIN; GENE; 5.8S AB The similarity of certain reported angiosperm rDNA internal transcribed spacer (ITS) region sequences to those of green algae prompted our analysis of the deep-level phylogenetic signal in the highly conserved but short 5.8S and hypervariable ITS2 sequences. We found that 5.8S sequences yield phylogenetic trees similar to but less well supported than those generated by a ca. 10-fold longer alignment from rDNA-18S sequences, as well as independent evidence. We attribute this result to our finding that, compared to 18S, the 5.8S has a higher proportion of sites subject to vary and greater among-site substitution rate homogeneity. We also determined that our phylogenetic results are not likely affected by intramolecular compensatory mutation to maintain RNA secondary structure nor by evident systematic biases in base composition. Despite historical homology, there appears to be no ITS2 primary sequence similarity shared between fungi, green algae, and angiosperms. ITS2 sequences within each of these groups, however, share sufficient similarity to cluster correctly on the basis of alignability. Our results indicate that ITS region sequences can diagnose organismal origins and phylogenetic relationships at many phylogenetic levels and provide a useful paradigm for molecular evolutionary study. C1 SMITHSONIAN INST,LAB MOL SYSTEMAT,WASHINGTON,DC 20560. UNIV NEW MEXICO,DEPT BIOL,ALBUQUERQUE,NM 87131. RP Hershkovitz, MA (reprint author), NIH,NATL LIB MED,NCBI GENBANK,BLDG 38A,8600 ROCKVILLE PIKE,BETHESDA,MD 20984, USA. NR 55 TC 134 Z9 143 U1 0 U2 14 PU SOC MOLECULAR BIOLOGY EVOLUTION PI LAWRENCE PA PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD NOV PY 1996 VL 13 IS 9 BP 1276 EP 1295 PG 20 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA VR299 UT WOS:A1996VR29900014 PM 8896380 ER PT J AU Weil, SE AF Weil, SE TI To help think about museums more intensely + To stimulate insightful discussion about museums: Three warm-up exercises SO MUSEUM NEWS LA English DT Article C1 SMITHSONIAN INST,CTR MUSEUM STUDIES,WASHINGTON,DC. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSN MUSEUMS PI WASHINGTON PA 1225 EYE ST NW SUITE 200, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD NOV-DEC PY 1996 VL 75 IS 6 BP 44 EP 47 PG 4 WC Art SC Art GA VR794 UT WOS:A1996VR79400015 ER PT J AU Lubar, S AF Lubar, S TI Mickey-Mouse history and other essays on American memory - Wallace,M SO MUSEUM NEWS LA English DT Book Review RP Lubar, S (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DIV HIST TECHNOL,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSN MUSEUMS PI WASHINGTON PA 1225 EYE ST NW SUITE 200, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD NOV-DEC PY 1996 VL 75 IS 6 BP 57 EP & PG 0 WC Art SC Art GA VR794 UT WOS:A1996VR79400018 ER PT J AU Kosowsky, A Kamionkowski, M Jungman, G Spergel, DN AF Kosowsky, A Kamionkowski, M Jungman, G Spergel, DN TI Determining cosmological parameters from the microwave background SO NUCLEAR PHYSICS B LA English DT Article; Proceedings Paper CT 2nd Symposium on Dark Matter in the Universe CY FEB 14-16, 1996 CL SANTA MONICA, CA SP UCLA ID ANISOTROPIES AB Recently funded satellites will map the cosmic microwave background radiation with unprecedented sensitivities and angular resolutions. Assuming only primordial adiabatic scalar and tensor perturbations, we evaluate how accurately experiments of this type will measure the basic cosmological parameters Omega (the total density of the Universe), Omega(b) (the baryon density), h (the Hubble constant), and Lambda (the cosmological constant). The proposed experiments are capable of measuring these parameters at the few-percent level. We briefly discuss the generality of these estimates and complications arising in actual data analysis. C1 COLUMBIA UNIV,DEPT PHYS,NEW YORK,NY 10027. SYRACUSE UNIV,DEPT PHYS,SYRACUSE,NY 13244. PRINCETON UNIV,DEPT ASTROPHYS SCI,PRINCETON,NJ 08544. RP Kosowsky, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Spergel, David/A-4410-2011 NR 23 TC 10 Z9 10 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0550-3213 J9 NUCL PHYS B JI Nucl. Phys. B PD NOV PY 1996 SU 51B BP 49 EP 53 DI 10.1016/S0920-5632(96)00481-1 PG 5 WC Physics, Particles & Fields SC Physics GA VY665 UT WOS:A1996VY66500007 ER PT J AU Dzuba, VA Flambaum, VV Kozlov, MG AF Dzuba, VA Flambaum, VV Kozlov, MG TI Combination of the many-body perturbation theory with the configuration-interaction method SO PHYSICAL REVIEW A LA English DT Article ID NONCONSERVING OPTICAL-ROTATION; COUPLED-CLUSTER METHOD; E1 TRANSITION AMPLITUDES; ENERGY-LEVELS; CESIUM ATOM; PARITY NONCONSERVATION; PRECISION-MEASUREMENT; HYPERFINE-STRUCTURE; ELECTROWEAK THEORY; HARTREE-FOCK AB An ab initio method for high accuracy calculations for atoms with more than one valence electron is described. The effective Hamiltonian for the valence electrons is formed using many-body perturbation theory for the interaction of the valence electrons with the core. The configuration-interaction method is then used to find the energy levels of the atom. An application of this to thallium shows that the method gives an accuracy of about 0.5% for the ionization potential and a few tenths of a percent for the first few energy intervals. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. HARVARD UNIV,CAMBRIDGE,MA 02138. PETERSBURG NUCL PHYS INST,GATCHINA 188350,RUSSIA. RP Dzuba, VA (reprint author), UNIV NEW S WALES,SCH PHYS,SYDNEY,NSW 2052,AUSTRALIA. RI Kozlov, Mikhail/D-8963-2011 OI Kozlov, Mikhail/0000-0002-7751-6553 NR 40 TC 193 Z9 193 U1 0 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD NOV PY 1996 VL 54 IS 5 BP 3948 EP 3959 DI 10.1103/PhysRevA.54.3948 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA VT673 UT WOS:A1996VT67300036 ER PT J AU Derrickson, EM Jerrard, N Oftedal, O AF Derrickson, EM Jerrard, N Oftedal, O TI Milk composition of two precocial, arid-dwelling rodents, Kerodon rupestris and Acomys cahirinus SO PHYSIOLOGICAL ZOOLOGY LA English DT Article ID LACTATION; REPRODUCTION; PREGNANCY; NUTRITION; MAMMALS; PROTEIN AB We collected milk samples from two rodents Kerodon rupestris and Acomys cahirinus, that live in avid habitats and produce precocial young, in order to determine milk composition throughout the lactation period. Milk from species producing precocial young has been predicted to be low in energy and protein content, while milk from arid-dwelling species has been Predicted to be high in total solids. Milk samples were analyzed for total fat, protein, and sugar content. Milk from Acomys was much higher in energy content than Kerodon milk, exhibiting higher concentrations of total solids (41% vs. 20%), fat (21% vs. 6.9%), and protein (12% vs. 6.6%); however, sugar concentration was lower in Acomys milk (2.9% vs. 5.3%). Milk composition varied throughout the lactation period in both species with protein levels increasing and fat levels decreasing in Kerodon and sugar levels decreasing and total solids and fat levels increasing in Acomys. The milk of Kerodon females exhibited a threefold variation in fat content, while milk from Acomys females showed a twofold variation in protein content. The results of this study lend some support to the idea that mammals inhabiting arid environments conserve water by producing milk with a high proportion of solids. Furthermore, these results do not support the hypothesis that milk from rodents with precocial young is low in energy content but instead indicate that precocial species produce milk that is high in total solids and fat. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RP Derrickson, EM (reprint author), LOYOLA COLL,DEPT BIOL,BALTIMORE,MD 21210, USA. NR 43 TC 13 Z9 13 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0031-935X J9 PHYSIOL ZOOL JI Physiol. Zool. PD NOV-DEC PY 1996 VL 69 IS 6 BP 1402 EP 1418 PG 17 WC Physiology; Zoology SC Physiology; Zoology GA VU670 UT WOS:A1996VU67000006 ER PT J AU GonzalezMeler, MA Ribas-Carbo, M Siedow, JN Drake, BG AF GonzalezMeler, MA Ribas-Carbo, M Siedow, JN Drake, BG TI Direct inhibition of plant mitochondrial respiration by elevated CO2 SO PLANT PHYSIOLOGY LA English DT Article ID CARBON-DIOXIDE EFFLUX; DARK RESPIRATION; ATMOSPHERIC CO2; ROOT RESPIRATION; LEAF RESPIRATION; PEAR FRUIT; SHORT-TERM; GROWTH; SOIL; PATHWAYS AB Doubling the concentration of atmospheric CO2 often inhibits plant respiration, but the mechanistic basis of this effect is unknown. We investigated the direct effects of increasing the concentration of CO2 by 360 mu L L(-1) above ambient on O-2 uptake in isolated mitochondria from soybean (Glycine max L. cv Ransom) cotyledons. Increasing the CO2 concentration inhibited the oxidation of succinate, external NADH, and succinate and external NADH combined. The inhibition was greater when mitochondria were preincubated for 10 min in the presence of the elevated CO2 concentration prior to the measurement of O-2 uptake. Elevated CO2 concentration inhibited the salicylhydroxamic acid-resistant cytochrome pathway, but had no direct effect on the cyanide-resistant alternative pathway. We also investigated the direct effects of elevated CO2 concentration on the activities of cytochrome c oxidase and succinate dehydrogenase (SDH) and found that the activity of both enzymes was inhibited. The kinetics of inhibition of cytochrome c oxidase were time-dependent. The level of SDH inhibition depended on the concentration of succinate in the reaction mixture. Direct inhibition of respiration by elevated CO2 in plants and intact tissues may be due at least in part to the inhibition of cytochrome c oxidase and SDH. C1 DUKE UNIV, DEPT BOT, DURHAM, NC 27708 USA. RP GonzalezMeler, MA (reprint author), SMITHSONIAN ENVIRONM RES CTR, POB 28, EDGEWATER, MD 21037 USA. RI Ribas-Carbo, Miquel/N-1634-2013; OI Ribas-Carbo, Miquel/0000-0002-7337-2089; Gonzalez-Meler, Miquel/0000-0001-5388-7969 NR 42 TC 102 Z9 105 U1 6 U2 14 PU AMER SOC PLANT PHYSIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD NOV PY 1996 VL 112 IS 3 BP 1349 EP 1355 PG 7 WC Plant Sciences SC Plant Sciences GA VT975 UT WOS:A1996VT97500052 ER PT J AU Leitherer, C Alloin, D FritzVonAlvensleben, U Gallagher, JS Huchra, JP Matteucci, F OConnell, RW Beckman, JE Bertelli, GP Bica, E Boisson, C Bonatto, C Bothun, GD Bressan, A Brodie, JP Bruzual, G Burstein, D Buser, R Caldwell, N Casuso, E Cervino, M Charlot, S Chavez, M Chiosi, C Christian, CA Cuisinier, F Dallier, R deKoter, A Delisle, S Diaz, AI Dopita, MA Dorman, B Fagotto, F Fanelli, MN Fioc, M GarciaVargas, ML Girardi, L Goldader, JD Hardy, E Heckman, TM Iglesias, J Jablonka, P Joly, M Jones, L Kurth, O Lancon, A Lejeune, T Loxen, J Maeder, A Malagnini, ML Marigo, P MasHesse, JM Meynet, G Moller, CS Molla, ML Morossi, C Nasi, E Nichols, JS Odegaard, KJR Parker, JWM Pastoriza, MG Peletier, R Robert, C RoccaVolmerange, B Schaerer, D Schmidt, A Schmitt, HR Schommer, RA Schmutz, W Roos, MS Silva, L Stasinska, G Sutherland, RS Tantalo, R Traat, P Vallenari, A Vazdekis, A Walborn, NR Worthey, G Wu, CC AF Leitherer, C Alloin, D FritzVonAlvensleben, U Gallagher, JS Huchra, JP Matteucci, F OConnell, RW Beckman, JE Bertelli, GP Bica, E Boisson, C Bonatto, C Bothun, GD Bressan, A Brodie, JP Bruzual, G Burstein, D Buser, R Caldwell, N Casuso, E Cervino, M Charlot, S Chavez, M Chiosi, C Christian, CA Cuisinier, F Dallier, R deKoter, A Delisle, S Diaz, AI Dopita, MA Dorman, B Fagotto, F Fanelli, MN Fioc, M GarciaVargas, ML Girardi, L Goldader, JD Hardy, E Heckman, TM Iglesias, J Jablonka, P Joly, M Jones, L Kurth, O Lancon, A Lejeune, T Loxen, J Maeder, A Malagnini, ML Marigo, P MasHesse, JM Meynet, G Moller, CS Molla, ML Morossi, C Nasi, E Nichols, JS Odegaard, KJR Parker, JWM Pastoriza, MG Peletier, R Robert, C RoccaVolmerange, B Schaerer, D Schmidt, A Schmitt, HR Schommer, RA Schmutz, W Roos, MS Silva, L Stasinska, G Sutherland, RS Tantalo, R Traat, P Vallenari, A Vazdekis, A Walborn, NR Worthey, G Wu, CC TI A data base for galaxy evolution modeling SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Review ID INTERMEDIATE-MASS STARS; ASYMPTOTIC GIANT BRANCH; STELLAR POPULATION SYNTHESIS; RADIATION-DRIVEN WINDS; THEORETICAL ISOCHRONES; GALACTIC NUCLEI; HII-REGIONS; LOSS RATES; SPECTRAL PROPERTIES; GLOBULAR-CLUSTERS AB This paper represents a collective effort to provide an extensive electronic data base useful for the interpretation of the spectra and evolution of galaxies. A broad variety of empirical and theoretical data is discussed here, and the data are made fully available in the AAS CD-ROM Series, Vol. 7. Several empirical stellar libraries are part of this data base. They cover the ultraviolet spectral range observed with IUE, optical data from different ground-based telescopes, and ground-based infrared data. Spectral type coverage depends on the wavelength, but is mostly complete for types O to M and luminosity classes V to I. A large metallicity range is covered as well. Theoretical libraries of selected spectral indices of cool stars and of stellar continuum fluxes in the temperature range 2000-50,000 K as well as Wolf-Rayet energy distributions are presented. Several libraries of star clusters and early-type galaxies have been selected for this data base. We discuss an extensive set of empirical spectral templates covering the wavelength region from 1200 to 9800 Angstrom, as well as narrow-band line indices in a large number of passbands. Bench-mark spectra of nearby galaxies for model tests are included as well. We compiled numerous evolutionary models and isochrones for stars of all mass ranges of interest, wide metallicity range, and for all evolutionary phases, including the pre-main-sequence phase. The majority of the models have been computed by the Geneva and Padova groups. Evolutionary synthesis models computed by several independent groups are made available. They can be applied to old and young systems, and are optimized with respect to different aspects of input physics. The model predictions include stellar (colors, magnitudes, absorption features) and nebular (emission-line fluxes) properties. Finally, we present models of ionized gas to be used for the interpretation of active galactic nuclei and young star-forming galaxies. The community is encouraged to make use of this electronic data base and to perform a critical comparison between the individual datasets. C1 CEA SACLAY, SERV ASTROPHYS, F-91191 GIF SUR YVETTE, FRANCE. UNIV STERNWARTE GOTTINGEN, D-37083 GOTTINGEN, GERMANY. UNIV WISCONSIN, DEPT ASTRON, MADISON, WI 53706 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. SISSA, I-34013 TRIESTE, ITALY. IAC, E-38200 SANTA CRUZ PALMA, TENERIFE, SPAIN. CNR, I-00185 ROME, ITALY. UNIV FED RIO GRANDE SUL, IF, BR-91501970 PORTO ALEGRE, RS, BRAZIL. UNIV OREGON, DEPT PHYS, F-92195 MEUDON, FRANCE. ASTRON OBSERV PADOVA, I-35122 PADUA, ITALY. UNIV CALIF SANTA CRUZ, LICK OBSERV, SANTA CRUZ, CA 95064 USA. CIDA, MERIDA 5101A, VENEZUELA. ARIZONA STATE UNIV, DEPT PHYS & ASTRON, TEMPE, AZ 85287 USA. UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. LAEFE, E-28080 MADRID, SPAIN. INST ASTROPHYS, F-75014 PARIS, FRANCE. INST NACL ASTROFIS OPT & ELECTR, PUEBLA 72000, MEXICO. UNIV PADUA, DEPT ASTRON, I-35122 PADUA, ITALY. UNIV VIRGINIA, DEPT ASTRON, UNIV STN, CHARLOTTESVILLE, VA 22903 USA. UNIV PARIS 07, URA 173, OBSERV PARIS MEUDON, DAEC, F-92195 MEUDON, FRANCE. UNIV BASEL, INST ASTRON, CH-4102 BINNINGEN, SWITZERLAND. NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. UNIV LAVAL, DEPT PHYS, ST FOY, PQ G1K 7P4, CANADA. UNIV AUTONOMA MADRID, DEPT FIS TEOR, FAC CIENCIAS, E-28049 MADRID, SPAIN. MT STROMLO & SIDING SPRING OBSERV, WESTON, ACT 2611, AUSTRALIA. IUE OBSERV VILLAFRANCA CASTILLO, E-28080 MADRID, SPAIN. JOHNS HOPKINS UNIV, BLOOMBERG CTR PHYS & ASTRON, BALTIMORE, MD 21218 USA. UNIV N CAROLINA, DEPT PHYS & ASTRON, CHAPEL HILL, NC 27599 USA. OBSERV STRASBOURG, F-67000 STRASBOURG, FRANCE. OBSERV GENEVA, CH-1290 SAUVERNY, SWITZERLAND. UNIV TRIESTE, DEPT ASTRON, I-34131 TRIESTE, ITALY. OSSERV ASTRON TRIESTE, I-34131 TRIESTE, ITALY. NASA, GODDARD SPACE FLIGHT CTR, IUE OBSERV CSC, GREENBELT, MD 20771 USA. UNIV OSLO, INST THEORET ASTROPHYS, N-0315 OSLO, NORWAY. SW RES INST, BOULDER, CO 80302 USA. KAPTEYN INST, NL-9700 AV GRONINGEN, NETHERLANDS. UNIV FED SANTA MARIA, DEPT MATEMAT NEPAE, BR-97100 SANTA MARIA, RS, BRAZIL. CTIO, LA SERENA, CHILE. ETH ZENTRUM, INST ASTRON, CH-8092 ZURICH, SWITZERLAND. TARTU OBSERV, EE-2400 TORAVERE, TARTUMAA, ESTONIA. UNIV MICHIGAN, DEPT ASTRON, ANN ARBOR, MI 48109 USA. RP Leitherer, C (reprint author), SPACE TELESCOPE SCI INST, 3700 SAN MARTIN DR, BALTIMORE, MD 21218 USA. RI Peletier, Reynier/B-9633-2012; Cervino, Miguel/L-7024-2014; Dopita, Michael/P-5413-2014; Schmidt, Alex/G-1886-2012; Molla, Mercedes/I-3189-2015; Schmutz, Werner/B-4153-2014; Mas-Hesse, J. Miguel /K-6805-2014; OI Cervino, Miguel/0000-0001-8009-231X; Dopita, Michael/0000-0003-0922-4986; Schmidt, Alex/0000-0001-8609-4375; Molla, Mercedes/0000-0003-0817-581X; Schmutz, Werner/0000-0003-1159-5639; Mas-Hesse, J. Miguel /0000-0002-8823-9723; Vallenari, Antonella/0000-0003-0014-519X NR 172 TC 173 Z9 173 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD NOV PY 1996 VL 108 IS 729 BP 996 EP 1017 DI 10.1086/133825 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VT192 UT WOS:A1996VT19200007 ER PT J AU Heyman, IM AF Heyman, IM TI The Smithsonian Institute, 150 year anniversary, 1846-1996 SO SMITHSONIAN LA English DT Editorial Material RP Heyman, IM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD NOV PY 1996 VL 27 IS 8 BP 18 EP 18 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA VQ783 UT WOS:A1996VQ78300001 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI The Peenemunde wind tunnels: A memoir - Wegener,PP SO NATURE LA English DT Book Review RP Neufeld, MJ (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD OCT 31 PY 1996 VL 383 IS 6603 BP 779 EP 779 DI 10.1038/383779a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VQ144 UT WOS:A1996VQ14400045 ER PT J AU Gacia, E Littler, MM Littler, DS AF Gacia, E Littler, MM Littler, DS TI The relationships between morphology and photosynthetic parameters within the polymorphic genus Caulerpa SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Caulerpa; functional-morphology; photosynthesis; surface area vs biomass ratio (SA:B); surface area vs volume ratio (SA:V) ID FUNCTIONAL-FORM MODEL; EPILITHIC FORMS; LIGHT; ALGAE; CHLOROPHYTA; RESPIRATION; TEMPERATURE; IRRADIANCE; TESTS AB The functional form theory predicts that surface area vs. volume ratio (SA:V) and maximum productivity (P-max) decrease as morphological complexity of an algal thallus increases. The genus Caulerpa demonstrates a tremendous range of morphological forms as well as interspecific plasticity which make it ideal to study intrageneric relationships between photosynthesis and morphology. We used two approaches to assess functional-morphology relationships: 1) an extensive survey of P-max for 15 Caulerpa taxa in relation to SA:V from species and forms of the Caribbean and 2) an intensive study of photosynthetic attributes [P-max, photosynthetic efficiency (alpha), compensation irradiance (I-c), saturation irradiance (I-k)] and respiration (R) for 4 Caulerpa taxa from the Indian River Lagoon, Florida, focusing on SA:V and surface area vs. biomass (SA:B) ratios. These two sites represent areas of relatively low and high nutrient water respectively. SA:V ratios for Caribbean Caulerpa ranged from 0.5+/-0.10 to 11.7+/-3.53 cm(2) . cm(-3) and were highly correlated (r(2)=0.74, p=0.01) to net photosynthetic rates (values from 0.4 to 4.6 mg C . g ODW-1. h(-1)). However, for clumped forms, e.g., C. sertularioides var. brevipes (J. Ag.) Svedelius, from the Indian River Lagoon, P-max Values were lower than predicted possibly due to an auto-shading effect of thin-overlapping branches. In these forms, SA:B ratio was more highly correlated to photosynthetic attributes than SA:V ratio. Our data from the Caribbean, with a mean P-max of 2.23 mg C . g ODW-1. h(-1), suggest that the genus Caulerpa, in low nutrient systems, approaches the lower mid-range of net primary production of other algal forms. Conversely, Indian River Lagoon values are much higher, reaching a maximum of 17.2 mg C . g ODW-1. h(-1), possibly due to nutrient enriched waters of this system that enhance P-max. Photosynthetic efficiency ranged between 0.007 to 0.042 mg C g ODW-1. h(-1) per mu M m(-2). s(-2). s(-1) PAR. P-max was mantained at 2500 mu M m(-2). s(-1) and only one species, C. prolifera f.zosterifolia Borgesen,showed a photoinhibitory effect at 3000 mu M m(-2). s(-1). Our data indicate that photosynthetic attributes of Caulerpa from shallow water in the Indian River Lagoon are characteristic of sun-adapted plants, i.e., high saturation and compensation irradiances, low efficiencies for capturing low photon flux densities and high exposure resistance to elevated light irradiances. C1 NATL MUSEUM NAT HIST,SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. HARBOR BRANCH OCEANOG INST INC,DIV MARINE SCI,FT PIERCE,FL 34946. RP Gacia, E (reprint author), SMITHSONIAN MARINE STN,5612 OLD DIXIE HIGHWAY,FT PIERCE,FL 34946, USA. RI Gacia, Esperanca/J-9238-2012 OI Gacia, Esperanca/0000-0002-7687-7437 NR 35 TC 22 Z9 23 U1 1 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD OCT 25 PY 1996 VL 204 IS 1-2 BP 209 EP 224 DI 10.1016/0022-0981(96)02585-3 PG 16 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA VQ305 UT WOS:A1996VQ30500014 ER PT J AU Forman, P AF Forman, P TI Particle physics. One hundred years of discoveries. An annotated chronological bibliography - Exhela,VV SO SCIENCE LA English DT Book Review RP Forman, P (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD OCT 25 PY 1996 VL 274 IS 5287 BP 522 EP 523 DI 10.1126/science.274.5287.522 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VN919 UT WOS:A1996VN91900029 ER PT J AU Srygley, RB Oliveira, EG Dudley, R AF Srygley, RB Oliveira, EG Dudley, R TI Wind drift compensation, flyways, and conservation of diurnal, migrant Neotropical Lepidoptera SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article ID FULGENS URANIIDAE MOTHS; NATURAL FREE FLIGHT AB The identification and conservation of migration corridors requires that migrating organisms are goal-oriented and capable of adjusting for drifting off-course. Migrating birds are capable of wind drift compensation over water, but no insects have been demonstrated to possess such capabilities. Using vector analysis of individual airspeeds, track directions, ambient windspeeds and wind directions, we quantified within-individual variation in compensation for wind drift in two migrating butterfly and one moth species in natural free flight over a lake. The pierid Aphrissa statira and nymphalid Marpesia chiron butterflies were capable of wind drift compensation, whereas Urania fulgens (Uraniidae) moths were incapable of course correction. Changes in heading across the lake were not indicative of the use of a single landmark for orientation, and thus the use of two landmarks or the vector orientation of the surface beneath the insect were potential orientation cues. Among migrating Aphrissa statira, Marpesia chiron, Phoebis argante, and Urania fulgens, individual headings corrected at least partly for wind drift. For Aphrissa, short-distance compensation over water extended to a long-distance flyway across the isthmus of Panama that is suitable for conservation. C1 UNIV TEXAS, DEPT ZOOL, AUSTIN, TX 78712 USA. SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RP Srygley, RB (reprint author), DEPT ZOOL NJ15, SEATTLE, WA 98195 USA. NR 31 TC 24 Z9 26 U1 1 U2 4 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD OCT 22 PY 1996 VL 263 IS 1375 BP 1351 EP 1357 DI 10.1098/rspb.1996.0198 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA VQ622 UT WOS:A1996VQ62200013 ER PT J AU Lewenstein, M You, L AF Lewenstein, M You, L TI Quantum phase diffusion of a Bose-Einstein condensate SO PHYSICAL REVIEW LETTERS LA English DT Article ID NONLINEAR SCHRODINGER-EQUATION; TRAPPED NEUTRAL ATOMS; GAS AB We discuss the quantum properties of the Bose-Einstein condensate of a dilute gas of atoms in a trap. We show that the phase of the condensate undergoes quantum diffusion which can be detected in far off-resonant light scattering experiments. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. RP Lewenstein, M (reprint author), CTR ETUD SACLAY,CEA,DSM,DRECAM,SPAM,F-91191 GIF SUR YVETTE,FRANCE. RI Lewenstein, Maciej/I-1337-2014 OI Lewenstein, Maciej/0000-0002-0210-7800 NR 34 TC 268 Z9 272 U1 0 U2 9 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 21 PY 1996 VL 77 IS 17 BP 3489 EP 3493 DI 10.1103/PhysRevLett.77.3489 PG 5 WC Physics, Multidisciplinary SC Physics GA VM890 UT WOS:A1996VM89000001 ER PT J AU Mohr, JJ Geller, MJ Fabricant, DG Wegner, G Thorstensen, J Richstone, DO AF Mohr, JJ Geller, MJ Fabricant, DG Wegner, G Thorstensen, J Richstone, DO TI An optical X-ray study of Abell 576, a galaxy cluster with a cold core SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies, clusters, individual (A576); galaxies, distances and redshifts; galaxies, luminosity function, mass function; galaxies, photometry; X-rays, galaxies ID RICH CLUSTERS; LUMINOSITY FUNCTION; COMA CLUSTER; VELOCITY DISPERSIONS; DISTANT CLUSTERS; REDSHIFT SURVEY; EVOLUTION; SPECTROSCOPY; MASS; GAS AB We analyze the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2 h(-1) Mpc x 2 h(-1) Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R(23.5) < 17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2 h(-1) Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a nonemission galaxy population and an intracluster medium which is significantly cooler (sigma(core) = 387(-105)(+250) km s(-1) and T-x = 1.6(-0.3)(+0.4) keV at 90% confidence) than the global populations (sigma = 977(-96)(+124) km s(-1) for the nonemission population and T-x > 4 keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 mag. contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r similar to 1 h(-1) Mpc is T-x similar to 8 keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is similar to 3 h(-3/2)% and the baryon fraction is similar to 4%. C1 UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. DARTMOUTH COLL,DEPT PHYS & ASTRON,HANOVER,NH 03755. RP Mohr, JJ (reprint author), UNIV MICHIGAN,DEPT PHYS,500 E UNIV,ANN ARBOR,MI 48109, USA. NR 106 TC 64 Z9 64 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1996 VL 470 IS 2 BP 724 EP 742 DI 10.1086/177903 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VM998 UT WOS:A1996VM99800006 ER PT J AU Momose, M Ohashi, N Kawabe, R Hayashi, M Nakano, T AF Momose, M Ohashi, N Kawabe, R Hayashi, M Nakano, T TI The dispersing cloud core around T Tauri SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM, jets and outflows; ISM, molecules; stars, individual (T Tauri); stars, pre-main-sequence ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MOLECULAR CLOUD; GAS DISK; INFRARED-SPECTRA; STAR-FORMATION; DENSE CORES; DARK CLOUD; GG TAURI; HL TAURI AB We have made (CO)-C-13 (J = 1-0) observations of T Tauri with the Nobeyama Millimeter Array (NMA) and with the Nobeyama 45 m telescope. The (CO)-C-13 (J = 1-0) emission detected with the NMA shows three different features: (1) a pair of ringlike features surrounding T Tauri with a radius of 30 '' (corresponding to 4200 AU at the distance of 140 pc to T Tauri) at the velocities blueshifted and redshifted by less than 1 km s(-1) from the systemic velocity, (2) a blueshifted compact feature 3 '' east of T Tauri, and (3) another compact feature 7 '' southwest of T Tauri at velocities redshifted by more than 1 km s(-1). On the other hand, the (CO)-C-13 maps obtained with the 45 m telescope show a smoothly extended feature near the systemic velocity, which is missed in the NMA observations, as well as the above-mentioned three features. The total masses of gas detected with the NMA and the 45 m telescope are estimated to be (0.054-0.23) M(.) and (0.31-1.3) M(.), respectively. The difference in the estimated mass between the two observations is mainly due to resolving out of the smoothly extended feature in the NMA observations. The (CO)-C-13 rings are interpreted as biconical outflowing shells in a nearly pole-on configuration. The high-velocity stellar wind ejected from T Tauri is estimated to be energetic enough to drive these outflowing shells. We have analyzed the three-dimensional structure of the shells by correcting for the projection effect on the plane of the sky, and we have found that the spatial extent of the shells is nearly equal to or slightly smaller than the typical size of the molecular cloud cores in the Taurus Molecular Cloud. This fact indicates that the outflowing shells are part of the parent cloud core that still remains around T Tauri, which is now dispersing under the influence of the stellar wind. Such an environment around T Tauri is quite different from those around typical T Tauri stars, which are associated only with compact gaseous components. These results suggest strongly that T Tauri is one of the objects in the transitional phase from the protostar stage, in which a central star is deeply embedded in an infalling envelope, to the T Tauri stage, in which a central star is surrounded by a compact circumstellar disk instead of a spatially extended envelope. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NATL ASTRON OBSERV, SUBARU PROJECT OFF, MITAKA, TOKYO 181, JAPAN. RP Momose, M (reprint author), GRAD UNIV ADV STUDIES, NOBEYAMA RADIO OBSERV, DEPT ASTON SCI, MINAMISA KU, MINAMIMAKI, NAGANO 38413, JAPAN. NR 66 TC 35 Z9 35 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1996 VL 470 IS 2 BP 1001 EP + DI 10.1086/177925 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VM998 UT WOS:A1996VM99800028 ER PT J AU Strelnitski, VS Ponomarev, VO Smith, HA AF Strelnitski, VS Ponomarev, VO Smith, HA TI Hydrogen masers .1. Theory and prospects SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; H II regions; masers; stars, emission-line, Be; stars, individual (MWC 349) ID RECOMBINATION LINE MASER; PHYSICAL-PROPERTIES; H2O MASERS; MWC-349; RADIO; EMISSION; INTENSITIES; IONS; M82 AB The discovery of the first high-gain hydrogen recombination line (HRL) maser in the millimeter/submillimeter spectrum of the emission-line star MWC 349A requires an expansion of current paradigms about HRLs. In this paper we reexamine the problem of non-LTE populations in recombining hydrogen and specify the conditions necessary for high-gain masing and lasing in HRLs. To do so, we use the extensive new results on hydrogen level populations produced by Storey & Hummer and our calculations for the net (that is, line plus continuum) absorption coefficient for HRLs. We present results for the alpha- and beta-lines whose principal quantum numbers n are between five and 100, for gas whose electron number density 3 less than or equal to log N-e(cm(-3))less than or equal to 11, at two electron temperatures, T-e = 5000 and 10,000 K. We show that the unsaturated maser gain in an HRL is a sharp function of N-e, and thus to achieve high-gain masing, each line requires a sufficiently extended region over which the density is rather closely specified. Saturation of masing recombination lines is a critical consideration. We derive a simple equation for estimating the degree of saturation from the observed flux density and the interferometric and/or model information about the amplification path length, avoiding the vague issue of the solid angle of masing. We also present a qualitative way to approach the effects of saturation on adjacent emission lines, although the detailed modeling is highly case-specific. We draw attention to another non-LTE phenomenon active in hydrogen: the overcooling of populations. This occurs for HRLs with n greater than or similar to 20, in gas where N-e less than or similar to 10(5) cm(-3). Observationally, the HRL overcooling might manifest itself as an anomalously weak emission recombination line, or as a ''dasar,'' that is, an anomalously strong absorption line. In the simplest case of a homogeneous H rr region, the absorption can be observed on the proper free-free continuum of the region, if some conditions for the line or/and continuum optical depths are satisfied. We briefly discuss the prospects of detecting hydrogen masers, lasers, and dasars in several classes of Galactic and extragalactic objects, including compact H II regions, Be or Wolf-Rayet stars, starburst galaxies, and active galactic nuclei. C1 NEW MEXICO INST MIN & TECHNOL,SOCORRO,NM 87801. PN LEBEDEV PHYS INST,MOSCOW 117924,RUSSIA. RP Strelnitski, VS (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560, USA. NR 46 TC 32 Z9 32 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1996 VL 470 IS 2 BP 1118 EP 1133 DI 10.1086/177936 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VM998 UT WOS:A1996VM99800039 ER PT J AU Strelnitski, VS Smith, HA Ponomarev, VO AF Strelnitski, VS Smith, HA Ponomarev, VO TI Hydrogen masers .2. MWC 349A SO ASTROPHYSICAL JOURNAL LA English DT Article DE masers; radio lines, stars; stars, individual (MWC 349); stars, mass loss ID RECOMBINATION LINE MASER; MWC-349; EMISSION AB The conditions of masing and lasing in the hydrogen recombination lines (HRLs) in the disk and outflow of MWC 349A are studied. Comparison of the observed integrated fluxes of virtually all the alpha-lines measured in this source-from H2 alpha through H92 alpha-with a simple model of spontaneous emission shows that observable HRL masing is limited to the interval of the principal quantum numbers n approximate to 10-40. We use our analytical and numerical results for the conditions of optimum masing and the morphological parameters of the photoevaporated circumstellar disk modeled by Hollenbach and coworkers to obtain analytical approximations and quantitative estimates for the expected unsaturated maser gain and the degree of saturation in HRL masers in the disk of MWC 349A. It is shown that the unsaturated gains of the infrared HRL lasers should be very high, but in fact all of these lasers are strongly saturated. Because of saturation, their relative intensity with respect to the spontaneous emission should drop steeply toward smaller n's, which explains why optical and near-infrared HRL lasers are not seen in MWC 349A. This result is quite general and makes the prognosis for observable high-frequency HRL lasers in other sources pessimistic as well. An exception might arise because of special geometry, if lasing were confined to a very small solid angle. We show that weak masing from the outflow of MWC 349A is only possible in low-n alpha-lines (n less than or similar to 20-30), and then only if the outflow begins much closer to the central star than the Hollenbach model predicts (approximate to 3 x 10(15) cm). We therefore conclude that maser emission from the disk, rather than from the outflow, is responsible for the observed weak amplification of the ''pedestal'' spectral components in the alpha-lines with n less than or similar to 40. The fluxes in the lower frequency alpha-lines are well explained by spontaneous emission from the outflow, with proper corrections for free-free absorption. We review the current state and prospects of observations of masing and lasing hydrogen beta-lines in MWC 349A. We argue in favor of ''close in n,'' rather than ''close in frequency'' alpha/beta pairs for intensity analysis, when maser amplification is present. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. PN LEBEDEV PHYS INST,MOSCOW 117924,RUSSIA. RP Strelnitski, VS (reprint author), NEW MEXICO INST MIN & TECHNOL,SOCORRO,NM 87801, USA. NR 30 TC 16 Z9 16 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1996 VL 470 IS 2 BP 1134 EP 1143 DI 10.1086/177937 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VM998 UT WOS:A1996VM99800040 ER PT J AU Aschwanden, MJ Kosugi, T Hudson, HS Wills, MJ Schwartz, RA AF Aschwanden, MJ Kosugi, T Hudson, HS Wills, MJ Schwartz, RA TI The scaling law between electron time-of-flight distances and loop lengths in solar flares SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; radiation mechanisms, nonthermal; Sun, corona; Sun, flares; Sun, X-rays, gamma rays ID HARD X-RAY; 1991 NOVEMBER 15; WHITE-LIGHT FLARES; YOHKOH OBSERVATIONS; A MISSION; BURSTS; TARGET; SPECTROMETER; RECONNECTION; PARTICLES AB From the complete data set of solar flares simultaneously observed with the Burst and Transient Source Experiment (BATSE) on board the Compton Gamma Ray Observatory (CGRO) in the high-time resolution mode (64 ms) and the Hard X-ray Telescope (HXT) on board Yohkoh, we were able to determine the electron time-of-flight (TOF) distance l' and the flare loop geometry in 42 events. The electron TOF distances were determined from time delays (of approximate to 10-100 ms) of hard X-ray (HXR) pulses (measured in 16 channel spectra over approximate to 20-200 keV), produced by the velocity difference of the HXR-producing electrons. The hare loops were mostly identified from double footpoint sources in greater than or similar to 30 keV HXT images, with radii in the range r = 3000-25,000 km. We find a scaling law between the electron TOF distance l' and the flare loop half-length s = r(pi/2), having a mean ratio (and standard deviation) of l'/s = 1.4 +/- 0.3. In five flares, we observe coronal greater than or similar to 30 keV HXR sources of the Masuda type in the cusp region above the flare loop and find that their heights are consistent with the electron TOF distance to the footpoints. These results provide strong evidence that particle acceleration in solar flares occurs in the cusp region above the flare loop and that the coronal HXR sources discovered by Masuda et al. are a signature of the acceleration site, probably controlled by a magnetic reconnection process. C1 NATL ASTRON OBSERV, MITAKA, TOKYO 181, JAPAN. UNIV HAWAII, INST ASTRON, HONOLULU, HI 96822 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NASA, GODDARD SPACE FLIGHT CTR, HUGES STX, GREENBELT, MD 20771 USA. RP Aschwanden, MJ (reprint author), UNIV MARYLAND, DEPT ASTRON, COLLEGE PK, MD 20742 USA. NR 63 TC 83 Z9 83 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1996 VL 470 IS 2 BP 1198 EP 1217 DI 10.1086/177943 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VM998 UT WOS:A1996VM99800046 ER PT J AU Pildis, RA McGaugh, SS AF Pildis, RA McGaugh, SS TI Could a local group X-ray halo affect the X-ray and microwave backgrounds? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; galaxies, clusters, general; Local Group ID GALAXIES; SPECTRUM; SHADOW AB Suto et al. have suggested that an X-ray halo in the Local Group might explain both the observed low-energy excess in the X-ray background and the quadrupole anisotropy in the cosmic microwave background. Recent observations of poor groups of galaxies by the ROSAT PSPC set reasonable limits on how extensive and dense such a halo could be. The poor groups most similar to the Local Group do not have a detectable halo, and the upper limits of these observations suggest that any Local Group halo would be nearly 2 orders of magnitude too tenuous to produce the effects that Suto et al. discuss. In particular, the Sunyaev-Zeldovich effect cannot contribute significantly to the quadrupole anisotropy measured by COBE. C1 CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,WASHINGTON,DC 20015. RP Pildis, RA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS 83,CAMBRIDGE,MA 02140, USA. NR 18 TC 13 Z9 13 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1996 VL 470 IS 2 BP L77 EP L79 DI 10.1086/310304 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VM999 UT WOS:A1996VM99900001 ER PT J AU Wilner, DJ Ho, PTP Rodriguez, LF AF Wilner, DJ Ho, PTP Rodriguez, LF TI Subarcsecond VLA observations of HL Tauri: Imaging the circumstellar disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; methods, observational; radio continuum, stars; stars, formation; stars, individual (HL Tauri) ID YOUNG STELLAR OBJECTS; R-MONOCEROTIS; STARS; GAS; OUTFLOWS; JETS AB We report high-resolution observations of HL Tau at 6 cm, 3.6 cm, and 7 mm using the VLA in B configuration. The new centimeter wavelength data are in accord with previous observations-taking into account resolution and sensitivity-and provide no evidence for time variability. At 7 mm, we have used a ''fast-switching'' calibration technique to partially overcome the problem of atmospheric phase fluctuations and achieve subarcsecond angular resolution. The 7 mm image, which is dominated by dust emission, shows a flattened structure with Gaussian deconvolved size (0''.75 +/- 0''.1) x (0''.35 +/- 0''.1) [(105 +/- 14) x (50 +/- 14) AU] and major axis P.A. 125 degrees +/- 10 degrees. This orientation is similar to that found at shorter wavelengths and is approximately orthogonal to the optical jet axis, consistent with a dusty accretion disk surrounding the star. C1 NATL AUTONOMOUS UNIV MEXICO,INST ASTRON,MEXICO CITY 04510,DF,MEXICO. RP Wilner, DJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 39 TC 47 Z9 47 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1996 VL 470 IS 2 BP L117 EP L121 DI 10.1086/310307 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VM999 UT WOS:A1996VM99900011 ER PT J AU Riley, SM AF Riley, SM TI Errands - Guest,J SO LIBRARY JOURNAL LA English DT Book Review RP Riley, SM (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 1996 VL 121 IS 17 BP 90 EP 90 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VN323 UT WOS:A1996VN32300221 ER PT J AU Shahbaz, T Smale, AP Naylor, T Charles, PA vanParadijs, J Hassall, BJM Callanan, P AF Shahbaz, T Smale, AP Naylor, T Charles, PA vanParadijs, J Hassall, BJM Callanan, P TI An atlas of optical continuum and line emission from low-mass X-ray binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE accretion, accretion discs; atlases; binaries, close; stars, neutron; X-rays, stars ID CENTAURUS X-4; CYGNUS X-2; ACCRETION DISKS; ORBITAL PERIOD; SCORPIUS X-1; BLACK-HOLE; AQUILA X-1; 4U 2129+47; OPTIMAL EXTRACTION; LIGHT-CURVE AB We have obtained broad-band optical spectra of a sample of 15 low-mass X-ray binaries (LMXBs) in the range 4000-9000 Angstrom and fitted them with combinations of standard accretion disc models plus secondary star templates. For the sample of LMXBs in which we determined the power-law indices of the accretion disc flux distribution, we can explain the steepness of the slopes in terms of an optically thick accretion disc and X-ray heating of the outer parts of the disc. We present for the first time optical spectra of X 1705 - 250, XB 1905 + 00 and XB 1916 - 053. Optical line emission was detected in most of the sample. The Balmer lines H alpha and H beta were generally the strongest lines with mean equivalent widths of 3.7 and 1.9 Angstrom, respectively. The He II lambda 4686 and the Bowen C III/N III blend at lambda 4640 were also observed, with equivalent widths of 3.0 and 4.1 Angstrom, respectively, The Paschen lines were: also present in Cen X - 4, GS 2000 + 25, and for the first time detected in Aql X - 1. The only systems in which stellar features were detected were those in which the companions were evolved e.g. GX 1 + 4, Cyg X - 2 and the source in which the mass accretion rate is low i.e. Cen X - 4. C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. UNIV KEELE,DEPT PHYS,KEELE ST5 5BG,STAFFS,ENGLAND. UNIV AMSTERDAM,ASTRON INST ANTON PANNEKOEK,NIKHEF H,NL-1098 SJ AMSTERDAM,NETHERLANDS. UNIV CENT LANCASHIRE,DEPT PHYS & ASTRON,PRESTON PR1 2HE,LANCS,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Shahbaz, T (reprint author), UNIV OXFORD,DEPT ASTROPHYS,NUCL PHYS BLDG,OXFORD OX1 3RH,ENGLAND. RI Naylor, Tim /A-9465-2015 NR 103 TC 36 Z9 36 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 15 PY 1996 VL 282 IS 4 BP 1437 EP 1453 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VN513 UT WOS:A1996VN51300034 ER PT J AU Silbermann, NA Harding, P Madore, BF Kennicutt, RC Saha, A Stetson, PB Freedman, WL Mould, JR Graham, JA Hill, RJ Turner, A Bresolin, F Ferrarese, L Ford, H Hoessel, JG Han, MS Huchra, J Hughes, SMG Illingworth, GD Phelps, R Sakai, S AF Silbermann, NA Harding, P Madore, BF Kennicutt, RC Saha, A Stetson, PB Freedman, WL Mould, JR Graham, JA Hill, RJ Turner, A Bresolin, F Ferrarese, L Ford, H Hoessel, JG Han, MS Huchra, J Hughes, SMG Illingworth, GD Phelps, R Sakai, S TI The Hubble Space Telescope Key Project on the Extragalactic Distance Scale .6. The Cepheids in NGC 925 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; distance scale; galaxies, individual (NGC 925) ID LINE-WIDTH RELATIONS; STELLAR PHOTOMETRY; SPIRAL GALAXIES; CCD PHOTOMETRY; NGC-1023 GROUP; II SUPERNOVAE; NEARBY GROUPS; FIELD; EXTINCTION; REDSHIFT AB We report the detection of Cepheid variable stars in the barred spiral galaxy NGC 925, using the Hubble Space Telescope (HST) Wide-Field and Planetary Camera 2 (WFPC2). Twelve V (F555W) and four I (F814W) epochs of cosmic-ray split observations were obtained. Eighty Cepheids were discovered, with periods from 6 to similar to 80 days. Light curves of the Cepheids are presented, and their corresponding period-luminosity diagrams are discussed. Using a distance modulus for the Large Magellanic Cloud Cepheids of 18.50 mag and an extinction of E(V-I)=0.13 mag, the measured distance modulus to NGC 925 is 29.84+/-0.16 mag, corresponding to a distance of 9.29+/-0.69 Mpc. A mean reddening of E(V-I)=0.17 mag is found for the Cepheids in this region of NGC 925. C1 UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. CALTECH,NASA,EXTRAGALACT DATABASE,INFRARED PROC & ANAL CTR,PASADENA,CA 91125. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,INST ADV STUDIES,WESTON,ACT 2611,AUSTRALIA. CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,WASHINGTON,DC 20015. NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. JOHNS HOPKINS UNIV,BALTIMORE,MD 21218. UNIV WISCONSIN,MADISON,WI 53706. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0EZ,ENGLAND. UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064. RP Silbermann, NA (reprint author), CALTECH,JET PROP LAB,INFRARED PROC & ANAL CTR,MS 100-22,PASADENA,CA 91125, USA. NR 46 TC 91 Z9 91 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1996 VL 470 IS 1 BP 1 EP & DI 10.1086/177845 PN 1 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VL723 UT WOS:A1996VL72300001 ER PT J AU Shectman, SA Landy, SD Oemler, A Tucker, DL Lin, HA Kirshner, RP Schechter, PL AF Shectman, SA Landy, SD Oemler, A Tucker, DL Lin, HA Kirshner, RP Schechter, PL TI The Las Campanas Redshift Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, observations; galaxies, clusters, general; galaxies, distances and redshifts; surveys ID GUIDE STAR CATALOG; COLD DARK MATTER; LUMINOSITY FUNCTION; GALAXY REDSHIFTS; POWER SPECTRUM; FIELD GALAXIES; UNIVERSE; STATISTICS; DENSITY; BOOTES AB The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg(2) in six strips, each 1.degrees 5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s(-1). Essential features of the galaxy selection and redshift measurement methods are described and tabulated here. These details are important for subsequent analysis of the LCRS data, Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s(-1), sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. The LCRS redshift catalog will be made available to interested investigators at an internet web site and in archival form as an AAS CD-ROM. C1 YALE UNIV, DEPT ASTRON, NEW HAVEN, CT 06520 USA. ASTROPHYS INST POTSDAM, D-14482 POTSDAM, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. RP CARNEGIE INST WASHINGTON OBSERV, 813 SANTA BARBARA ST, PASADENA, CA 91101 USA. NR 59 TC 398 Z9 400 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1996 VL 470 IS 1 BP 172 EP 188 DI 10.1086/177858 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VL723 UT WOS:A1996VL72300014 ER PT J AU Crenshaw, DM RodriguezPascual, PM Penton, SV Edelson, RA Alloin, D Ayres, TR Clavel, J Horne, K Johnson, WN Kaspi, S Korista, KT Kriss, GA Krolik, JH Malkan, MA Maoz, D Netzer, H OBrien, PT Peterson, BM Reichert, GA Shull, JM Ulrich, MH Wamsteker, W Warwick, RS Yaqoob, T Balonek, TJ Barr, P Bromage, GE Carini, M Carone, TE Cheng, FZ Chuvaev, KK Dietrich, M Doroshenko, VT DultzinHacyan, D Filippenko, AV Gaskell, CM Glass, IS Goad, MR Hutchings, J Kazanas, D Kollatschny, W Koratkar, AP Laor, A Leighly, K Lyutyi, VM MacAlpine, GM Malkov, YF Martin, PG McCollum, B Merkulova, NI Metik, L Metlov, VG Miller, HR Morris, SL Oknyanskij, VL Penfold, J Perez, E Perola, GC Pike, G Pogge, RW Pronik, I Pronik, VI Ptak, RL RecondoGonzalez, MC RodriguezEspinoza, JM Rokaki, EL Roland, J Sadun, AC Salamanca, I SantosLleo, M Sergeev, SG Smith, SM Snijders, MAJ Sparke, LS Stirpe, GM Stoner, RE Sun, WH vanGroningen, E Wagner, RM Wagner, S Wanders, I Welsh, WF Weymann, RJ Wilkes, BJ Zheng, W AF Crenshaw, DM RodriguezPascual, PM Penton, SV Edelson, RA Alloin, D Ayres, TR Clavel, J Horne, K Johnson, WN Kaspi, S Korista, KT Kriss, GA Krolik, JH Malkan, MA Maoz, D Netzer, H OBrien, PT Peterson, BM Reichert, GA Shull, JM Ulrich, MH Wamsteker, W Warwick, RS Yaqoob, T Balonek, TJ Barr, P Bromage, GE Carini, M Carone, TE Cheng, FZ Chuvaev, KK Dietrich, M Doroshenko, VT DultzinHacyan, D Filippenko, AV Gaskell, CM Glass, IS Goad, MR Hutchings, J Kazanas, D Kollatschny, W Koratkar, AP Laor, A Leighly, K Lyutyi, VM MacAlpine, GM Malkov, YF Martin, PG McCollum, B Merkulova, NI Metik, L Metlov, VG Miller, HR Morris, SL Oknyanskij, VL Penfold, J Perez, E Perola, GC Pike, G Pogge, RW Pronik, I Pronik, VI Ptak, RL RecondoGonzalez, MC RodriguezEspinoza, JM Rokaki, EL Roland, J Sadun, AC Salamanca, I SantosLleo, M Sergeev, SG Smith, SM Snijders, MAJ Sparke, LS Stirpe, GM Stoner, RE Sun, WH vanGroningen, E Wagner, RM Wagner, S Wanders, I Welsh, WF Weymann, RJ Wilkes, BJ Zheng, W TI Multiwavelength observations of short-timescale variability in NGC 4151 .1. Ultraviolet observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, individual (NGC 4151); galaxies, Seyfert; ultraviolet, galaxies ID BROAD-LINE REGION; ACTIVE GALACTIC NUCLEI; X-RAY; DETAILED OBSERVATIONS; SEYFERT-GALAXIES; OPTICAL WAVELENGTHS; NGC-4151; IUE; NGC-5548; SIZE AB We present the results of an intensive ultraviolet monitoring campaign on the Seyfert 1 galaxy NGC 4151, as part of an effort to study its short-timescale variability over a broad range in wavelength. The nucleus of NGC 4151 was observed continuously with the International Ultraviolet Explorer for 9.3 days, yielding a pair of LWP and SWP spectra every similar to 70 minutes, and during 4 hr periods for 4 days prior to and 5 days after the continuous-monitoring period. The sampling frequency of the observations is an order of magnitude higher than that of any previous UV monitoring campaign on a Seyfert galaxy. The continuum fluxes in bands from 1275 to 2688 Angstrom went through four significant and well-defined ''events'' of duration 2-3 days during the continuous-monitoring period. We find that the amplitudes of the continuum variations decrease with increasing wavelength, which extends a general trend for this and other Seyfert galaxies to smaller timescales (i.e., a few days). The continuum variations in all the UV bands are simultaneous to within an accuracy of similar to 0.15 days, providing a strict constraint on continuum models. The emission-line light curves show only one major event during the continuous monitoring (a slow rise followed by a shallow dip) and do not correlate well with continuum light curves over the short duration of the campaign, because the timescale for continuum variations is apparently smaller than the response times of the emission lines. C1 EUROPEAN SPACE AGCY, IUE OBSERV, E-28080 MADRID, SPAIN. UNIV COLORADO, CTR ASTROPHYS & SPACE ASTRON, BOULDER, CO 80309 USA. UNIV IOWA, DEPT PHYS & ASTRON, IOWA CITY, IA 52242 USA. OBSERV PARIS, CNRS, URA 173, F-92195 MEUDON, FRANCE. ESTEC, EUROPEAN SPACE AGCY, DIV ASTROPHYS, ISO OBSERV, NL-2200 AG NOORDWIJK, NETHERLANDS. UNIV ST ANDREWS, SCH PHYS & ASTRON, ST ANDREWS KY16 9SS, FIFE, SCOTLAND. USN, RES LAB, WASHINGTON, DC 20375 USA. TEL AVIV UNIV, RAYMOND & BEVERLY SACKLER FAC EXACT SCI, SCH PHYS & ASTRON, IL-69978 TEL AVIV, ISRAEL. TEL AVIV UNIV, RAYMOND & BEVERLY SACKLER FAC EXACT SCI, WISE OBSERV, IL-69978 TEL AVIV, ISRAEL. UNIV KENTUCKY, DEPT PHYS & ASTRON, LEXINGTON, KY 40506 USA. JOHNS HOPKINS UNIV, DEPT PHYS & ASTRON, BLOOMBERG CTR, BALTIMORE, MD 21218 USA. UNIV CALIF LOS ANGELES, DEPT ASTRON, LOS ANGELES, CA 90024 USA. UNIV OXFORD, DEPT ASTRON, OXFORD OX1 3RH, ENGLAND. OHIO STATE UNIV, DEPT ASTRON, COLUMBUS, OH 43210 USA. NASA, GODDARD SPACE FLIGHT CTR, UNIV SPACE RES ASSOC, GREENBELT, MD 20771 USA. UNIV COLORADO, JOINT INST LAB ASTROPHYS, BOULDER, CO 80309 USA. UNIV COLORADO, NATL INST STAND & TECHNOL, BOULDER, CO 80309 USA. European So Observ, D-85748 Garching, GERMANY. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, ENGLAND. NASA, Goddard Space Flight Ctr, Lab High Energy Astrophys, Greenbelt, MD 20771 USA. Colgate Univ, Dept Phys & Astron, Hamilton, NY 13346 USA. Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, ENGLAND. Western Kentucky Univ, Dept Phys & Astron, Ctr Automated Space Studies, Bowling Green, KY 42101 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, PEOPLES R CHINA. Landessternwarte Konigstuhl, D-69117 Heidelberg, GERMANY. Sternberg State Astron Inst, UA-334413 Crimea, UKRAINE. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, MEXICO. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Nebraska, Dept Phys & Astron, Lincoln, NE 68588 USA. S African Astron Observ, ZA-7935 Observ, SOUTH AFRICA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Dominion Astrophys Observ, Victoria, BC V8X 4M6, CANADA. Univ Sternwarte Gottingen, D-37083 Gottingen, GERMANY. CALTECH, Dept Astron, Pasadena, CA 91125 USA. RIKEN, Cosm Radiat Lab, Wako, Saitama 35101, JAPAN. Univ Moscow, Sternberg Astron Inst, Moscow 119899, RUSSIA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Crimean Astrophys Observ, UA-334413 Crimea, UKRAINE. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, CANADA. NASA, Goddard Space Flight Ctr, Comp Sci Corp, Greenbelt, MD 20771 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. Astron Observ, S-75120 Uppsala, SWEDEN. Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, CANADA. Mt Royal Coll, Dept Math Phys & Engn, Calgary, AB T3E 6K6, CANADA. Inst Astrofis Andalucia, E-18080 Granada, SPAIN. Univ Rome, Inst Astron, I-00161 Rome, ITALY. Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA. Inst Astrofis Canarias, E-38200 La Laguna, Tenerife, SPAIN. Univ Edinburgh, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, SCOTLAND. Inst Astrophys, F-75014 Paris, FRANCE. Agnes Scott Coll, Dept Phys & Astron, Decatur, GA 30030 USA. Agnes Scott Coll, Bradley Observ, Decatur, GA 30030 USA. Inst Radio Astron Millimetr, F-38046 St Martin Dheres, FRANCE. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Osservatorio Astron Bologna, I-40126 Bologna, ITALY. Natl Cent Univ, Inst Astron, Chungli 32054, TAIWAN. Lowell Observ, Flagstaff, AZ 86001 USA. Keele Univ, Dept Phys, Keele ST5 5BG, Staffs, ENGLAND. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Crenshaw, DM (reprint author), NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, COMP SCI CORP, CODE 681, GREENBELT, MD 20771 USA. RI Morris, Simon/G-7981-2011; Oknyanskij, Victor/I-9267-2012; Johnson, Neil/G-3309-2014; Recondo, Carmen/B-1215-2012; Stirpe, Giovanna/O-9393-2015; OI Perez, Enrique/0000-0001-9737-4559; Morris, Simon/0000-0003-4866-110X; Recondo, Carmen/0000-0001-9813-6798; Stirpe, Giovanna/0000-0002-3702-8731; Gaskell, C/0000-0003-4888-2009; Wilkes, Belinda/0000-0003-1809-2364 NR 53 TC 66 Z9 66 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1996 VL 470 IS 1 BP 322 EP 335 DI 10.1086/177869 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VL723 UT WOS:A1996VL72300025 ER PT J AU Edelson, RA Alexander, T Crenshaw, DM Kaspi, S Malkan, MA Peterson, BM Warwick, RS Clavel, J Filippenko, AV Horne, K Korista, KT Kriss, GA Krolik, JH Maoz, D Nandra, K OBrien, PT Penton, SV Yaqoob, T Albrecht, P Alloin, D Ayres, TR Balonek, TJ Barr, P Barth, AJ Bertram, R Bromage, GE Carini, M Carone, TE Cheng, FZ Chuvaev, KK Dietrich, M DultzinHacyan, D Gaskell, CM Glass, IS Goad, MR Hemar, S Ho, LC Huchra, JP Hutchings, J Johnson, WN Kazanas, D Kollatschny, W Koratkar, AP Kovo, O Laor, A MacAlpine, GM Magdziarz, P Martin, PG Matheson, T McCollum, B Miller, HR Morris, SL Oknyanskij, VL Penfold, J Perez, E Perola, GC Pike, G Pogge, RW Ptak, RL Qian, BC RecondoGonzalez, MC Reichert, GA RodriguezEspinoza, JM RodriguezPascual, PM Rokaki, EL Roland, J Sadun, AC Salamanca, I SantosLleo, M Shields, JC Shull, JM Smith, DA Smith, SM Snijders, MAJ Stirpe, GM Stoner, RE Sun, WH Ulrich, MH vanGroningen, E Wagner, RM Wagner, S Wanders, I Welsh, WF Weymann, RJ Wilkes, BJ Wu, H Wurster, J Xue, SJ Zdziarski, AA Zheng, W Zou, ZL AF Edelson, RA Alexander, T Crenshaw, DM Kaspi, S Malkan, MA Peterson, BM Warwick, RS Clavel, J Filippenko, AV Horne, K Korista, KT Kriss, GA Krolik, JH Maoz, D Nandra, K OBrien, PT Penton, SV Yaqoob, T Albrecht, P Alloin, D Ayres, TR Balonek, TJ Barr, P Barth, AJ Bertram, R Bromage, GE Carini, M Carone, TE Cheng, FZ Chuvaev, KK Dietrich, M DultzinHacyan, D Gaskell, CM Glass, IS Goad, MR Hemar, S Ho, LC Huchra, JP Hutchings, J Johnson, WN Kazanas, D Kollatschny, W Koratkar, AP Kovo, O Laor, A MacAlpine, GM Magdziarz, P Martin, PG Matheson, T McCollum, B Miller, HR Morris, SL Oknyanskij, VL Penfold, J Perez, E Perola, GC Pike, G Pogge, RW Ptak, RL Qian, BC RecondoGonzalez, MC Reichert, GA RodriguezEspinoza, JM RodriguezPascual, PM Rokaki, EL Roland, J Sadun, AC Salamanca, I SantosLleo, M Shields, JC Shull, JM Smith, DA Smith, SM Snijders, MAJ Stirpe, GM Stoner, RE Sun, WH Ulrich, MH vanGroningen, E Wagner, RM Wagner, S Wanders, I Welsh, WF Weymann, RJ Wilkes, BJ Wu, H Wurster, J Xue, SJ Zdziarski, AA Zheng, W Zou, ZL TI Multiwavelength observations of short-timescale variability in NGC 4151 .4. Analysis of multiwavelength continuum variability SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, individual (NGC 4151); galaxies, Seyfert; ultraviolet, galaxies; X-rays, galaxies ID ACTIVE GALACTIC NUCLEI; OBJECT PKS 2155-304; BROAD-LINE REGION; X-RAY-EMISSION; CFA SEYFERT-GALAXIES; ULTRAVIOLET VARIABILITY; ACCRETION DISKS; COMPTON REFLECTION; BAND PROPERTIES; UV CONTINUUM AB This paper combines data from the three preceding papers in order to analyze the multi-wave-band variability and spectral energy distribution of the Seyfert 1 galaxy NGC 4151 during the 1993 December monitoring campaign. The source, which was near its peak historical brightness, showed strong, correlated variability at X-ray, ultraviolet, and optical wavelengths. The strongest variations were seen in medium-energy (similar to 1.5 keV) X-rays, with a normalized variability amplitude (NVA) of 24%. Weaker (NVA = 6%) variations (uncorrelated with those at lower energies) were seen at soft gamma-ray energies of similar to 100 keV. No significant variability was seen in softer (0.1-1 keV) X-ray bands. In the ultraviolet/optical regime, the NVA decreased from 9% to 1% as the wavelength increased from 1275 to 6900 Angstrom These data do not probe extreme ultraviolet (1200 Angstrom to 0.1 keV) or hard X-ray (2-50 keV) variability. The phase differences between variations in different bands were consistent with zero lag, with upper limits of less than or similar to 0.15 day between 1275 Angstrom and the other ultraviolet bands, less than or similar to 0,3 day between 1275 Angstrom and 1.5 keV, and less than or similar to 1 day between 1275 and 5125 Angstrom These tight limits represent more than an order of magnitude improvement over those determined in previous multi-wave-band AGN monitoring campaigns. The ultraviolet fluctuation power spectra showed no evidence for periodicity, but were instead well fitted with a very steep, red power law (a less than or equal to -2.5). If photons emitted at a ''primary'' wave band are absorbed by nearby material and ''reprocessed'' to produce emission at a secondary wave band, causality arguments require that variations in the secondary band follow those in the primary band. The tight interband correlation and limits on the ultraviolet and medium-energy X-ray lags indicate that the reprocessing region is smaller than similar to 0.15 it-day in size. After correcting for strong (a factor of greater than or similar to 15) line-of-sight absorption, the medium-energy X-ray luminosity variations appear adequate to drive the ultraviolet/optical variations. However, the medium-energy X-ray NVA is 2-4 times that in the ultraviolet, and the single-epoch, absorption-corrected X-ray/gamma-ray luminosity is only about one-third of that of the ultraviolet/optical/infrared, suggesting that at most about a third of the total low-energy flux could be reprocessed high-energy emission. The strong wavelength dependence of the ultraviolet NVAs is consistent with an origin in an accretion disk, with the variable emission coming from the hotter inner regions and nonvariable emission from the cooler outer regions. These data, when combined with the results of disk fits, indicate a boundary between these regions near a radius of order R approximate to 0.07 1t-day. No interband lag would be expected, as reprocessing (and thus propagation between regions) need not occur, and the orbital timescale of similar to 1 day is consistent with the observed variability timescale. However, such a model does not immediately explain the good correlation between ultraviolet and X-ray variations. C1 TEL AVIV UNIV,SACKLER FAC EXACT SCI,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. TEL AVIV UNIV,SACKLER FAC EXACT SCI,WISE OBSERV,IL-69978 TEL AVIV,ISRAEL. NASA,GODDARD SPACE FLIGHT CTR,ASTRON PROGRAM,COMP SCI CORP,GREENBELT,MD 20771. UNIV CALIF LOS ANGELES,DEPT ASTRON,LOS ANGELES,CA 90024. OHIO STATE UNIV,DEPT ASTRON,COLUMBUS,OH 43210. UNIV LEICESTER,DEPT ASTRON,LEICESTER LE1 7RH,LEICS,ENGLAND. EUROPEAN SPACE AGCY,ISO PROJECT,MADRID 28080,SPAIN. UNIV ST ANDREWS,SCH PHYS & ASTRON,ST ANDREWS KY16 9SS,FIFE,SCOTLAND. UNIV KENTUCKY,DEPT PHYS & ASTRON,LEXINGTON,KY 40506. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY PHYS LAB,GREENBELT,MD 20771. UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,BOULDER,CO 80309. UNIV STERNWARTE GOTTINGEN,D-37083 GOTTINGEN,GERMANY. CTR ETUD SACLAY,SERV ASTROPHYS,F-91191 GIF SUR YVETTE,FRANCE. COLGATE UNIV,DEPT PHYS & ASTRON,HAMILTON,NY 13346. LOWELL OBSERV,FLAGSTAFF,AZ 86001. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. EUREKA SCI INC,OAKLAND,CA. UNIV SCI & TECHNOL,CTR ASTROPHYS,HEFEI,ANHUI,PEOPLES R CHINA. CRIMEAN ASTROPHYS OBSERV,UA-334413 NAUCHNYI,CRIMEA,UKRAINE. LANDESSTERNWARTE KONIGSTUHL,D-69117 HEIDELBERG,GERMANY. UNIV NACL AUTONOMA MEXICO,INST ASTRON,MEXICO CITY 04510,DF,MEXICO. UNIV NEBRASKA,DEPT PHYS & ASTRON,LINCOLN,NE 68588. S AFRICAN ASTRON OBSERV,ZA-7935 CAPE TOWN,SOUTH AFRICA. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. USN,RES LAB,WASHINGTON,DC 20375. TECHNION ISRAEL INST TECHNOL,DEPT PHYS,IL-32000 HAIFA,ISRAEL. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. JAGIELLONIAN UNIV,ASTRON OBSERV,PL-30244 KRAKOW,POLAND. UNIV TORONTO,CANADIAN INST THEORET ASTROPHYS,TORONTO,ON M5S 1A1,CANADA. GEORGIA STATE UNIV,DEPT PHYS & ASTRON,ATLANTA,GA 30303. MOSCOW MV LOMONOSOV STATE UNIV,STERNBERG ASTRON INST,MOSCOW 119899,RUSSIA. UNIV CALGARY,DEPT PHYS & ASTRON,CALGARY,AB T2N 1N4,CANADA. MT ROYAL COLL,DEPT ENGN MATH & PHYS,CALGARY,AB T3E 6K6,CANADA. UNIV ROMA LA SAPIENZA,IST ASTRON,I-00161 ROME,ITALY. BOWLING GREEN STATE UNIV,DEPT PHYS & ASTRON,BOWLING GREEN,OH 43403. CHINESE ACAD SCI,SHANGHAI OBSERV,SHANGHAI,PEOPLES R CHINA. UNIV OVIEDO,FAC CIENCIAS,DEPT FIS,OVIEDO,ASTURIAS,SPAIN. INST ASTROFIS CANARIAS,E-38200 LA LAGUNA,TENERIFE,SPAIN. ESA,IUE OBSERV,MADRID 28080,SPAIN. UNIV EDINBURGH,ROYAL OBSERV EDINBURGH,EDINBURGH EH9 3HJ,MIDLOTHIAN,SCOTLAND. INST ASTROPHYS,F-75014 PARIS,FRANCE. AGNES SCOTT COLL,DEPT PHYS & ASTRON,DECATUR,GA 30030. AGNES SCOTT COLL,BRADLEY OBSERV,DECATUR,GA 30030. ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0EZ,ENGLAND. LAEFF,E-28080 MADRID,SPAIN. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85726. UNIV COLORADO,JILA,BOULDER,CO 80309. NATL INST STAND & TECHNOL,BOULDER,CO 80309. IRAM,F-38046 ST MARTIN DHERES,FRANCE. OSSERVATORIO ASTRON BOLOGNA,I-40126 BOLOGNA,ITALY. NATL CENT UNIV,INST ASTRON,CHUNGLI 32054,TAIWAN. EUROPEAN SO OBSERV,D-85748 GARCHING,GERMANY. ASTRON OBSERV,S-75120 UPPSALA,SWEDEN. UNIV KEELE,DEPT PHYS,KEELE ST5 5BG,STAFFS,ENGLAND. CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. CHINESE ACAD SCI,BEIJING ASTRON OBSERV,BEIJING 100080,PEOPLES R CHINA. NICHOLAS COPERNICUS ASTRON CTR,PL-00716 WARSAW,POLAND. RP Edelson, RA (reprint author), UNIV IOWA,DEPT PHYS & ASTRON,203 VAN ALLEN,IOWA CITY,IA 52242, USA. RI Morris, Simon/G-7981-2011; Oknyanskij, Victor/I-9267-2012; Johnson, Neil/G-3309-2014; Recondo, Carmen/B-1215-2012; Stirpe, Giovanna/O-9393-2015; OI Morris, Simon/0000-0003-4866-110X; Recondo, Carmen/0000-0001-9813-6798; Stirpe, Giovanna/0000-0002-3702-8731; Gaskell, C/0000-0003-4888-2009; Wilkes, Belinda/0000-0003-1809-2364; Perez, Enrique/0000-0001-9737-4559 NR 64 TC 141 Z9 144 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1996 VL 470 IS 1 BP 364 EP 377 DI 10.1086/177872 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VL723 UT WOS:A1996VL72300028 ER PT J AU Mason, CG Gehrz, RD Woodward, CE Smilowitz, JB Greenhouse, MA Hayward, TL Houck, JR AF Mason, CG Gehrz, RD Woodward, CE Smilowitz, JB Greenhouse, MA Hayward, TL Houck, JR TI Infrared observations of dust formation and coronal emission in Nova Aquilae 1995 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared, stars; novae, cataclysmic variables; stars, individual (Nova Aquilae 1995) ID OPTICAL-PROPERTIES; SILICATE GRAINS; SPECTRUM; CALIBRATION; GRAPHITE; STARS AB We report 1.25-18.5 mu m infrared spectrophotometric measurements of Nova Aquilae 1995. Photometric measurements were obtained over a four month period following the formation of an optically thin dust shell. Hydrogen and helium emission lines were evident throughout this period, along with strong near-infrared coronal line emission that appeared approximately 120 days after outburst. Both the photometric and the spectroscopic data suggest that the ejecta were clumpy, and that they contained both a dust component and a hot gas component. The outflow velocity of the ionized ejecta was observed to be similar to 1365-1600 km s(-1) (FWHM), and no appreciable deceleration of the ejecta was observed over the duration of these observations. Based on a M(v)-t(2) light decline relationship, we calculate a distance of similar to 3.6-4.8 kpc. C1 UNIV WYOMING,WYOMING INFRARED OBSERV,DEPT PHYS & ASTRON,LARAMIE,WY 82071. SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. CORNELL UNIV,CTR RADIOPHYS & SPACE RES,ITHACA,NY 14853. RP Mason, CG (reprint author), UNIV MINNESOTA,SCH PHYS & ASTRON,DEPT ASTRON,MINNEAPOLIS,MN 55455, USA. NR 36 TC 22 Z9 22 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1996 VL 470 IS 1 BP 577 EP 582 DI 10.1086/177889 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VL723 UT WOS:A1996VL72300045 ER PT J AU Dobereiner, S Junkes, N Wagner, SJ Zinnecker, H Fosbury, R Fabbiano, G Schreier, EJ AF Dobereiner, S Junkes, N Wagner, SJ Zinnecker, H Fosbury, R Fabbiano, G Schreier, EJ TI ROSAT HRI observations of Centaurus A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, individual (Centaurus A); galaxies, jets; X-rays, galaxies ID RAY-EMITTING GAS; RADIO LOBES; NGC-5128 AB We present results from a sensitive high-resolution X-ray observation of the nearby active galaxy Centaurus A (NGC 5128) with the ROSAT high-resolution imager (HRI). The 65 ks X-ray image clearly distinguishes different components of the X-ray emission from Cen A: the nucleus and the jet, the diffuse galaxy halo, and a number of individual sources associated with the galaxy. The luminosity of the nucleus increased by a factor of 2 compared to an earlier ROSAT observation in 1990. The high spatial resolution of the ROSAT HRI shows that most of the knots in the jet are extended both along and perpendicular to the jet axis. We report the detection of a new X-ray feature, at the opposite side of the X-ray jet, which is probably due to compression of hot interstellar gas by the expanding southwestern inner radio lobe. C1 ASTRON INST POTSDAM,D-14482 POTSDAM,GERMANY. LANDESSTERNWARTE HEIDELBERG,D-69117 HEIDELBERG,GERMANY. EUROPEAN SO OBSERV,SPACE TELESCOPE EUROPEAN COORDINATING FACIL,D-85748 GARCHING,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. RP Dobereiner, S (reprint author), MAX PLANCK INST EXTRATERR PHYS,KARL SCHWARZSCHILD STR 1,D-85740 GARCHING,GERMANY. OI Fosbury, Robert/0000-0001-9975-8003 NR 13 TC 20 Z9 20 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1996 VL 470 IS 1 BP L15 EP & DI 10.1086/310288 PN 2 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VL724 UT WOS:A1996VL72400004 ER PT J AU Almany, GR Baldwin, CC AF Almany, GR Baldwin, CC TI A new Atlantic species of Acanthemblemaria (Teleostei: Blennioidei: Chaenopsidae): Morphology and relationships SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID PHYLOGENETIC-RELATIONSHIPS; GENUS-ACANTHEMBLEMARIA; PISCES AB Acanthemblemaria johnsoni is described from six specimens collected from shallow coral reefs at the north end of the Caribbean island of Tobago. The new species differs from all other Atlantic species of Acanthemblemaria by the combined spinous and soft dorsal-fin ray count of XXIV, 12-13. Evolutionary relationships of the new species are discussed in relation to the phylogeny of the genus proposed by Hastings (1990). RP Almany, GR (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DIV FISHES,MRC 159,WASHINGTON,DC 20560, USA. NR 12 TC 6 Z9 6 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 419 EP 429 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400002 ER PT J AU Lemaitre, R Felder, DL AF Lemaitre, R Felder, DL TI A new species of ghost shrimp of the genus Sergio Manning&Lemaitre, 1994 (Crustacea: Decapoda: Callianassidae) from the Caribbean coast of Colombia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID SEA AB A new species of ghost shrimp, Sergio sulfureus, is described from shoreline habitats of Bani, on the Caribbean coast of Colombia. This new species is the seventh known of the genus Sergio Manning & Lemaitre, and is most similar to S. guassutinga (Rodrigues), from Brazil, and S. mericeae Manning & Felder, from Florida. The new species can be distinguished from these two primarily by characters derived from the major cheliped, including color. The new species is described in detail, and information is given on adult and immature stages, habitat, and co-occurring burrowing decapods. C1 UNIV SW LOUISIANA,DEPT BIOL,LAFAYETTE,LA 70504. RP Lemaitre, R (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 9 TC 4 Z9 6 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 453 EP 463 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400005 ER PT J AU Tavares, M Lemaitre, R AF Tavares, M Lemaitre, R TI Lonchodactylus messingi, a new genus and species of Cyclodorippidae (Crustacea: Decapoda: Brachyura) from the Bahamas SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new genus and species of the family Cyclodorippidae, Lonchodactylus messingi, is described from specimens collected in the Bahamas using a research submersible. The new genus is more closely related to two Indo-West Pacific genera (Genkaia Miyake & Takeda and Phyllotymolinum Tavares) than to any other cyclodorippid from the coasts of America. Morphological similarities and differences between these genera are discussed. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. RP Tavares, M (reprint author), UNIV SANTA URSULA,DEPT BIOL ANIM,BR-22231045 RIO JANEIRO,BRAZIL. RI Tavares, Marcos/F-7151-2012 OI Tavares, Marcos/0000-0002-7186-5787 NR 7 TC 2 Z9 2 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 464 EP 469 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400006 ER PT J AU Lewis, JJ Bowman, TE AF Lewis, JJ Bowman, TE TI The subterranean asellids of Texas (Crustacea: Isopoda: Asellidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Seven species of subterranean asellids are recognized from Texas. Four are species of Lirceolus, including Caecidotea bisetus now reassigned to Lirceolus, and Lirceolus hardeni, n. sp., described from caves and springs in east-central Texas. Previously known only from the type-locality, a new collection site for Lirceolus pilus is also reported. Three species of subterranean Caecidotea are known from the state. Caecidotea reddelli is redescribed and reported from both caves and collection sites that sample phreatic habitats such as wells and seeps. Caecidotea bilineata, n. sp., is a phreatobite occurring in non-cave groundwater habitats in northeastern Texas. A troglobitic Caecidotea sp. from Border Cave, Culberson County remains undescribed due to insufficient material. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. NR 25 TC 4 Z9 4 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 482 EP 500 PG 19 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400009 ER PT J AU Kornicker, LS McKenzie, KG AF Kornicker, LS McKenzie, KG TI The adult male of the myodocopid ostracode Philomedes cubitum Kornicker, 1975, from the Strait of Magellan (Crustacea: Ostracoda: Myodocopina) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The carapace and appendages of the adult male of Philomedes cubitum Kornicker, 1975, are described and illustrated from a specimen collected in the Strait of Magellan, which is the type locality. Observed sexual dimorphism is normal for the genus. C1 UNIV MELBOURNE,DEPT GEOL,MELBOURNE,FL. RP Kornicker, LS (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 11 TC 0 Z9 0 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 517 EP 525 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400012 ER PT J AU Child, CA AF Child, CA TI Additions to the Pycnogonida fauna of Carrie Bow Cay, Belize, middle America SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID ISLANDS AB Five additional species are added to the 31 species in 14 genera known to inhabit reefs in the vicinity of Carry Bow Gay, Belize. Four of these species are known from other localities while one is new; Ascorhynchus petilus, new species. The new species is described, illustrated, and its morphology compared with related species in this genus. Additional illustrations are provided for another species, Parapallene bermudensis Lebour, from an adult specimen where the species was known previously only from juveniles. RP Child, CA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 42 TC 1 Z9 1 U1 1 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 526 EP 532 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400013 ER PT J AU Child, CA AF Child, CA TI Pycnogonida of the western Pacific islands .12. A recent diving survey of Okinawa, Ryukyu Islands SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID SOUTHERN AB Seven known pycnogonid species are reported from the Ryukyu Islands at Okinawa, five of them found here for the first time and one new species. The new species, Parapallene virgosa, is described, illustrated, compared with others in its genus and with several species in other genera displaying a few similar characteristics. Previous Okinawan pycnogonid literature is discussed in light of these additional species and distribution of all species is included. RP Child, CA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 37 TC 1 Z9 1 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 533 EP 539 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400014 ER PT J AU Child, CA AF Child, CA TI Pycnogonida of the western Pacific islands .13. Collections from Indonesia, Melanesia, and Micronesia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Twenty nine species are reported in collections from Java and Sunda Strait in Indonesia, Papua New Guinea and Fiji in Melanesia, and from three island groups in the Caroline Islands, Micronesia. Current distribution for each species is given along with remarks on the specimens where pertinent. Three new species are described: Achelia bullosa, Tanystylum papuensis, and Anoplodactylus brochus. Each new species is illustrated and compared with congeners. RP Child, CA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 79 TC 10 Z9 10 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 540 EP 559 PG 20 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400015 ER PT J AU Zecchini, F Vecchione, M Roper, CFE AF Zecchini, F Vecchione, M Roper, CFE TI A quantitative comparison of hectocotylus morphology between Mediterranean and western Atlantic populations of the squid Illex coindetii (Mollusca: Cephalopoda: Oegopsida: Ommastrephidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Geographic variation in morphology of the commercially important squid species Illex coindetii has led to speculation about possible taxonomic differences among populations. We compared hectocotylus morphology between western Atlantic specimens, from the Gulf of Mexico and Caribbean, and Mediterranean specimens, from the Tyrrhenian Sea. Although a few differences were found in morphometrics and meristics, we conclude that the two populations are conspecific. C1 NATL MUSEUM NAT HIST,NATL MARINE FISHERIES SERV,WASHINGTON,DC 20560. SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL MOLLUSKS,WASHINGTON,DC 20560. RP Zecchini, F (reprint author), UNIV PISA,DIPARTIMENTO SCI AMBIENTE TERRITORIO,VIA VOLTA 6,I-56126 PISA,ITALY. NR 11 TC 6 Z9 6 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 1996 VL 109 IS 3 BP 591 EP 599 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VM334 UT WOS:A1996VM33400019 ER PT J AU Colinvaux, PA DeOliveira, PE Moreno, JE Miller, MC Bush, MB AF Colinvaux, PA DeOliveira, PE Moreno, JE Miller, MC Bush, MB TI A long pollen record from lowland Amazonia: Forest and cooling in glacial times SO SCIENCE LA English DT Article ID RAIN-FOREST; BASIN; VEGETATION; MAXIMUM; CLIMATE; PANAMA; MODEL AB A continuous pollen history of more than 40,000 years was obtained from a lake in the lowland Amazon rain forest. Pollen spectra demonstrate that tropical rain forest occupied the region continuously and that savannas or grasslands were not present during the last glacial maximum. The data suggest that the western Amazon forest was not fragmented into refugia in glacial times and that the lowlands were not a source of dust. Glacial age forests were comparable to modern forests but also included species now restricted to higher elevations by temperature, suggesting a cooling of the order of 5 degrees to 6 degrees C. C1 FIELD MUSEUM NAT HIST,CHICAGO,IL 60605. UNIV CINCINNATI,DEPT BIOL,CINCINNATI,OH 45221. RP Colinvaux, PA (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO,AA 34002, USA. RI De Oliveira, Paulo/B-4559-2017; OI De Oliveira, Paulo/0000-0003-1040-4001; Bush, Mark/0000-0001-6894-8613 NR 42 TC 357 Z9 370 U1 3 U2 53 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD OCT 4 PY 1996 VL 274 IS 5284 BP 85 EP 88 DI 10.1126/science.274.5284.85 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VK748 UT WOS:A1996VK74800051 ER PT J AU deQueiroz, K AF deQueiroz, K TI Including the characters of interest during tree reconstruction and the problems of circularity and bias in studies of character evolution SO AMERICAN NATURALIST LA English DT Article ID CORRELATED EVOLUTION; PHYLOGENETIC ANALYSIS; TESTS; HYPOTHESES; SCENARIOS; INFERENCE; BEHAVIOR; SYSTEMS; FISHES; ORIGIN RP deQueiroz, K (reprint author), SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT VERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. NR 37 TC 63 Z9 66 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD OCT PY 1996 VL 148 IS 4 BP 700 EP 708 DI 10.1086/285948 PG 9 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA VL154 UT WOS:A1996VL15400007 ER PT J AU Jones, BF Fischer, DA Stauffer, JR AF Jones, BF Fischer, DA Stauffer, JR TI Keck rotational velocities of the faintest Pleiades and Hyades members SO ASTRONOMICAL JOURNAL LA English DT Article ID LOW-MASS STARS; T-TAURI STARS; ALPHA-PERSEI CLUSTER; MAIN-SEQUENCE; PROMINENCE ACTIVITY; RADIAL-VELOCITIES; UV CETI; X-RAY; ACCRETION; EVOLUTION AB We have derived rotational velocities of faint Pleiades and Hyades members from high resolution spectra obtained with the HIRES spectrograph on the Keck telescope. The stars observed span the mass where stilts become totally convective. We find no change in the character of the distribution of rotational velocities at this point, but instead a gradual trend of increasing rotational velocities. The range in rotational velocities al a given mass in the Pleiades decreases with decreasing mass, and the amount of spindown between Pleiades and Hyades age decreases with decreasing mass, We observe for two of our stars a broad Hn emission component. (C) 1996 American Astronomical Society. C1 UNIV CALIF SANTA CRUZ,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP Jones, BF (reprint author), UNIV CALIF OBSERV,LICK OBSERV,SANTA CRUZ,CA 95064, USA. OI Fischer, Debra/0000-0003-2221-0861 NR 44 TC 44 Z9 44 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1996 VL 112 IS 4 BP 1562 EP 1569 DI 10.1086/118123 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VK840 UT WOS:A1996VK84000019 ER PT J AU Prosser, CF Randich, S Stauffer, JR Schmitt, JHMM Simon, T AF Prosser, CF Randich, S Stauffer, JR Schmitt, JHMM Simon, T TI ROSAT pointed observations of the Alpha Persei cluster SO ASTRONOMICAL JOURNAL LA English DT Article ID LOW-MASS STARS; X-RAY FLARE; SPECTROSCOPY; EVOLUTION; EXOSAT AB We extend the results of a previous ROSAT x-ray raster survey of the open cluster alpha Persli by the analysis of three 22-25 ksec ROSATPSPC pointings in this relatively nearby (d similar to 170 pc) and young (age similar to 50 Myr) open cluster. The present study reports on those catalogued stars in the cluster region which are found to be associated, or possibly associated, with an x-ray sourer. Out of a total of 222 sources, approximately 80 sources are identified with a catalogued star, We detect all previously known K dwarfs, and a majority of M dwarfs within the higher sensitivity, inner PSPC regions. The results from the deep pointings are consistent with those from the previous raster survey of this cluster in terms of the x-ray luminosities measured for sources in common, the detection frequencies among cluster members as a function of spectral type, and the distribution of L(X) as a function of color. The x-ray detections and upper limits provided by the PSPC observations have been combined with the raster survey results to create a merged raster/PSPC dataset reflecting the x-ray properties of the alpha Per cluster. The upsilon sin i-activity relation among G/K members is reviewed using the combined dataset. The alpha Per members with upsilon sin i > 30 km/s all show saturated levels of coronal activity, with the saturation level decreasing slowly from log(L(X)/L(bol))similar to-3 at 50 km/s to log(L(X)/L(bol)similar to-3.4 at 200 km/s. The stars with upsilon sin i < 15 km/s, most with only upsilon sin i upper limits, show a wide range in coronal activity (-4.3 < L(X)/L(bol) < -2.9), we assume that coronal activity in alpha Per increases with increasing rotation rate for v sin i < 15 km/s, but the functional form of the relation cannot be determined from existing data. The x-ray luminosity distribution functions among F-M alpha Per stars have been recomputed using the merged raster/PSPC dataset and compared to the Pleiades. The findings of the raster survey are confirmed, with F and G alpha Per dwarfs clearly exhibiting higher average emission than their Pleiades counterparts, while alpha Per K dwarfs show only slightly higher activity. The revised alpha Per M dwarf XLDF is in closer agreement with the Pleiades M dwarf distribution. We discuss the apparent detection in x rays of the one evolving blue supergiant member or this cluster, a Per itself. In addition, the sensitive PSPC observations may have detected x-ray sources associated with very low mass candidate cluster members al spectral type similar to M5. We also provide a summary of the x-ray flare characteristics (peak similar to 10(31) ergs/s) for three alpha Per members. (C) 1996 American Astronomical Society. C1 MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. UNIV HAWAII, INST ASTRON, HONOLULU, HI 96822 USA. RP Prosser, CF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, MS-66, CAMBRIDGE, MA 02138 USA. OI Randich, Sofia/0000-0003-2438-0899 NR 53 TC 84 Z9 84 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 1996 VL 112 IS 4 BP 1570 EP 1587 DI 10.1086/118124 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VK840 UT WOS:A1996VK84000020 ER PT J AU Ball, R Meixner, MM Keto, E Arens, JF Jernigan, JG AF Ball, R Meixner, MM Keto, E Arens, JF Jernigan, JG TI Thermal dust imaging of the ultracompact H II region G29.96-0.02 SO ASTRONOMICAL JOURNAL LA English DT Article ID PHYSICAL-PROPERTIES; INFRARED SOURCES; EMISSION; STARS; MODELS; SPECTROPHOTOMETRY; DYNAMICS; SPECTRA; BUBBLES; GRAINS AB We have obtained mid-infrared images of the ultracompact H II region G29.96-0.02 at 1 '' resolution. These include three broadband images at 8.5, 9.7, and 12.0 mu m and three narrowband images covering the spectrum around the 12.8 mu m [Ne II] emission line. The appearance of the object in all bands is basically similar to the arcuate or ''cometary'' shape seen in previously published high-resolution radio maps. At our shortest wavelength of 8.5 mu m, the faint, diffuse emission from the cometary ''tail'' is enhanced compared to its brightness at other wavelengths. Taking advantage of well-matched passbands, we have used the ratio between the images at 12.0 and at 8.5 mu m to construct maps of the dust color temperature T-d and emission optical depth tau(em) in the object. The optical depth is sharply peaked along a long, thin ridge near the leading edge of the cometary are. The shape of this ridge is nearly identical to that seen in the high-resolution 2 cm maps, strongly suggesting that the dust which is warm enough to emit at 8 and 12 mu m is inside or extremely close to the zone of ionized gas in G29.96-0.02. This conclusion is further bolstered by the essentially identical distribution of the [Ne II] emission and the thermal dust continuum at adjacent wavelengths. The key feature of the dust temperature map is its lack of marked variation. The great majority of the nebula shows temperatures between 190 and 240 K. The small variations that do occur present a clear pattern. At the center of the ridge of high tau(rmem), T-d is around 210 K. Moving outward to the wings of the are, the temperature falls slowly to about 190 K at the extreme ends. On the other hand, moving back along the symmetry axis into the nebula's tail we find that mean temperatures increase to around 230 K, with a good deal of scatter. We have tried modeling these temperature variations using some simple concepts derived from earlier radiative transfer work on related objects, together with a published model of G29.96-0.02 as a bow shock. Unlike our previous success in applying such a framework to our observations of the ultracompact source G5.89-0.39, the models fail to match the temperature pattern in G29.96-0.02. Of several possible processes which may account for the discrepancy, an increased abundance of small grains caused by shock processing of the dust seems to present the fewest obvious difficulties. (C) 1996 American Astronomical Society. C1 LAWRENCE LIVERMORE NATL LAB, INST GEOPHYS & PLANETARY PHYS, LIVERMORE, CA 94550 USA. UNIV ILLINOIS, DEPT ASTROPHYS, URBANA, IL 61801 USA. SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. UNIV CALIF BERKELEY, SPACE SCI LAB, BERKELEY, CA 94720 USA. NR 47 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1996 VL 112 IS 4 BP 1645 EP 1658 DI 10.1086/118130 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VK840 UT WOS:A1996VK84000026 ER PT J AU Mikolajewska, J Kenyon, SJ AF Mikolajewska, J Kenyon, SJ TI The inscrutable hot component in the symbiotic binary Z Andromedae SO ASTRONOMICAL JOURNAL LA English DT Article ID SPECTROSCOPIC ORBITS; ACCRETION DISKS; COOL COMPONENTS; HE-I; STARS; SYSTEMS; MODEL; ULTRAVIOLET; SUPERHUMPS; EVOLUTION AB We analyze optical and ultraviolet spectroscopic observations of the symbiotic binary star Z Andromedae. This system consists of an M3-M4 giant and a hot component surrounded by an ionized nebula. The orbital mass function is consistent with M(g) similar to 2 M. and M(h) similar to 0.5-1 M. as in other symbiotic stars. The nature of the hot component remains unclear. Most quiescent data are consistent with a luminous stellar source powered by thermonuclear burning. The decrease in the effective temperature of the hot component and the fluxes of most high ionization emission lines during outburst provides further support for a nuclear-powered hot component. However, the evolution of He II emission lines in outburst, the short outburst recurrence times, and the presence of short period oscillations in the outburst light curves are all more easily interpreted with an accretion disk model, in which a luminous disk surrounds a solar-type main sequence star. Better models for the light variations and the evolution of emission lines during outburst are needed to choose between accretion disk and thermonuclear models for the hot component. (C) 1996 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Mikolajewska, J (reprint author), NICOLAUS COPERNICUS ASTRON CTR, BARTYCKA 18, PL-00716 WARSAW, POLAND. OI Kenyon, Scott/0000-0003-0214-609X NR 86 TC 58 Z9 59 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1996 VL 112 IS 4 BP 1659 EP 1669 DI 10.1086/118131 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VK840 UT WOS:A1996VK84000027 ER PT J AU Sugars, BJA Evans, NR AF Sugars, BJA Evans, NR TI Z Lac: Orbital circularization in supergiants SO ASTRONOMICAL JOURNAL LA English DT Article ID CEPHEID Z-LACERTAE; VELOCITY CURVES; BINARIES; STARS AB We have obtained new radial velocities for the binary Cepheid Z Lac. These data have been combined with new velocities by Imbert (1996) and other data in the literature to derive an orbit. The orbital period is close to a year, making Z Lac the Cepheid with the shortest orbital period known. It is also the only Cepheid with an orbital eccentricity indistinguishable from zero, Comparison between the projected semi-major axis and the radii of 5 and 7 M. stars at the tip of the red giant branch [from the evolutionary tracks of Schaller et al. (1992)] indicates that the orbit was probably circularized during the red giant phase. (C) 1996 American Astronomical Society. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. YORK UNIV,N YORK,ON M3J 1P3,CANADA. TORONTO SUN PUBLISHING CORP,TORONTO,ON M5A 3X5,CANADA. NR 26 TC 14 Z9 14 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1996 VL 112 IS 4 BP 1670 EP 1677 DI 10.1086/118132 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VK840 UT WOS:A1996VK84000028 ER PT J AU Bartel, N Chandler, JF Ratner, MI Shapiro, II Pan, R Cappallo, RJ AF Bartel, N Chandler, JF Ratner, MI Shapiro, II Pan, R Cappallo, RJ TI Toward a frame tie via millisecond pulsar VLBI SO ASTRONOMICAL JOURNAL LA English DT Article ID ASTROMETRY; EPHEMERIDES; POSITIONS; EQUINOX; SYSTEM AB Millisecond pulsars, by virtue of their relatively stable rotations and sharp poises of nearly point-source radio emission, can be used to tie Earth-orbit-oriented reference frames to Earth-spin-oriented reference frames with unprecedented accuracy through a combination of timing and VLBI measurements. From 18 cm Mark IIIA VLBI observations on 1987 February 27, we determined the coordinates of PSR B1937+21 relative to those of the extragalactic source 1923+210, whose coordinates in a quasi-inertial extragalactic reference frame have a standard error of similar to 0.1 mas. These coordinates of PSR B1937+21 at our epoch of observation are: alpha(J2000)=19(h)39(m)38.5613(s)+/-0.0004(s), delta(J2000)=21 degrees 34'59.130 ''+/-0.003 ''. They agree within the root-sum-square standard errors with those determined via VLBI by Petit (1994) and Dewey et al. (1996) and with those yielded by the application of the rotation of an indirect frame tie of Folkner er al. (1994) to the pulse-timing positions obtained by Kaspi et al. (1994) with JPL's DE200 ephemeris. To allow comparison of these positions with pulse-timing positions obtained with respect to other ephemerides. we compute rotation matrices for transforming among the various ephemerides. Pulsar coordinates determined in the frame of one specific planetary ephemeris can now be convened to the frame of any of several other planetary ephemerides or to the IERS frame (via the rotation matrix of Folkner et al.) with the conversion procedure given in this paper. Using our own PEP740 ephemeris we obtained a pulse-timing position for PSR B1937+21, and, applying the: appropriate rotations, we find agreement within 0.3 mas with that obtained by Kaspi pr al. with DE200, i.e., within the root-sum-square standard error in each coordinate. We also discuss how a direct frame time tie can be established between these ephemerides and the extragalactic reference frame. (C) 1996 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MIT,HAYSTACK OBSERV,WESTFORD,MA 01886. RP Bartel, N (reprint author), YORK UNIV,DEPT PHYS & ASTRON,4700 KEELE ST,N YORK,ON M3J 1P3,CANADA. NR 33 TC 14 Z9 15 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1996 VL 112 IS 4 BP 1690 EP 1696 DI 10.1086/118135 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VK840 UT WOS:A1996VK84000031 ER PT J AU Lasota, JP Narayan, R Yi, I AF Lasota, JP Narayan, R Yi, I TI Mechanisms for the outbursts of soft X-ray transients SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; black hole physics; instabilities; binaries, close; X-rays, stars ID DWARF NOVA OUTBURSTS; BLACK-HOLE; SIGMA-OBSERVATIONS; ACCRETION DISKS; MODEL; QUIESCENCE; INSTABILITY; ADVECTION; SPEED; X-1 AB We show that the Keplerian thin disk in quiescent Soft X-ray Transients cannot extend down to the last stable orbit around the central black hole. We analyse the properties of the Narayan, McClintock & Yi (1996) model of quiescent Soft X-ray Transients in which the cold Keplerian disk has its inner edge at a large transition radius and transforms to a hot, advection-dominated flow on the inside. We show that outbursts of transient sources could be triggered in this model either by a pure thermal accretion disk instability or by a disk instability generated by an enhanced mass transfer from the stellar companion. Both mechanisms operate in the outer thin disk and could be at work, either in different systems or in the same system at different epochs, depending on the mass transfer rate and the value of the viscosity parameter alpha(t) of the thin disk. We show that the recurrence time between outbursts in SXTs can be explained with values of alpha(t) similar to these required by the dwarf nova disk instability model instead of the unreasonably low values needed in the model in which the thin disks extends down to the last stable orbit. We extend the Narayan, McClintock & Yi (1996) model to the case when the outer disk is non-stationary. We show that such disk is too cold to account for the observed UV flux. This difficulty is common to all models in which the outer disk is assumed to be optically thick. C1 OBSERV PARIS, DARC, CNRS, UPR 176, F-92195 MEUDON, FRANCE. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV CALIF SANTA BARBARA, INST THEORET PHYS, SANTA BARBARA, CA 93106 USA. INST ADV STUDY, PRINCETON, NJ 08540 USA. RP Lasota, JP (reprint author), WEIZMANN INST SCI, DEPT CONDENSED MATTER PHYS, IL-76100 REHOVOT, ISRAEL. NR 59 TC 61 Z9 62 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 1996 VL 314 IS 3 BP 813 EP 820 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VN759 UT WOS:A1996VN75900017 ER PT J AU Latham, DW Nordstrom, B Andersen, J Torres, G Stefanik, RP Thaller, M Bester, MJ AF Latham, DW Nordstrom, B Andersen, J Torres, G Stefanik, RP Thaller, M Bester, MJ TI Accurate mass determination for double-lined spectroscopic binaries by digital cross-correlation spectroscopy: DM Virginis revisited SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods, data analysis; stars, binaries, spectroscopic; stars, binaries, eclipsing; stars, evolution; stars, fundamental parameters; stars, individual, DM Vir ID ABSOLUTE DIMENSIONS; ECLIPSING BINARIES; STELLAR MASSES; STARS; EVOLUTION; MODELS; RADII AB Fundamental mass determinations in eclipsing binaries rely on radial velocities derived from double-lined spectra. We evaluate the performance of the CfA Digital Speedometers for deriving radial velocities of double-lined systems, using simulated observations of composite spectra. When XCSAO (Kurtz et al. 1992) is used to calculate a one-dimensional cross-correlation, simple fits to the double peaks in the correlation function can lead to systematic errors as large as 3 km s(-1) due to the effects of line blending. The two-dimensional correlation scheme TODCOR (Zucker & Mazeh 1994) can reduce the systematic errors by an order of magnitude. We apply TODCOR to a new mass determination for the F-type eclipsing binary DM Vir, achieving an accuracy of 0.6%. The improved physical properties of DM Vir agree very well with stellar evolution models incorporating the most recent opacity data, both with and without convective core overshooting. and for reasonable assumptions about the chemical composition. The age of DM Vir is found to be 1.75 +/- 0.20 10(9) yr, metallicity being the dominant source of uncertainty. C1 NIELS BOHR INST ASTRON PHYS & GEOPHYS, ASTRON OBSERV, DK-2100 COPENHAGEN, DENMARK. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. GEORGIA STATE UNIV, DEPT PHYS & ASTRON, ATLANTA, GA 30303 USA. NR 21 TC 55 Z9 55 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 1996 VL 314 IS 3 BP 864 EP 870 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VN759 UT WOS:A1996VN75900023 ER PT J AU Hartmann, D Kalberla, PMW Burton, WB Mebold, U AF Hartmann, D Kalberla, PMW Burton, WB Mebold, U TI Stray-radiation correction as applied to the Leiden/Dwingeloo survey of HI in the galaxy SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article DE methods data analysis; surveys; radio lines, ISM; telescopes AB This article describes the stray-radiation correction that was applied to the HI observations of the Leiden/Dwingeloo survey of Hartmann & Burton. This correction involved convolving the empirically-determined antenna pattern with the measured all-sky HI distribution. The importance of the correction is demonstrated and practice regarding its application described. The general algorithm used here is presented. The results obtained with this algorithm are compared to those following from other methods. The 0.07 K sensitivity level of the survey depends critically on the success of the stray-radiation correction. C1 STERREWACHT LEIDEN,NL-2300 RA LEIDEN,NETHERLANDS. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV BONN,INST RADIOASTRON,D-53121 BONN,GERMANY. NR 27 TC 45 Z9 45 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD OCT PY 1996 VL 119 IS 1 BP 115 EP 151 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VK578 UT WOS:A1996VK57800011 ER PT J AU Seljak, U Zaldarriaga, M AF Seljak, U Zaldarriaga, M TI A line-of-sight integration approach to cosmic microwave background anisotropies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology, theory; methods, numerical ID COLD DARK MATTER; RADIATION; UNIVERSES; PERTURBATIONS; FLAT AB We present a new method for calculating linear cosmic microwave background (CMB) anisotropy spectra based on integration over sources along the photon past light cone. In this approach the temperature anisotropy is written as a time integral over the product of a geometrical term and a source term. The geometrical term is given by radial eigenfunctions, which do not depend on the particular cosmological model. The source term can be expressed in terms of photon, baryon, and metric perturbations, all of which can be calculated using a small number of differential equations. This split clearly separates the dynamical from the geometrical effects on the CMB anisotropies. More importantly, it allows us to significantly reduce the computational time compared to standard methods. This is achieved because the source term, which depends on the model and is generally the most time-consuming part of calculation, is a slowly varying function of wavelength and needs to be evaluated only in a small number of points. The geometrical term, which oscillates much more rapidly than the source term, does not depend on the particular model and can be precomputed in advance. Standard methods that do not separate the two terms require much higher number of evaluations. The new method leads to about 2 orders of magnitude reduction in CPU time when compared to standard methods and typically requires a few minutes on a workstation for a single model. The method should be especially useful for accurate determinations of cosmological parameters from CMB anisotropy and polarization measurements that will become possible with the next generation of experiments. A program implementing this method can be obtained from the authors. C1 MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 35 TC 1605 Z9 1610 U1 2 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1996 VL 469 IS 2 BP 437 EP 444 DI 10.1086/177793 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VJ788 UT WOS:A1996VJ78800001 ER PT J AU Drake, JJ Stern, RA Stringfellow, GS Mathioudakis, M Laming, JM Lambert, DL AF Drake, JJ Stern, RA Stringfellow, GS Mathioudakis, M Laming, JM Lambert, DL TI Detection of quiescent extreme-ultraviolet emission from the very low mass dwarf van Biesbroeck 8: Evidence for a turbulent field dynamo SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; stars, coronae; stars, individual (van Biesbroeck 8); stars, low-mass, brown dwarfs; turbulence; ultraviolet, stars ID LOWER MAIN-SEQUENCE; X-RAY-EMISSION; STELLAR CORONAE; STARS; ROTATION; SCALE; END AB We report the detection of quiescent EUV emission from the very low mass dwarf VB 8 by the Extreme Ultraviolet Explorer (EUVE) in the Lexan/B band (65-190 Angstrom). We interpret this emission in terms of a hot coronal plasma and combine this information with previous X-ray detections to estimate the quiescent plasma temperature and emission measure. The combined observations made by Einstein, ROSAT, and EUVE between 1979 and 1994 are consistent with a quiescent coronal plasma temperature of(2-6) x 10(6) degrees and indicate the same emission measure to within a factor of about 2. The non-flaring corona of VB 8 then appears relatively constant over timescales of more than 10 yr. Our results are consistent with the picture of a turbulently driven or distributive dynamo for VB 8, rather than with a large-scale field dynamo which appears to dominate the solar corona. Evidence from X-ray and optical data concerning the long-term coronal variability of the more active stars of higher mass also points toward the idea that active late-type stars in general are dominated by a turbulent dynamo. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 01238 USA. SOLAR & ASTROPHYS LAB, PALO ALTO, CA 94304 USA. UNIV CALIF BERKELEY, CTR EUV ASTROPHYS, BERKELEY, CA 94720 USA. PENN STATE UNIV, DEPT ASTRON & ASTROPHYS, UNIVERSITY PK, PA 16802 USA. UNIV COLORADO, CTR ASTROPHYS & SPACE ASTRON, BOULDER, CO 80309 USA. ARMAGH OBSERV, ARMAGH BT61 9DG, NORTH IRELAND. SACHS FREEMAN ASSOCIATES INC, LANDOVER, MD 20785 USA. USN, RES LAB, EO HULBURT CTR SPACE RES, WASHINGTON, DC 20375 USA. UNIV TEXAS, DEPT ASTRON, AUSTIN, TX 78712 USA. RP UNIV CALIF BERKELEY, CTR EUV ASTROPHYS, 2150 KITTREDGE ST, BERKELEY, CA 94720 USA. NR 44 TC 26 Z9 26 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1996 VL 469 IS 2 BP 828 EP 833 DI 10.1086/177830 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VJ788 UT WOS:A1996VJ78800038 ER PT J AU Szkody, P Long, KS Sion, EM Raymond, JC AF Szkody, P Long, KS Sion, EM Raymond, JC TI ASCA observations of U Geminorum during quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars, individual (U Geminorum); X-rays, stars ID HOPKINS-ULTRAVIOLET-TELESCOPE; X-RAY OBSERVATIONS; CATACLYSMIC VARIABLES; DWARF NOVAE; WHITE-DWARF; ACCRETION DISKS; BOUNDARY-LAYER; LIGHT CURVES; EMISSION; EVOLUTION AB ASCA observations of the dwarf nova U Gem separated by 3 weeks during a long quiescent interval show no noticeable differences in count rates nor in the relatively hard (7-10 keV) X-ray spectrum. However, there are orbital phase-dependent variations in the quiescent X-ray light curves, which are similar to the absorption dips previously reported during outburst and decline from outburst. The dips are only apparent at low energies, and the different structure of the light curves indicates changes in the absorbing material between the two observations. These results imply that the X-ray emission at quiescence must be confined to a small area and that absorbing material must be located at very stable positions far out from the orbital plane. C1 SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. VILLANOVA UNIV,DEPT ASTRON,VILLANOVA,PA 19085. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Szkody, P (reprint author), UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195, USA. NR 41 TC 28 Z9 28 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1996 VL 469 IS 2 BP 834 EP 840 DI 10.1086/177831 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VJ788 UT WOS:A1996VJ78800039 ER PT J AU Long, KS Mauche, CW Raymond, JC Szkody, P Mattei, JA AF Long, KS Mauche, CW Raymond, JC Szkody, P Mattei, JA TI EUVE observations of U Geminorum in outburst SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, eclipsing; novae, cataclysmic variables; stars, individual (U Geminorum); ultraviolet, stars ID X-RAY-EMISSION; EXTREME-ULTRAVIOLET EXPLORER; CATACLYSMIC VARIABLES; ACCRETION DISKS; DWARF NOVAE; BOUNDARY-LAYER; URSAE-MAJORIS; LIGHT CURVES; WHITE-DWARF; SS CYGNI AB We have observed U Gem during the peak and declining phases of a wide outburst in 1993 December with the Extreme Ultraviolet Explorer (EUVE) satellite. At peak, U Gem was one of the brightest EUV sources in the sky. The spectrum of the source is complex. Fitted to a blackbody spectrum, the apparent temperature at peak is similar to 140,000 K, the luminosity is similar to 4 x 10(34)(D/90 pc)(2) ergs s(-1), and the minimum size of the emitting region is comparable to that of the white dwarf (WD). If the EUV emission arises primarily from the boundary layer, then the boundary layer luminosity in U Gem is comparable to the disk luminosity. The EUV source is partially eclipsed at orbital phases 0.6-0.8. The eclipse spectrum, which we associate with a wind emerging from the vicinity of the white dwarf, is dominated by emission features. The identification of these emission features with transitions expected in a relatively cool (T < 160,000 K), photoionized plasma helps to resolve a controversy concerning the ionization state of winds of dwarf novae. The EUV lines arise from the dominant ionization states of the wind, and their strengths suggest that the wind mass-loss rate, at least in U Gem, is a substantial fraction of the WD accretion rate. C1 LAWRENCE LIVERMORE NATL LAB,LIVERMORE,CA 94450. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195. AMER ASSOC VARIABLE STAR OBSERVERS,CAMBRIDGE,MA 02138. RP Long, KS (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 70 TC 55 Z9 55 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1996 VL 469 IS 2 BP 841 EP 853 DI 10.1086/177832 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VJ788 UT WOS:A1996VJ78800040 ER PT J AU Magnani, L Hartmann, D Speck, BG AF Magnani, L Hartmann, D Speck, BG TI A catalog of molecular gas at high galactic latitudes SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE catalogs; Galaxy, structure; ISM, clouds; ISM, kinematics and dynamics; ISM, molecules ID INTER-STELLAR CLOUDS; SURFACE MASS DENSITY; X-RAY ENHANCEMENT; H-I CLOUDS; CO SURVEY; MILKY-WAY; DARK CLOUDS; SPECTROSCOPIC ANALYSIS; RADIAL-DISTRIBUTION; STAR FORMATION AB The global distribution and physical properties of the high-latitude molecular clouds are tabulated and discussed. As of this writing, more than 100 objects have been identified at Galactic latitudes \b\ greater than or equal to 25 degrees. Positions are listed for all the known clouds and LSR velocity, angular extent, mass, and internal velocity dispersion are listed when such data are available from the literature. The high-latitude molecular clouds consist primarily of translucent clouds, so that this catalog is the largest, most complete compendium of these objects at high Galactic latitudes. The velocity dispersion of the ensemble of clouds is 5.8 km s(-1) if seven intermediate velocity objects are excluded and 9.9 km s(-1) otherwise. The former dispersion implies a scale height for the clouds of 124 pc and a mean distance of 150 pc; the latter dispersion yields 210 pc and 260 pc, respectively. Thus, the majority of high-latitude clouds are local objects that may be situated at the nearer edges of the Local Bubble. As a group, they are the nearest molecular clouds to the Sun. The average velocity of the ensemble of clouds is -0.3 km s(-1) without the intermediate velocity objects and -2.4 km s(-1) including these clouds. From the catalog of clouds, we determine values for the filling fraction and mass surface density of the high-latitude molecular clouds (and thus of translucent gas) of 0.005 and 0.1-0.2 M. pc(-2), respectively, at \b\ greater than or equal to 25 degrees. Including the lower latitude contribution, we estimate the total local mass surface density of translucent clouds to be 0.2-0.3 M. pc(-2). In the local interstellar medium, these objects represent from 10% to 20% of the molecular gas inventory. Individual clouds range in size from less than 10(-1) to 10(1) pc and in mass from 10(-1) to 10(3) M.. An asymmetry between the northern and southern Galactic hemisphere distribution of the clouds can be interpreted as a displacement of the Sun from the Galactic midplane of 18 pc, a value consistent with determinations based on other tracers. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. BENEDICTINE COLL, ATCHISON, KS 66002 USA. RP Magnani, L (reprint author), UNIV GEORGIA, DEPT PHYS & ASTRON, ATHENS, GA 30602 USA. NR 116 TC 65 Z9 65 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 1996 VL 106 IS 2 BP 447 EP 461 DI 10.1086/192344 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA WE459 UT WOS:A1996WE45900008 ER PT J AU Howarth, RW Billen, G Swaney, D Townsend, A Jaworski, N Lajtha, K Downing, JA Elmgren, R Caraco, N Jordan, T Berendse, F Freney, J Kudeyarov, V Murdoch, P Zhu, ZL AF Howarth, RW Billen, G Swaney, D Townsend, A Jaworski, N Lajtha, K Downing, JA Elmgren, R Caraco, N Jordan, T Berendse, F Freney, J Kudeyarov, V Murdoch, P Zhu, ZL TI Regional nitrogen budgets and riverine N&P fluxes for the drainages to the North Atlantic Ocean: Natural and human influences SO BIOGEOCHEMISTRY LA English DT Article DE anthropogenic; atmospheric deposition; eutrophication; fertilizer; nitrogen; nitrogen budget; nitrogen fixation; N:P ratio; phosphorus; pristine; rivers; temperate; tropical ID NUTRIENT DYNAMICS; PRECIPITATION CHEMISTRY; COASTAL EUTROPHICATION; NITRATE CONCENTRATIONS; INORGANIC NITROGEN; FOREST ECOSYSTEMS; AMAZON BASIN; WEST-AFRICA; ST-LAWRENCE; COSTA-RICA AB We present estimates of total nitrogen and total phosphorus fluxes in rivers to the North Atlantic Ocean from 14 regions in North America, South America, Europe, and Africa which collectively comprise the drainage basins to the North Atlantic. The Amazon basin dominates the overall phosphorus flux and has the highest phosphorus flux per area. The total nitrogen flux from the Amazon is also large, contributing 3.3 Tg yr(-1) out of a total for the entire North Atlantic region of 13.1 Tg yr(-1). On a per area basis, however, the largest nitrogen fluxes are found in the highly disturbed watersheds around the North Sea, in northwestern Europe, and in the northeastern U.S., all of which have riverine nitrogen fluxes greater than 1,000 kg N km(-2) yr(-1). Non-point sources of nitrogen dominate riverine fluxes to the coast in all regions. River fluxes of total nitrogen from the temperate regions of the North Atlantic basin are correlated with population density, as has been observed previously for fluxes of nitrate in the world's major rivers. However, more striking is a strong linear correlation between river fluxes of total nitrogen and the sum of anthropogenically-derived nitrogen inputs to the temperate regions (fertilizer application, human-induced increases in atmospheric deposition of oxidized forms of nitrogen, fixation by leguminous crops, and the import/export of nitrogen in agricultural products). On average, regional nitrogen fluxes in rivers are only 25% of these anthropogenically derived nitrogen inputs. Denitrification in wetlands and aquatic ecosystems is probably the dominant sink, with storage in forests perhaps also of importance. Storage of nitrogen in groundwater, although of importance in some localities, is a very small sink for nitrogen inputs in all regions. Agricultural sources of nitrogen dominate inputs in many regions, particularly the Mississippi basin and the North Sea drainages. Deposition of oxidized nitrogen, primarily of industrial origin, is the major control over river nitrogen export in some regions such as the northeastern U.S. Using data from relatively pristine areas as an index of change, we estimate that riverine nitrogen fluxes in many of the temperate regions have increased from pre-industrial times by 2 to 20 fold, although some regions such as northern Canada are relatively unchanged. Fluxes from the most disturbed region, the North Sea drainages, have increased by 6 to 20 fold. Fluxes from the Amazon basin are also at least 2 to 5 fold greater than estimated fluxes from undisturbed temperate-zone regions, despite low population density and low inputs of anthropogenic nitrogen to the region. This suggests that natural riverine nitrogen fluxes in the tropics may be significantly greater than in the temperate zone. However, deforestation may be contributing to the tropical fluxes. In either case, projected increases in fertilizer use and atmospheric deposition in the coming decades are likely to cause dramatic increases in nitrogen loading to many tropical river systems. C1 FREE UNIV BRUSSELS, GRP MICROBIOL MILIEUX AQUAT, B-1050 BRUSSELS, BELGIUM. US EPA, ENVIRONM RES LAB, NARRAGANSETT, RI 02882 USA. OREGON STATE UNIV, DEPT BOT & PLANT PATHOL, CORVALLIS, OR 97331 USA. IOWA STATE UNIV, AMES, IA 50011 USA. UNIV STOCKHOLM, DEPT SYST ECOL, S-10691 STOCKHOLM, SWEDEN. UNIV STOCKHOLM, CTR MARINE RES, S-10691 STOCKHOLM, SWEDEN. INST ECOSYST STUDIES, MILLBROOK, NY 12545 USA. SMITHSONIAN ENVIRONM RES CTR, EDGEWATER, MD 21037 USA. DLO, CABO, NL-6700 AA WAGENINGEN, NETHERLANDS. CSIRO, DIV PLANT IND, CANBERRA, ACT 2601, AUSTRALIA. INST SOIL SCI & PHOTOSYNTH, PUSHCHINO 142292, RUSSIA. US GEOL SURVEY, DIV WATER RESOURCES, ALBANY, NY 12201 USA. INST SOIL SCI, LAB MAT CYCLING PEDOSPHERE, NANJING, PEOPLES R CHINA. RP Howarth, RW (reprint author), CORNELL UNIV, ITHACA, NY 14853 USA. RI Freney, John/E-9462-2011; Elmgren, Ragnar/A-1854-2013; OI Freney, John/0000-0001-7545-6529; Kudeyarov, Valery/0000-0002-0217-2872 NR 217 TC 931 Z9 996 U1 61 U2 379 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD OCT PY 1996 VL 35 IS 1 BP 75 EP 139 DI 10.1007/BF02179825 PG 65 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA VU200 UT WOS:A1996VU20000004 ER PT J AU Grosholz, ED Ruiz, GM AF Grosholz, ED Ruiz, GM TI Predicting the impact of introduced marine species: Lessons from the multiple invasions of the European green crab Carcinus maenas SO BIOLOGICAL CONSERVATION LA English DT Article DE body size; Carcinus maenas; diet preference; ecological impact; green crabs; habitat usage; invasions; rate of spread ID BOTTOM-UP; WADDEN SEA; TOP-DOWN; CALIFORNIA; DISPERSAL; ORGANISMS; PREDATORS; SHORES; FORCES; ROLES AB We compared ecological characteristics of three spatially independent invasions of the European green crab Carcinus maenas to determine which characteristics were most consistent across invasions, and hence would be most predictable in future invasions. For invasions in western North America (WNA), eastern North America (ENA), and South Africa (SAF), we compared five characteristics: (1) habitat usage, (2) diet preferences, (3) size of individuals, (4) rate of range expansion, and (5) demonstrated and potential impacts. We found that two characteristics, diet preference and ecological impact were relatively similar across the three invasions. Diet preference was particularly consistent with the rank order of taxa being virtually identical at the three sites. In contrast, habitat usage, individual size, and rate of range expansion were more variable. Differences in habitat usage and size were particularly evident in the WNA invasion, where C. maenas have failed to colonize protected and exposed rocky shores used elsewhere and have grown much larger than at other sites. We suggest that the degree of similarity of these characteristics across invasions provides a valuable measure of how predictable they will be in future invasions. Copyright (C) 1996 Elsevier Science Limited C1 UNIV CALIF DAVIS,CTR POPULAT BIOL,DAVIS,CA 95616. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. OI Ruiz, Gregory/0000-0003-2499-441X NR 64 TC 170 Z9 177 U1 6 U2 91 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD OCT-NOV PY 1996 VL 78 IS 1-2 BP 59 EP 66 DI 10.1016/0006-3207(94)00018-2 PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA VP468 UT WOS:A1996VP46800007 ER PT J AU Munson, L Wilhite, A Boltz, VF Wilkinson, JE AF Munson, L Wilhite, A Boltz, VF Wilkinson, JE TI Transforming growth factor beta in bovine placentas SO BIOLOGY OF REPRODUCTION LA English DT Article ID TGF-BETA; LOCALIZATION; ENDOMETRIAL; EXPRESSION; ISOFORMS; RECEPTOR; CELLS; FACTOR-BETA-1; TGF-BETA-1; SEQUENCE AB Transforming growth factor beta s (TGF beta) are a family of multifunctional growth factors that are important embryonic morphogens. Because TGF beta s may regulate the development of epitheliochorial placentas, we investigated the location, expression, secretion, and effects of TGF beta s in bovine placentomes and cell cultures derived from chorionic and endometrial epithelia. Placentomes from early second-trimester pregnancies were examined by immunohistochemistry for TGF beta 1, TGF beta 2, and TGF beta 3, and for TGF beta expression in Northern slot-blots. Effects of TGF beta s were assessed in trophoblastic and endometrial epithelial cell lines by DNA synthesis assays. Secretion of TGF beta s by trophoblastic and endometrial epithelial cells was determined using bioassays. All forms of TGF beta were immunolocalized in bovine placentomes. TGF beta mRNA was expressed in chorioallantois, caruncles, and in cultured trophoblastic and endometrial epithelial cells. Endometrial and trophoblastic cells secreted active and latent TGF beta s, and these cells had a transient proliferative response to all forms of TGF beta. These results indicate that TGF beta are present at the fetal-maternal interface of the bovine placentome and may promote endometrial and chorionic growth. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT PATHOL,WASHINGTON,DC 20008. RP Munson, L (reprint author), UNIV TENNESSEE,COLL VET MED,DEPT PATHOL,KNOXVILLE,TN 37901, USA. NR 39 TC 24 Z9 24 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD OCT PY 1996 VL 55 IS 4 BP 748 EP 755 DI 10.1095/biolreprod55.4.748 PG 8 WC Reproductive Biology SC Reproductive Biology GA VH056 UT WOS:A1996VH05600003 PM 8879485 ER PT J AU Monfort, SL Bush, M Wildt, DE AF Monfort, SL Bush, M Wildt, DE TI Natural and induced ovarian synchrony in golden lion tamarins (Leontopithecus rosalia) SO BIOLOGY OF REPRODUCTION LA English DT Article ID MARMOSET MONKEY CALLITHRIX; URINARY ESTROGEN EXCRETION; SAGUINUS-OEDIPUS-OEDIPUS; SAKI PITHECIA-PITHECIA; COTTON-TOP TAMARIN; CALLIMICO-GOELDII; CYCLE; PREGNANCY; JACCHUS; PROGESTERONE AB Ovarian cycle synchrony was assessed in spontaneously cycling female golden lion tamarins by monitoring longitudinal (16 mo) urinary steroid metabolite (estrone conjugates; pregnanediol-3 alpha-glucuronide, PdG) excretion in four pairs (n = 8) of females isolated from males. The overall mean ovarian cycle duration was 18.5 +/- 0.3 days (n = 136 cycles; mean range, 15.7-21.0 days), and there was no evidence of reproductive seasonality. Laparoscopic ovarian examinations confirmed that cyclic fluctuations in urinary steroid metabolite excretion were temporally associated with the formation and demise of corpora lutea. Evaluation of ovarian synchronization tested the null hypothesis that urinary hormone cycles were expressed randomly relative to those of cagemates or other females housed in separate cages but within close proximity. Natural ovarian synchrony (expressed as the mean difference in ovarian cycle onset) between cagemates (4.1 +/- 0.4 days) and among noncagemates (4.2 +/- 0.2 days) did not differ (p > 0.05) from a random ovarian cycle distribution. Two trials also were conducted to evaluate the efficacy of the prostaglandin (PC) F-2 alpha analogue, cloprostenol, for artificially synchronizing ovarian cycles. Induced ovarian synchrony was not achieved with a single 0.8-mu g i.m. injection of cloprostenol. However, doubling the cloprostenol dose (1.6 mu g) caused a rapid decrease in mean urinary PdG (p < 0.05) within 2 days, and synchronous ovulation was demonstrated by an increase (p < 0.01) in mean urinary PdG 10 days after cloprostenol administration. In summary, females housed in pairs, in the absence of males, exhibit spontaneous, year-round ovarian cycles with no evidence of among-female ovarian synchrony. Results also suggest that this New World primate has a reduced sensitivity to cloprostenol (compared to common marmosets) but that a single, midcycle cloprostenol injection of 1.6 mu g effectively induces luteolysis and synchronous ovulation. RP Monfort, SL (reprint author), NATL ZOOL PK,SMITHSONIAN INST,CONSERVAT & RES CTR,1500 REMOUNT RD,FRONT ROYAL,VA 22630, USA. NR 47 TC 19 Z9 21 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD OCT PY 1996 VL 55 IS 4 BP 875 EP 882 DI 10.1095/biolreprod55.4.875 PG 8 WC Reproductive Biology SC Reproductive Biology GA VH056 UT WOS:A1996VH05600021 PM 8879503 ER PT J AU Boness, DJ Bowen, WD AF Boness, DJ Bowen, WD TI The evolution of maternal care in Pinnipeds SO BIOSCIENCE LA English DT Article ID NORTHERN ELEPHANT SEALS; MASS-TRANSFER EFFICIENCY; CYSTOPHORA-CRISTATA; HARBOR SEAL; HOODED SEAL; HALICHOERUS-GRYPUS; GRAY SEALS; PHOCA-GROENLANDICA; BODY-COMPOSITION; ENERGY-TRANSFER C1 FISHERIES & OCEANS CANADA,BEDFORD INST OCEANOG,MARINE FISH DIV,DARTMOUTH,NS B2Y 4A2,CANADA. RP Boness, DJ (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. RI Bowen, William/D-2758-2012 NR 61 TC 107 Z9 112 U1 5 U2 33 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD OCT PY 1996 VL 46 IS 9 BP 645 EP 654 DI 10.2307/1312894 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VK972 UT WOS:A1996VK97200005 ER PT J AU Jordan, TE Weller, DE AF Jordan, TE Weller, DE TI Human contributions to terrestrial nitrogen flux SO BIOSCIENCE LA English DT Article ID ECOSYSTEMS; FOREST; BUDGET; GROUNDWATER; DEPOSITION; NUTRIENTS; FIXATION; LOSSES; CARBON RP Jordan, TE (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. NR 49 TC 136 Z9 142 U1 3 U2 18 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD OCT PY 1996 VL 46 IS 9 BP 655 EP 664 DI 10.2307/1312895 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VK972 UT WOS:A1996VK97200006 ER PT J AU Faden, RB AF Faden, RB TI New endemic species of Aneilema and Commelina (Commelinaceae) from Somalia SO BRITTONIA LA English DT Article DE Somalia; Commelina; Aneilema; Commelinaceae; endemism AB Three new, endemic species of Commelinaceae from central and southern Somalia are described. Aneilema trispermum is unique in the genus in having capsules with three one-seeded locules. The annual, buff-orange-flowered Commelina arenicola differs from the annual C. subulata Roth and related perennials in having a capsule with an indehiscent dorsal locule. Commelina frutescens has a unique shrubby habit. RP Faden, RB (reprint author), SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT BOT,WASHINGTON,DC 20560, USA. NR 4 TC 1 Z9 2 U1 1 U2 1 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 SN 0007-196X J9 BRITTONIA JI Brittonia PD OCT-DEC PY 1996 VL 48 IS 4 BP 544 EP 550 DI 10.2307/2807874 PG 7 WC Plant Sciences SC Plant Sciences GA WE787 UT WOS:A1996WE78700013 ER PT J AU Ralls, K Eagle, TC Siniff, DB AF Ralls, K Eagle, TC Siniff, DB TI Movement and spatial use patterns of California sea otters SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID ALASKA AB Movement patterns of sea otters (Enhydra lutris) were followed by daily monitoring of 40 individuals with implanted radio transmitters. Otters of all age and sex classes were most often found within 1-2 km of their locations on the previous day. However, individuals often remained within a small area for an extended period and then suddenly moved a much greater distance within a short time period. There were significant differences among age-sex classes, but not months, in the mean monthly distances between successive daily locations and between extreme locations of individual otters. There were significant differences among both age-sex classes and months in the harmonic mean distance deviation. For all three measures, juvenile males tended to move the greatest distances. Adult males tended to be more sedentary than adult females over the short term, but traveled over greater distances in the long term. Individuals within age-sex classes had different movement patterns, and individuals often had different movement patterns during the same month in successive years. Estimates of the area used by individual otters during a single 24-h period (6.9-1166.4 ha) overlapped previous estimates of home-range size based on much longer time periods. C1 UNIV MINNESOTA,DEPT ECOL EVOLUT & BEHAV,ST PAUL,MN 55108. RP Ralls, K (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 21 TC 22 Z9 22 U1 0 U2 7 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD OCT PY 1996 VL 74 IS 10 BP 1841 EP 1849 DI 10.1139/z96-207 PG 9 WC Zoology SC Zoology GA VM955 UT WOS:A1996VM95500009 ER PT J AU Lovelock, CE Kyllo, D Winter, K AF Lovelock, CE Kyllo, D Winter, K TI Growth responses to vesicular-arbuscular mycorrhizae and elevated CO2 in seedlings of a tropical tree, Beilschmiedia pendula SO FUNCTIONAL ECOLOGY LA English DT Article DE elevated CO2; plant-growth analysis; tropical forests; VA-mycorrhizae ID ATMOSPHERIC CO2; PLANTAGO-MAJOR; CARBON; INFECTION; FOREST; ASSOCIATIONS; RESPIRATION; ECOSYSTEMS; DEMAND AB 1. Vesicular-arbuscular (VA) mycorrhizae increased relative growth rates (RGR) of the shade-tolerant tropical tree species Beilschmiedia pendula at both ambient and doubled CO2 concentrations. 2. RGR was correlated with the net assimilation rate (NAR) of plants. Within this general correlation, in plants with similar RGR, NAR was decreased in VA-mycorrhizal plants compared with non-mycorrhizal plants. As RGR is the product of NAR and the leaf area ratio (LAR, the ratio of leaf area to plant mass), increases in RGR in VA-mycorrhizal plants were the results of increased LAR. Thus, VA-mycorrhizae increased growth rates of B. pendula by altering the morphology of the seedlings. 3. Under elevated CO2 the amount of fungus within roots increased in VA-mycorrhizal plants compared with those grown under ambient CO2 and this was associated with a greater post-inoculation depression in leaf growth. Post-inoculation depressions in leaf growth and the lower NAR (in plants with similar RGR) of VA-mycorrhizal plants indicate there is increased carbon transfer to soils under elevated CO2. C1 UNIV MISSOURI,DEPT BIOL,ST LOUIS,MO 63121. RP Lovelock, CE (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 28 TC 32 Z9 33 U1 0 U2 15 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD OCT PY 1996 VL 10 IS 5 BP 662 EP 667 DI 10.2307/2390177 PG 6 WC Ecology SC Environmental Sciences & Ecology GA WC880 UT WOS:A1996WC88000013 ER PT J AU Fagents, SA Wilson, L AF Fagents, SA Wilson, L TI Numerical modeling of ejecta dispersal from transient volcanic explosions on Mars SO ICARUS LA English DT Article ID ICE INTERACTIONS; MARTIAN SURFACE; VENUS; PATERA; ATMOSPHERE; ERUPTIONS; LANDFORMS; GEOLOGY; WATER; TEMPERATURES AB The dynamics of ejecta dispersal in transient volcanic eruptions on Mars are distinct from those on Earth and Venus because of the low atmospheric pressure and gravitational acceleration. Numerical modeling of the physical mechanisms of such activity, accounting for the different martian environmental conditions, can help constrain the style of emplacement of the eruptive products. The scenario envisaged is one of pressurized gas, contributed from either a magmatic or meteoric source, accumulating in the near-surface crust beneath a retaining medium, On failure of the confining material, the gas expands rapidly out of the vent, displacing both the ''caprock'' and a mass of atmospheric gas overlying the explosion site, in a discrete, transient event. Trajectories of large blocks of ejecta are computed subject to the complex aerodynamic interactions of atmospheric and volcanic gases which are set in motion by the initiation of the explosion. Reservoirs of crustal and surface water and carbon dioxide may have increased the chances of occurrence of transient explosive events on Mars in two ways: by supplying a source of volatiles for vaporization by the magma and by acting to slow the ascent of the magma by chilling it, providing conditions favorable for gas accumulation. Results of the modeling indicate that ejection velocities ranging up to similar to 580 m sec(-1) were possible in martian H2O-driven explosions, with CO2-driven velocities typically a factor of similar to 1,5 smaller. Travel distances of large blocks of ejecta lie within the range of a few kilometers to the order of 100 km from the vent, The low martian atmospheric pressure and gravity would thus have conspired to produce more vigorous explosions and more widely dispersed deposits than are associated with analogous events on Earth or Venus. Other phenomena likely to be associated with transient explosions include ashfall deposits from associated convecting clouds of fine material, pyroclastic flows, and ejecta impact crater fields, It is anticipated that the martian environment would have caused such features to be greater in size than would be the case in the terrestrial environment. Ash clouds associated with discrete explosions are expected to have risen to a maximum of similar to 25 km on Mars, producing deposits having similar widths. Another indication of a volcanic explosion site might be found in areas of high regolith ice content, such as fretted terrains, where ice removal and mass-wasting may have modified the vent's initial morphology, The modeling results highlight the implications of the occurrence of transient explosive eruptions for the global crustal volatile distribution and provide some predictions of the likely manifestation of such activity for testing by upcoming spacecraft missions to Mars. (C) 1996 Academic Press, Inc. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560. UNIV LANCASTER,INST ENVIRONM & BIOL SCI,DIV ENVIRONM SCI,LANCASTER LA1 4YQ,ENGLAND. RI Fagents, Sarah/B-3983-2014 NR 93 TC 20 Z9 20 U1 1 U2 2 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD OCT PY 1996 VL 123 IS 2 BP 284 EP 295 DI 10.1006/icar.1996.0158 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VP447 UT WOS:A1996VP44700004 ER PT J AU Kawamura, J Blundell, R Tong, CYE Goltsman, G Gershenzon, E Voronov, B AF Kawamura, J Blundell, R Tong, CYE Goltsman, G Gershenzon, E Voronov, B TI Performance of NbN lattice-cooled hot-electron bolometric mixers SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID RECEIVER AB The heterodyne performance of lattice-cooled hot-electron bolometric mixers is measured at 200 GHz. Superconducting thin-film niobium nitride strips with similar to 5 nm thickness are used as waveguide mixer elements. A double-sideband receiver noise temperature of 750 K at 244 GHz is measured at an intermediate frequency centered at 1.5 GHz with 500 MHz bandwidth and with 4.2 K device temperature. The instantaneous bandwidth for this mixer is 2.6 GHz. The local oscillator power required by the mixer is about 0.5 mu W. The mixer is linear to within 1 dB to an input power level 6 dB below the local oscillator power. A receiver incorporating a hot-electron bolometric mixer was used to detect molecular line emission in a laboratory gascell. This experiment unambiguously confirms that the receiver noise temperature determined from Y-factor measurements reflects the true heterodyne sensitivity. (C) 1996 American Institute of Physics. C1 MOSCOW STATE PEDAG UNIV,MOSCOW 119435,RUSSIA. RP Kawamura, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Tong, Edward/0000-0002-7736-4203 NR 11 TC 11 Z9 11 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD OCT 1 PY 1996 VL 80 IS 7 BP 4232 EP 4234 DI 10.1063/1.363304 PG 3 WC Physics, Applied SC Physics GA VL801 UT WOS:A1996VL80100098 ER PT J AU Kegley, DR Oberacker, VE Strayer, MR Umar, AS Wells, JC AF Kegley, DR Oberacker, VE Strayer, MR Umar, AS Wells, JC TI Basis spline collocation method for solving the Schrodinger equation in axillary symmetric systems SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article ID BOUNDARY-VALUE-PROBLEMS; LATTICE AB We use basis spline collocation to solve the Schrodinger equation on a lattice for axially symmetric systems, with and without spin. The focus of the present work is on systems which have continuum states, weakly bound states, or strong spin-orbit coupling, since these are the most difficult to solve on the lattice. A brief overview of the basis spline collocation method is included which concentrates primarily on those aspects of the theory which are relevant to its application in cylindrical coordinates. To demonstrate the method, we solve several model problems selected from the fields of atomic and nuclear physics. (C) 1996 Academic Press, Inc. C1 VANDERBILT UNIV,DEPT PHYS & ASTRON,NASHVILLE,TN 37235. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Kegley, DR (reprint author), OAK RIDGE NATL LAB,DIV PHYS,CTR COMPUTAT INTENS PHYS,OAK RIDGE,TN 37831, USA. RI Umar, Ahmet/J-4125-2013; Wells, Jack/D-3675-2016 OI Umar, Ahmet/0000-0002-9267-5253; Wells, Jack/0000-0002-5083-3030 NR 25 TC 16 Z9 16 U1 1 U2 6 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD OCT 1 PY 1996 VL 128 IS 1 BP 197 EP 208 DI 10.1006/jcph.1996.0203 PG 12 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA VL091 UT WOS:A1996VL09100013 ER PT J AU Chai, P Dudley, R AF Chai, P Dudley, R TI Limits to flight energetics of hummingbirds hovering in hypodense and hypoxic gas mixtures SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE air density; heliox; helium; hovering flight; hummingbird; Archilochus colubris; hypoxia; muscle power; oxygen consumption ID INSECT FLIGHT; OXYGEN-CONSUMPTION; POWER OUTPUT; AERODYNAMICS; MUSCLE; BIRDS; SELECTION; FUEL AB Hovering hummingbirds offer a model locomotor system for which analyses of both metabolism and flight mechanics are experimentally tractable, Because hummingbirds exhibit the highest mass-specific metabolic rates among vertebrates, maximum performance of hovering flight represents the upper limit of aerobic locomotion in vertebrates, This study evaluates the potential constraints of flight mechanics and oxygen availability on maximum flight performance, Hummingbird flight performance was manipulated non-invasively using air and gas mixtures which influenced metabolism via variable oxygen partial pressure and/or altered flight mechanics via variable air densities, Limits to the locomotor capacity of hovering ruby-throated hummingbirds (Archilochus colubris) were unequivocally indicated by aerodynamic failure in either air/helium or air/heliox mixtures, Air/helium mixtures are hypodense and hypoxic; failure to sustain hovering flight occurred at 63% of the density of sea-level air and at an oxygen concentration of 12%, Air/heliox mixtures are hypodense but normoxic; failure in hovering occurred at 47% of sea-level air density, Thus, hummingbirds demonstrated considerable power reserves in hovering flight as well as hypoxic tolerance, In air/helium mixtures, hovering was limited by oxygen supply and not by flight mechanics, Birds hovering in air/helium mixtures increased their mechanical power output but not their rate of oxygen consumption, By contrast, birds hovering in air/heliox mixtures increased both mechanical performance and metabolic expenditure, Under hypoxia, hovering hummingbirds demonstrated non-negligible, but still limited, capacities for anaerobic metabolism and/or oxygen storage, Depending on the physical context, hummingbird flight performance can therefore be limited by oxygen availability or by flight aerodynamics. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP Chai, P (reprint author), UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712, USA. NR 44 TC 60 Z9 60 U1 1 U2 12 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE, CAMBS, ENGLAND CB4 4DL SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD OCT PY 1996 VL 199 IS 10 BP 2285 EP 2295 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VP246 UT WOS:A1996VP24600016 PM 8896366 ER PT J AU Levinton, J Sturmbauer, C Christy, J AF Levinton, J Sturmbauer, C Christy, J TI Molecular data and biogeography: Resolution of a controversy over evolutionary history of a pan-tropical group of invertebrates SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE biogeography; phylogeny; Ocypodidae; crustacea; evolution; behavior ID FIDDLER-CRABS; VISUAL CONTROL; PACIFIC; CORALS; UCA; COURTSHIP; BEHAVIOR; SEAGRASSES; SYSTEMS AB Phylogenetic analyses of sequences of 16S rDNA suggest that the current hypothesis of the evolution of the pan-tropical fiddler crab genus Uca (Decapoda, Brachyura, Ocypodidae) is false. This hypothesis rests of the assumption that the increase of complexity of reproductive behavior, together with a tendency of a habitat shift towards the higher intertidal, arose only once in the history of the fiddler crabs. The origin of fiddler crabs was placed in the IndoPacific, which is widely thought to be a center of origin for several marine groups. There, relatively lower intertidal crabs were thought to give rise to a radiation in the Americas in which higher intertidal forms with more complex reproductive behavior evolved, and finally, derived crabs were thought to disperse back to the IndoPacific from the Americas, In contrast our phylogeny suggests that the ancestral group, which shows complex reproductive behavior, now resides wholly in the American-Atlantic region, as opposed to the postulated Indo-west-Pacific. Behavioral and ecological complexity must have arisen independently in the American and IndoPacific faunal regions. The pan-tropical subgenus Celuca seems to be polyphyletic, which suggests that the evolution of morphology, ecology and behavior involves convergence in geographically separated locales. This study highlights the dangers of postulating evolution from a center of origin, even if it fits data that can be assigned to an evolutionary trend. C1 UNIV INNSBRUCK, INST ZOOL, A-6020 INNSBRUCK, AUSTRIA. SMITHSONIAN TROP RES INST, MIAMI, FL 34002 USA. RP Levinton, J (reprint author), SUNY STONY BROOK, DEPT ECOL & EVOLUT, STONY BROOK, NY 11794 USA. NR 42 TC 38 Z9 45 U1 2 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD OCT 1 PY 1996 VL 203 IS 1 BP 117 EP 131 DI 10.1016/0022-0981(96)02573-7 PG 15 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA VM828 UT WOS:A1996VM82800010 ER PT J AU Oliver, WL Glotfelty, K AF Oliver, WL Glotfelty, K TI O+-O collision cross section and long-term F region O density variations deduced from the ionospheric energy budget SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LOWER THERMOSPHERIC STRUCTURE; SCATTER RADAR MEASUREMENTS; MILLSTONE HILL; AERONOMICAL MEASUREMENTS; TEMPERATURE; FREQUENCY; ARECIBO AB Recent estimates of the O+-O collision cross section Q(O+-O) have suggested that the commonly used value of Banks [1966b] is too low by a factor of 1.2-1.9. On the other hand, past deductions of the F region neutral atomic oxygen density [O] from incoherent scatter (IS) radar studies have been quite compatible with the original Banks value, and any serious adjustment of that value would cause serious disagreement between these radar [O] results and those of the mass spectrometer incoherent scatter (MSIS) model. We have derived the mean daytime value for the product of Q(O+-O) and [O] for 153 days during the period 1970-1975 from Millstone Hill IS radar measurements of ionospheric temperature and density. If we assume that MSIS model [O] is correct on average over this period, we find that Q(O+-O) is only 75% of the Banks value and 40 to 60% lower than other values recently proposed. We show that all previous derivations of [O] from IS radar energy-budget studies are compatible with our value, and thus a discrepancy exists in Q(O+-O) determination by different methods. We could make our Q(O+-O) results compatible with the larger values noted above by allowing a neutral temperature gradient to exist at high altitudes, where none is currently expected, or by increasing the heat input to the ion gas. We note that both of these effects could be produced by a sufficient reservoir of hot oxygen in the topside of the ionosphere. Independent of the way in which we choose a value of Q(O+-O) to make the radar and MSIS [O] values agree on average over our 6-year span of data, the radar record shows [O] to have episodic departures from MSIS predictions reaching amplitudes of up to 50% and lasting for periods of several months. This argues for caution in analyses which depend crucially upon the validity of MSIS densities during campaign-like experimental studies. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA. BOSTON UNIV,DEPT ELECT COMP & SYST ENGN,BOSTON,MA 02215. BOSTON UNIV,CTR SPACE PHYS,BOSTON,MA 02215. RP Oliver, WL (reprint author), NATL CTR ATMOSPHER RES,HIGH ALTITUDE OBSERV,POB 3000,BOULDER,CO 80307, USA. NR 29 TC 27 Z9 27 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES JI J. Geophys. Res-Space Phys. PD OCT 1 PY 1996 VL 101 IS A10 BP 21769 EP 21784 DI 10.1029/96JA01585 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VK704 UT WOS:A1996VK70400026 ER PT J AU Jakab, PL AF Jakab, PL TI A passion for wings: Aviation and the Western imagination, 1908-1918 - Wohl,R SO JOURNAL OF MILITARY HISTORY LA English DT Book Review RP Jakab, PL (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU VIRGINIA MILITARY INST PI LEXINGTON PA LEXINGTON, VA 24450 SN 0899-3718 J9 J MILITARY HIST JI J. Mil. Hist. PD OCT PY 1996 VL 60 IS 4 BP 779 EP 780 DI 10.2307/2944675 PG 2 WC History SC History GA VM298 UT WOS:A1996VM29800018 ER PT J AU Pelaez, J Lorenzini, EC AF Pelaez, J Lorenzini, EC TI Sensitivity analysis of tether-mediated orbital injection SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article AB This paper investigates the injection of a satellite from lower to higher orbit by means of the tether sling-shot technique. This technique utilizes the increment of velocity (Delta upsilon) imparted by a long librating tether, attached to a suitable orbiting platform (e.g., the Space Shuttle), for changing the satellite's orbit. With a scheme that miners a two-impulse orbital transfer, the tether is cut twice: the first time on the platform side when the tether crosses the local vertical after deployment and the second time on the satellite side at a convenient apogee passage. The two cuts increase the apogee and the perigee heights, respectively. Issues addressed in this paper, which are essential for an accurate and effective orbital injection, are the maximization of the first by and its sensitivity to uncertainties associated with tether unmotorized deployers (e.g., the Small Expendable Deployment System). The initial conditions that minimize the sensitivity to variations of the deployer's model parameters and the optimal timing of the second cut are evaluated. Although the sling-shot technique is of general use for orbital transfer of tethered satellites, a specific numerical case is made for the injection of the SEDSAT satellite in order to prove that the orbital altitude after injection can be maximized and made insensitive to unpredictable variations of the deployer's tension model. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Pelaez, J (reprint author), UNIV POLITECN MADRID,ETSI AERONAUT,MADRID,SPAIN. RI Pelaez, Jesus/M-7806-2016 OI Pelaez, Jesus/0000-0001-9755-1674 NR 15 TC 15 Z9 15 U1 0 U2 1 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 SN 0021-9142 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD OCT-DEC PY 1996 VL 44 IS 4 BP 491 EP 514 PG 24 WC Engineering, Aerospace SC Engineering GA XF358 UT WOS:A1996XF35800004 ER PT J AU Eberhard, WG Pereira, F AF Eberhard, WG Pereira, F TI Functional morphology of male genitalic surstyli in the dungflies Achisepsis diversiformis and A-ecalcarata (Diptera: Sepsidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article ID SEXUAL SELECTION; EVOLUTIONARY; CONFLICT; SYSTEM AB During copulation the species-specific male genitalic surstyli of Achisepsis diversiformis and A. ecalcarata grasp the female's abdomen near her 6th abdominal sternite. Variation in the sites grasped by the male and the lack of female structures that limit male access rule out several versions of both mechanical and sensory ''lock and key'' explanations for the differences in male morphology. Alternative hypotheses for surstylus function are discussed; a combination of physical restraint and stimulation of the female seems most likely. C1 UNIV COSTA RICA,ESCUELA BIOL,SAN JOSE,COSTA RICA. RP Eberhard, WG (reprint author), UNIV COSTA RICA,SMITHSONIAN TROP RES INST,CIUDAD UNIV,SAN JOSE,COSTA RICA. NR 29 TC 28 Z9 28 U1 0 U2 5 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD OCT PY 1996 VL 69 IS 4 SU S BP 43 EP 60 PG 18 WC Entomology SC Entomology GA WJ925 UT WOS:A1996WJ92500004 ER PT J AU Cocroft, RB Pogue, M AF Cocroft, RB Pogue, M TI Social behavior and communication in the neotropical cicada Fidicina mannifera (Fabricius) (Homoptera: Cicadidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article ID DICEROPROCTA-APACHE HOMOPTERA; CYSTOSOMA-SAUNDERSII; SOUND-PRODUCTION; BLADDER CICADA; DESERT CICADA; ADVERTISEMENT; TEMPERATURE; COURTSHIP; RESPONSES; FLIGHT AB We investigated signalling behavior in relation to social context in the cicada Fidicina mannifera. Four types of acoustic signals were recorded from males: songs, calls, low-amplitude songs, and disturbance sounds. Signal types were similar in frequency and fine temporal structure, but differed markedly in gross temporal structure. Songs and calls were the most frequently observed signals, and these differed in the social context in which they were used. When inter-male distances were large, males produced songs, overlapping them with songs of neighboring males. As nearest-neighbor distance decreased, males switched to calls, which were typically alternated back and forth between males. Bouts of calls often were followed by a parallel walk display, which apparently was involved in settling disputes over calling sites. C1 UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712. SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ENTOMOL,WASHINGTON,DC 20560. NR 51 TC 8 Z9 8 U1 1 U2 9 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD OCT PY 1996 VL 69 IS 4 SU S BP 85 EP 97 PG 13 WC Entomology SC Entomology GA WJ925 UT WOS:A1996WJ92500008 ER PT J AU Wcislo, WT Engel, MS AF Wcislo, WT Engel, MS TI Social behavior and nest architecture of nomiine bees (Hymenoptera: Halictidae; Nomiinae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article AB To facilitate future comparative studies among halictid bees, we review social behavior and nest architecture for 21 species of Nomiinae (Halictidae). Nothing is known of the biology of the vast majority of named species. Approximately half of the species consist of solitary bees, and half consist of females which live within social groups. Social organization varies among species, but there is insufficient information to assess whether it also varies within species. All nomiines nest in the ground, and nest architecture is variable within the subfamily. Architectural characters may provide some useful information for taxonomic and systematic purposes. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. CORNELL UNIV, DEPT ENTOMOL, ITHACA, NY 14853 USA. RI Engel, Michael/C-5461-2012 OI Engel, Michael/0000-0003-3067-077X NR 50 TC 5 Z9 5 U1 1 U2 7 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD OCT PY 1996 VL 69 IS 4 SU S BP 158 EP 167 PG 10 WC Entomology SC Entomology GA WJ925 UT WOS:A1996WJ92500013 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI High art down home: An economic ethnography of a local art market - Plattner,S SO LIBRARY JOURNAL LA English DT Book Review RP Kalfatovic, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 1 PY 1996 VL 121 IS 16 BP 74 EP 74 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VL060 UT WOS:A1996VL06000039 ER PT J AU Lessios, HA Pearse, JS AF Lessios, HA Pearse, JS TI Hybridization and introgression between Indo-Pacific species of Diadema SO MARINE BIOLOGY LA English DT Article ID MOSAIC HYBRID ZONE; LINKAGE DISEQUILIBRIUM; NATURAL-POPULATIONS; REPRODUCTIVE ISOLATION; DROSOPHILA; MITOCHONDRIAL; GENETICS; CRICKETS; OVERLAP; LOCI AB We present the first case of hybridization between echinoid species evaluated through genetic markers and morphology. We examined the three tropical Tndo-Pacific species of the genus Diadema: D. paucispinum A. Agassiz, D. savignyi (Audouin) Michelin and D. setosusum (Leske). Specimens morphologically intermediate between two of these species, D. savignyi and D. setosum have previously been noted. Fertile hybrids have also been produced in the laboratory. To determine extent of hybridization, we first assayed the allozyme products of 22 loci in individuals which, on the basis of morphology and collection locality, could be unambiguously assigned to one of the three species. We found four loci that were either diagnostic or semi-diagnostic between D. setosum and the other two species, and one locus semi-diagnostic between D. savignyi and D. paucispinum. We then assayed individuals of intermediate morphology to find out whether they had hybrid genotypes. In the Ryukyu islands? where D. setosum and D. savignyi coexist, we found one specimen which on the basis of all four diagnostic loci was an F-1 hybrid, and several individuals that could be either F-2 (or later-generation) hybrids or progeny of backcrosses. We also found one individual that on both genetic and morphological grounds appeared to belong to D. paucispinum (even though this species has only been reported from Hawaii and Kiribati) and three other individuals that carried alleles characteristic of D. paucispinum. Thus, previous reports of hybridization between D. setosum and D. savignyi were correct; it is also possible that larvae of D. paucispinum occasionally arrive at localities outside Hawaii, reach sexual maturity, and hybridize with the other two species. Counts of pure and hybrid morphotypes in other populations across the western tropical Pacific revealed a low but widespread incidence of apparent F-1 hybrids and backcrosses of D. savignyi and D. setosum. However, the existence of diagnostic or semi-diagnostic loci, low interspecific gene-flow estimates based on F-ST statistics, and the lack of Hardy-Weinberg or linkage disequilibria among individuals of pure morphology all suggest that gene introgression between the three species is limited. C1 UNIV CALIF SANTA CRUZ,INST MARINE SCI,SANTA CRUZ,CA 95064. RP Lessios, HA (reprint author), SMITHSONIAN TROP RES INST,BOX 2072,BALBOA,PANAMA. NR 58 TC 35 Z9 37 U1 0 U2 3 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD OCT PY 1996 VL 126 IS 4 BP 715 EP 723 DI 10.1007/BF00351338 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA VR103 UT WOS:A1996VR10300016 ER PT J AU Glenn, TC Stephan, W Dessauer, HC Braun, MJ AF Glenn, TC Stephan, W Dessauer, HC Braun, MJ TI Allelic diversity in alligator microsatellite loci is negatively correlated with GC content of flanking sequences and evolutionary conservation of PCR amplifiability SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Letter DE Alligator mississippiensis; Crocodilia; GC content; interspecific priming; polymorphisms; microsatellites; SSR; STR ID DNA MISMATCH REPAIR; RICH ISOCHORES C1 UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742. LOUISIANA STATE UNIV,DEPT BIOCHEM,BATON ROUGE,LA 70803. RP Glenn, TC (reprint author), SMITHSONIAN INST,LAB MOL SYSTEMAT,MRC 534,WASHINGTON,DC 20560, USA. RI Glenn, Travis/A-2390-2008 NR 22 TC 55 Z9 59 U1 1 U2 3 PU SOC MOLECULAR BIOLOGY EVOLUTION PI LAWRENCE PA PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD OCT PY 1996 VL 13 IS 8 BP 1151 EP 1154 PG 4 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA VN652 UT WOS:A1996VN65200011 PM 8865669 ER PT J AU Wen, J Zimmer, EA AF Wen, J Zimmer, EA TI Phylogeny and biogeography of Panax L (the ginseng genus, Araliaceae): Inferences from ITS sequences of nuclear ribosomal DNA SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID TRANSCRIBED SPACER SEQUENCES; NORTH-AMERICAN; NUCLEOTIDE-SEQUENCES; TRIFOLIUM ARALIACEAE; EVOLUTIONARY RATES; DWARF GINSENG; REGIONS; GENDER; DIVERGENCE; ASTERACEAE AB Panax the ginseng genus, is one of the most medicinally important genera in the Orient and demonstrates a classical eastern Asian and eastern North American disjunct distributional pattern. Sequences of the internal transcribed spacers (ITS) and the 5.8S coding region of the nuclear ribosomal DNA repeat were obtained for the 12 species of Panax to reconstruct phylogenetic relationships. Of the 2 eastern North American species, P. quinquefolius and P. trifolius, P. quinquefolius was suggested to be more closely related to the eastern Asian species in the ITS tree, while P. trifolius was phylogenetically isolated. Monophyly of the three medicinally most important species, P. ginseng, P. notoginseng, and P. quinquefolius, suggested by previous workers, was not supported by the ITS data. A close phylogenetic relationship between Panax: and Aralia was supported. Several biogeographical implications were inferred: (1) two divergence events have produced the eastern Asian and eastern North American disjunct distribution in Panax (2) no intercontinental species pairs are found in Panax; (3) a discrepancy between the sequence divergence pattern and the phylogenetic pattern was observed in Panax, suggesting the need for caution in using sequence divergence data alone in inferring biogeographical patterns; (4) the Himalayas and central and western China are the current centers of diversity of the ginseng genus; and (5) the low ITS sequence divergence and a close relationship among species in that region suggest that rapid evolutionary radiation may have created such a diversity of Panax in the Himalayas and in central and western China. (C) 1996 Academic Press, Inc. C1 SMITHSONIAN INST, NATL MUSEUM NAT HIST, LAB MOL SYSTEMAT, WASHINGTON, DC 20560 USA. SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT BOT, WASHINGTON, DC 20560 USA. RI Zimmer, Elizabeth/G-3890-2011 NR 71 TC 248 Z9 278 U1 7 U2 39 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 1996 VL 6 IS 2 BP 167 EP 177 DI 10.1006/mpev.1996.0069 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA VM611 UT WOS:A1996VM61100001 PM 8899721 ER PT J AU Mariaux, J Braun, MJ AF Mariaux, J Braun, MJ TI A molecular phylogenetic survey of the nightjars and allies (Caprimulgiformes) with special emphasis on the potoos (Nyctibiidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID MITOCHONDRIAL CYTOCHROME-B; DNA-SEQUENCES; CLASS AVES; EVOLUTION; GENE; PROTEIN; CLASSIFICATION; VERTEBRATES; UTILITY; REGIONS AB A 656-pb fragment of the mitochondrial cytochrome b gene was sequenced for six species of Central and South American potoos (genus Nyctibius, Nyctibiidae) as well as for selected representatives of all other caprimulgiform families. Sequence divergence among potoos was much higher (11.1-16.2%) than has typically been observed among congeneric species of birds, suggesting that the species of Nyctibius are quite old. Divergence among families was also quite high (13.7-21.8%), confirming recent DNA-DNA hybridization studies. Such high genetic divergences in a functionally constrained gene like cyt b indicate that many of those sites which are free to vary will have experienced multiple substitutions. We therefore performed phylogenetic analysis using parsimony under a variety of weighting schemes intended to reduce the effect of multiple substitutions. The monophyly of all the traditional caprimulgiform families was confirmed and a number of new hypotheses of relationship emerged. From our analysis, it appears that the oilbird (Steatornis) is an ancient member of the order, and it is not closely related to the potoos. We also note the close link between Aegothelidae and Caprimulgidae, and the basal position of the Podargidae/Batrachostomidae clade in the phylogeny. These results are in accordance with several classical works of the first half of the century. The relationships of the various Nyctibius species to each other have not been fully resolved; however, a close link between N. leucopterus and N. maculosus appears to be highly probable from our data. (C) 1996 Academic Press, Inc. C1 SMITHSONIAN INST,LAB MOL SYSTEMAT,WASHINGTON,DC 20560. RI Mariaux, Jean/A-1142-2010 OI Mariaux, Jean/0000-0002-9601-855X NR 58 TC 37 Z9 40 U1 0 U2 2 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 1996 VL 6 IS 2 BP 228 EP 244 DI 10.1006/mpev.1996.0073 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA VM611 UT WOS:A1996VM61100005 PM 8899725 ER PT J AU Capson, TL Coley, PD Kursar, TA AF Capson, TL Coley, PD Kursar, TA TI A new paradigm for drug discovery in tropical rainforests SO NATURE BIOTECHNOLOGY LA English DT Editorial Material ID BRINE SHRIMP; PLANTS C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP Capson, TL (reprint author), UNIV UTAH,DEPT BIOL,SALT LAKE CITY,UT 84112, USA. NR 10 TC 7 Z9 7 U1 1 U2 2 PU NATURE PUBLISHING CO PI NEW YORK PA 345 PARK AVE SOUTH, NEW YORK, NY 10010-1707 SN 1087-0156 J9 NAT BIOTECHNOL JI Nat. Biotechnol. PD OCT PY 1996 VL 14 IS 10 BP 1200 EP & DI 10.1038/nbt1096-1200 PG 2 WC Biotechnology & Applied Microbiology SC Biotechnology & Applied Microbiology GA VK618 UT WOS:A1996VK61800002 PM 9631071 ER PT J AU Robertson, DR AF Robertson, DR TI Egg size in relation to fertilization dynamics in free-spawning tropical reef fishes SO OECOLOGIA LA English DT Article DE fish; egg size; fertilization dynamics; sperm competition, limitation, and economy ID MALE MATING SUCCESS; THALASSOMA-BIFASCIATUM; SPERM LIMITATION; SEA-URCHIN; INVERTEBRATES; SYSTEM; ALLOCATION; STRATEGIES; EVOLUTION; BUOYANCY AB In marine invertebrates that spawn by simply releasing their gametes into the water (free-spawning), fertilization success likely is often limited by low sperm concentrations, due to dispersion of mates and dispersal of gametes by water movements. Production of large, low density eggs might be advantageous when sperm concentrations consistently are low, because large target size might increase egg/sperm encounters, and more low than high density eggs could be produced per clutch. Although average fertilization success in the labrid Thalassoma bifasciatum is similar to 95% in both group spawns (in which multiple males compete for fertilizations by producing large quantities of sperm) and pair (mono-male) spawns, it is slightly lower in pair spawns, due to low level sperm limitation that arises because pair-spawning males release near the minimum number of sperm necessary for maximum fertilization. I examined whether variation in egg size and content in T. bifasciatum and other free-spawning fishes is related to variation in spawning mode, to assess whether compensatory production of large, low-density eggs might be contributing to high fertilization success in pair spawns. I found no difference between the volume or density of eggs of (1) pair- and group-spawning females of T. bifasciatum, or (2) pair- and group-spawning congeneric species of labrids, scarids, and serranids, or (3) labrids and scarids with vigorous, rapid spawning movements (which could turbulently diffuse gamete clouds) and those with slow movements. Further, egg density does not decline with increasing egg volume among those fishes. Assuming that egg size can affect fertilization success, then sperm limitation seems unlikely to represent a significant problem for pair-spawning T. bifasciatum, probably because mates place their vents close together during gamete release. The situation regarding sperm limitation in other fishes, and effects of environmentally generated water turbulence on it, are less clear. Interspecific variation in the size and content of these fishes' eggs may relate to provisioning of offspring for different larval life-histories. RP Robertson, DR (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO,AA 34002, USA. NR 58 TC 13 Z9 13 U1 0 U2 6 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD OCT PY 1996 VL 108 IS 1 BP 95 EP 104 DI 10.1007/BF00333220 PG 10 WC Ecology SC Environmental Sciences & Ecology GA VL383 UT WOS:A1996VL38300013 PM 28307739 ER PT J AU DiMichele, WA Pfefferkorn, H Phillips, TL AF DiMichele, WA Pfefferkorn, H Phillips, TL TI Persistence of Late Carboniferous tropical vegetation during glacially driven climatic and sea-level fluctuations SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Review ID COAL-SWAMP VEGETATION; NORTH-AMERICA; DEPOSITIONAL MODELS; ILLINOIS BASIN; SHALE FACIES; PATTERNS; EURAMERICA; PALEOBOTANY; EVOLUTION; ORIGIN AB The Late Carboniferous glaciation reached its peak during the latter part of the Westphalian (late Desmoinesian). In the tropical Illinois basin this was the time of deposition of the Carbondale and lower Modesto Formations, characterized by the cyclic repetition of major coal deposits, black shales, limestones, gray shales and sandstones. These lithological changes evidence repeated major fluctuations in climate and sealevel. Fossil floras from the tropical ever-wet to seasonally wet terrestrial lithofacies, coals and shales above coals, remain compositionally similar throughout the 1-1.5 m.y. time interval. Floras from coals, known from coal balls and palynology, characteristically were composed of three major plant communities: the wettest sites were dominated by monocarpic lycopsids, intermediate sites were dominated by polycarpic lycopsids, and areas subject to fires and intermittent flooding were dominated by medullosans and the small lycopsid Paralycopodites. Clastic-substrate environments were dominated by ferns and pteridosperms and conform to a single biozone, indicating their compositional unity and distinctness from earlier and later assemblages. The composition of lowland floras is poorly known from times between the deposition of coals and associated terrestrial rocks, intervals during which most of the lowlands were flooded and marine rocks were being deposited. Consequently, the temporally intermittent recurrence of lowland floras despite repeated, widespread environmental disruption may be explained either by vegetational persistence and migration of floras, or repeated disruption and reassembly. Several lines of evidence suggest persistence as a likely explanation. C1 UNIV PENN,DEPT GEOL,PHILADELPHIA,PA 19104. UNIV ILLINOIS,DEPT PLANT BIOL,URBANA,IL 61801. RP DiMichele, WA (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. RI DiMichele, William/K-4301-2012 NR 105 TC 48 Z9 49 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD OCT PY 1996 VL 125 IS 1-4 BP 105 EP 128 DI 10.1016/S0031-0182(96)00026-0 PG 24 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA VZ399 UT WOS:A1996VZ39900006 ER PT J AU Aslan, A Behrensmeyer, AK AF Aslan, A Behrensmeyer, AK TI Taphonomy and time resolution of bone assemblages in a contemporary fluvial system: The East Fork River, Wyoming SO PALAIOS LA English DT Article ID DINOSAUR-PROVINCIAL-PARK; BEDLOAD MEASUREMENTS; QUANTITATIVE MODEL; PALEOSOLS; MONTANA; ALBERTA; SUITES; CANADA AB Experiments that recorded the dispersal of 142 bones within a meandering, 2030 m-long reach of the East Fork River, Wyoming over a 13-year period provide a basis for interpreting distribution patterns and time averaging in. fossiliferous channel deposits. Results show that light and porous bones, (e.g., vertebrae, patellae, and phalanges) were transported farther than heavy bones (e.g., limb bones and mandibles). Dispersal patterns of bones from individual experimental sets representing point sources demonstrate that bones became sorted by size and shape within 1 to 2 years and that sorting patterns varied according to initial channel position. The combined distribution of bones from all the experimental sets, however was unsorted and generally random, suggesting that unsorted fluvial bone assemblages reflect multiple bone sources and differences in the time at which bones enter the channel. Estimates of time-averaging of potential and observed natural bone assemblages in. the East Fork River and the South Platte River range from 10(1)-10(4) years. The upper Limit for this estimate is controlled by both the age of fossiliferous floodplain deposits that border the rivers and by the ability of the rivers to rework these floodplain. deposits. The lower limit reflects either the scarcity of bones in the floodplain sediments or the inability of the rivers to rework these older bones; in this case channel bone assemblages should represent only remains from deaths in the channel or remains that were transported into the channel from adjoining land surfaces, resulting in. short intervals of time-averaging (10(1)-10(2) years). The East Fork study further suggests that sandstone geometry, paleosol development, and the sedimentary context of fossil occurrences cart be used to evaluate time-averaging in ancient fossiliferous channel deposits. Fossil bone assemblages that are present exclusively in ribbon-shaped channel deposits associated with weakly developed paleosols and unfossiliferous floodplain deposits should represent shorter time intervals than similar fossil assemblages associated with Sheet sandstones and moderately developed paleosols with abundant fossils. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560. NR 43 TC 47 Z9 47 U1 2 U2 8 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 1731 E 71ST STREET, TULSA, OK 74136-5108 SN 0883-1351 J9 PALAIOS JI Palaios PD OCT PY 1996 VL 11 IS 5 BP 411 EP 421 DI 10.2307/3515209 PG 11 WC Geology; Paleontology SC Geology; Paleontology GA VQ020 UT WOS:A1996VQ02000002 ER PT J AU Culver, SJ Woo, HJ Oertel, GF Buzas, MA AF Culver, SJ Woo, HJ Oertel, GF Buzas, MA TI Foraminifera of coastal depositional environments, Virginia, USA: Distribution and taphonomy SO PALAIOS LA English DT Article ID SOUTHERN DELMARVA-PENINSULA AB The coastal zone of the southern Delmarva Peninsula exhibits a wide variety of barrier island system subenvironments. This study investigated, a) whether 20 a priori subenvironments could be distinguished from each other on the basis of total (living plus dead) foraminiferal assemblages, and b) the potential utility of modern, foraminiferal assemblages as paleoenvironmental indicators in barrier island systems. Sixty-eight foraminiferal species were recorded from 57 surface sediment samples. The values of species diversity (H(S)) and equitability (E) exhibit a striking contrast between. the marshes and other areas. The marshes had higher values of species diversity and equitability than the tidal flats and the channels-inlets-shoreface. Stepwise regression analyses indicate correlation of the seven most frequently occurring species in total assemblages (>30% of the total stations) with combinations of one to three environmental variables at the 95% level. Species diversity data and taxonomic composition data analysed by canonical variate analysis indicate that not 20, but four major environments can be readily and reliably distinguished, namely brackish marsh/channel, Lagoonal tidal flats, lagoonal marshes/washover fans, and channels/inlets/shoreface. Combined sedimentologic and microfaunal data can provide greater environmental discrimination. Although these modern foraminiferal distribution patterns are useful as a model for paleoenvironmental interpretations of Quaternary coastal deposits, the model should be applied with great caution. because the nature of fossil assemblages in short cores taken in outer fringe marsh and tidal flat environments indicates that taphonomic loss of foraminiferal tests is both considerable and variable. C1 KORDI ANSAN,MARINE GEOL RES GRP,SEOUL 425600,SOUTH KOREA. OLD DOMINION UNIV,DEPT OCEANOG,NORFOLK,VA 23529. SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT PALEOBIOL,WASHINGTON,DC 20560. RP Culver, SJ (reprint author), BRITISH MUSEUM NAT HIST,DEPT PALAEONTOL,CROMWELL RD,LONDON SW7 5BD,ENGLAND. NR 68 TC 35 Z9 36 U1 0 U2 1 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 1731 E 71ST STREET, TULSA, OK 74136-5108 SN 0883-1351 J9 PALAIOS JI Palaios PD OCT PY 1996 VL 11 IS 5 BP 459 EP 486 DI 10.2307/3515213 PG 28 WC Geology; Paleontology SC Geology; Paleontology GA VQ020 UT WOS:A1996VQ02000006 ER PT J AU Langley, HD AF Langley, HD TI A quest for glory: A biography of Rear Admiral John A. Dahlgren - Schneller,R SO PENNSYLVANIA MAGAZINE OF HISTORY AND BIOGRAPHY LA English DT Book Review RP Langley, HD (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU HISTORICAL SOC PA PI PHILADELPHIA PA 1300 LOCUST ST, PHILADELPHIA, PA 19107 SN 0031-4587 J9 PENN MAG HIST BIOG JI Pa. Mag. Hist. Biogr. PD OCT PY 1996 VL 120 IS 4 BP 391 EP 392 PG 2 WC History SC History GA VP583 UT WOS:A1996VP58300016 ER PT J AU Ward, DC AF Ward, DC TI Maverick's progress: An autobiography - Flexner,JT SO PENNSYLVANIA MAGAZINE OF HISTORY AND BIOGRAPHY LA English DT Book Review RP Ward, DC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU HISTORICAL SOC PA PI PHILADELPHIA PA 1300 LOCUST ST, PHILADELPHIA, PA 19107 SN 0031-4587 J9 PENN MAG HIST BIOG JI Pa. Mag. Hist. Biogr. PD OCT PY 1996 VL 120 IS 4 BP 404 EP 405 PG 2 WC History SC History GA VP583 UT WOS:A1996VP58300025 ER PT J AU Yan, ZC Babb, JF Dalgarno, A Drake, GWF AF Yan, ZC Babb, JF Dalgarno, A Drake, GWF TI Variational calculations of dispersion coefficients for interactions among H, He, and Li atoms SO PHYSICAL REVIEW A LA English DT Article ID LITHIUM ISOELECTRONIC SEQUENCE; DER-WAALS COEFFICIENTS; DYNAMIC POLARIZABILITIES; DIPOLE POLARIZABILITIES; MULTIPOLE POLARIZABILITIES; VANDERWAALS COEFFICIENTS; ABINITIO CALCULATIONS; RYDBERG STATES; GROUND-STATES; ALKALI ATOMS AB The dispersion coefficients C-6, C-8, and C-10 for the interactions among H, He, and Li are calculated using variational wave functions in Hylleraas basis sets with multiple exponential scale factors, With these highly correlated wave functions, significant improvements are made upon previous calculations and our results provide definitive values for these coefficients. C1 UNIV WINDSOR,DEPT PHYS,WINDSOR,ON N9B 3P4,CANADA. RP Yan, ZC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Yan, Zong-Chao/F-6668-2014; OI Babb, James/0000-0002-3883-9501 NR 45 TC 221 Z9 221 U1 2 U2 18 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD OCT PY 1996 VL 54 IS 4 BP 2824 EP 2833 DI 10.1103/PhysRevA.54.2824 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA VM255 UT WOS:A1996VM25500044 ER PT J AU Epstein, ME AF Epstein, ME TI A new species and generic placement for the misidentified type species of Epiclea Dyar, 1905 (Lepidoptera: Limacodidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Epiclea; Euprosterna; Monoleuca; Limacodidae; type species; Mexico; mislabelled type AB A Mexican species of Limacodidae has remained undescribed, hidden under the name Epiclea elaea (Druce) 1887 because of an improper type label on a specimen now in the collection of The Natural History Museum, London. The species is described as Monoleuca longifascia, new species, and is placed in Monoleuca based on a number of putative synapomorphies with the type species Monoleuca semifascia Walker. RP Epstein, ME (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,NHB 105,WASHINGTON,DC 20560, USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 1996 VL 98 IS 4 BP 812 EP 817 PG 6 WC Entomology SC Entomology GA VT191 UT WOS:A1996VT19100016 ER PT J AU Sturmbauer, C Levinton, JS Christy, J AF Sturmbauer, C Levinton, JS Christy, J TI Molecular phylogeny analysis of fiddler crabs: Test of the hypothesis of increasing behavioral complexity in evolution SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID VISUAL CONTROL; UCA; COURTSHIP; DISPERSAL; SYSTEMS; PANAMA AB The current phylogenetic hypothesis for the evolution and biogeography of fiddler crabs relies on the assumption that complex behavioral traits are assumed to also be evolutionary derived, Indo-west Pacific fiddler crabs have simpler reproductive social behavior and are more marine and were thought to be ancestral to the more behaviorally complex and more terrestrial American species, It was also hypothesized that the evolution of more complex social and reproductive behavior was associated with the colonization of the higher intertidal zones, Our phylogenetic analysis, based upon a set of independent molecular characters, however, demonstrates how widely entrenched ideas about evolution and biogeography led to a reasonable, but apparently incorrect, conclusion about the evolutionary trends within this pantropical group of crustaceans, Species bearing the set of ''derived traits'' are phylogenetically ancestral, suggesting an alternative evolutionary scenario: the evolution of reproductive behavioral complexity in fiddler crabs may have arisen multiple times during their evolution, The evolution of behavioral complexity may have arisen by coopting of a series of other adaptations for high intertidal living and antipredator escape. A calibration of rates of molecular evolution from populations on either side of the Isthmus of Panama suggest a sequence divergence rate for 16S rRNA of 0.9% per million years, The divergence between the ancestral clade and derived forms is estimated to be approximate to 22 million years ago, whereas the divergence between the American and Indo-west Pacific is estimated to be approximate to 17 million years ago. C1 SUNY STONY BROOK, DEPT ECOL & EVOLUT, STONY BROOK, NY 11794 USA. SMITHSONIAN TROP RES INST, MIAMI, FL 34002 USA. RP Sturmbauer, C (reprint author), UNIV INNSBRUCK, INST ZOOL, A-6020 INNSBRUCK, AUSTRIA. NR 30 TC 110 Z9 117 U1 0 U2 7 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD OCT 1 PY 1996 VL 93 IS 20 BP 10855 EP 10857 DI 10.1073/pnas.93.20.10855 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VL333 UT WOS:A1996VL33300061 PM 11607711 ER PT J AU Eikenberry, SS Fazio, GG Ransom, SM AF Eikenberry, SS Fazio, GG Ransom, SM TI An SSPM-based high-speed near-infrared photometer for astronomy SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ARRAYS AB We describe the design, operation, and performance of a new high-speed infrared photometer using the Solid-State Photomultiplier (SSPM) detector. The SSPM was developed by Rockwell International Science Center and has single-photon counting capability over the 0.4-28 mu m wavelength range, intrinsic time response of order 1 ns, and low detector noise (Petroff et al. 1987, Appl. Phys. Lett., 51, 6). We have operated a 200X200 mu m back-illuminated SSPM in a liquid-helium cooled dewar with a room-temperature transimpedance amplifier output. Single photon pulses can be easily distinguished above the amplifier noise. The individual photon pulses are binned at a selectable time resolution ranging from 5 mu s to 64 ms, and then written to Exabyte tape. In the first astronomical application of such a device, we have made observations of the Crab Nebula pulsar and Her X-1 at near-infrared wavelengths (J, H, and K bands), and we present the instrument sensitivities established by these observations. We discuss other astronomical observations which are either planned or currently underway. Finally, we present design specifications and predicted performances for a second-generation SSPM high-speed infrared photometer. RP Eikenberry, SS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Ransom, Scott/0000-0001-5799-9714 NR 9 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD OCT PY 1996 VL 108 IS 728 BP 939 EP 943 DI 10.1086/133816 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VN251 UT WOS:A1996VN25100013 ER PT J AU DiMichele, WA Bateman, RM AF DiMichele, WA Bateman, RM TI The rhizomorphic lycopsids: A case-study in paleobotanical classification SO SYSTEMATIC BOTANY LA English DT Review ID GEN-NOV; EVOLUTIONARY RELATIONSHIPS; GROWTH ARCHITECTURE; PENNSYLVANIAN-AGE; DINANTIAN FLORAS; NORTH-AMERICA; OXROAD BAY; PALEOECOLOGY; MORPHOLOGY; LYCOPHYTES AB The rhizomorphic lycopsids are a putatively monophyletic group delimited by the rhizomorphic syndrome: centralized determinate growth and secondary thickening in their rooting systems. A cladistic analysis of the most completely understood species provides the basis for two alternative, new classifications of the group, one following strict phylogenetic classification criteria, the other more traditionally Linnean. Both are based on the same preferred most-parsimonious cladogram and place the rhizomorphic lycopsids in one order, the Isoetales. Also, both classifications delimit the same suprageneric groups: Hizemodendron + Lepidodendron + Lepidophloios, Diaphorodendron + Synchysidendron, Sigillaria, and Chaloneria + Isoetes are well supported as monophyletic clades, but the basal plexus of bisporangiate-coned ulodendrids (Paralycopodites + Oxroadia + Paurodendron) is paraphyletic. Both classifications differ from all previous studies in 1) assigning all rhizomorphic lycopsids to a single order, and 2) recognizing the trees Diaphorodendron plus Synchysidendron as a distinct family the Diaphorodendraceae. A generally applicable paleobotanical taxonomic philosophy is outlined that broadly reflects a phylogenetic framework based on living species (if available) and reconstructed whole-plant fossil species. These core species provide a framework into which are interpolated satellite taxa: fossil isolated organs and partial plants. C1 ROYAL MUSEUM SCOTLAND, EDINBURGH EH1 7JF, MIDLOTHIAN, SCOTLAND. ROYAL BOT GARDENS, EDINBURGH EH3 5LR, MIDLOTHIAN, SCOTLAND. RP SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT PALEOBIOL, WASHINGTON, DC 20560 USA. RI DiMichele, William/K-4301-2012 NR 109 TC 46 Z9 52 U1 1 U2 5 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 1996 VL 21 IS 4 BP 535 EP 552 DI 10.2307/2419613 PG 18 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA WZ714 UT WOS:A1996WZ71400005 ER PT J AU Mulkey, SS Kitajima, K Wright, SJ AF Mulkey, SS Kitajima, K Wright, SJ TI Plant physiological ecology of tropical forest canopies SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID RAIN-FOREST; WATER RELATIONS; HYDRAULIC ARCHITECTURE; CARBON BALANCE; GAS-EXCHANGE; LEAF; TREE; PHOTOSYNTHESIS; PATTERNS; XYLEM AB Mechanistic information about tropical canopy function is emerging at the leaf, tree, stand and landscape levels. With improved canopy access, comprehensive data are accumulating about seasonal and spatial variation in light, temperature and humidity, and corresponding variation in leaf carbon gain and water loss. At the whole-plant level, simultaneous measurements at different spatial scales have revealed the role of boundary layer dynamics in regulating transpiration. Emergent properties of canopy function are being explored through models that integrate leaf and landscape-level exchange processes. Integration of exchange processes that include functional diversity at different scales has the potential to validate regional estimates of gas exchange, which are critical to our understanding of the role of tropical forests in global atmospheric carbon balance. C1 SMITHSONIAN TROP RES INST, MIAMI, FL 34002 USA. RP Mulkey, SS (reprint author), UNIV MISSOURI, DEPT BIOL, 8001 NAT BRIDGE RD, ST LOUIS, MO 63121 USA. RI Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 48 TC 48 Z9 51 U1 1 U2 22 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD OCT PY 1996 VL 11 IS 10 BP 408 EP 412 DI 10.1016/0169-5347(96)10043-4 PG 5 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA VK115 UT WOS:A1996VK11500007 PM 21237899 ER PT J AU Stibbe, DT Tennyson, J AF Stibbe, DT Tennyson, J TI Time-delay matrix analysis of resonances in electron scattering: e(-)-H-2 and H-2(+) SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID R-MATRIX; MOLECULAR-HYDROGEN; EXCITATION; IMPACT AB In electron scattering from complex targets such as complex atoms or molecules, resonance features often occur at energies where the target has many excited electronic states. Standard methods of determining resonance positions and widths are unreliably close to electronic thresholds or fail when a resonance is too wide or found to overlap another resonance. By finding the time-delay matrix given by Q = -ihS(*) dS/dE it is possible to fit the resonance positions and widths more precisely and with greater certainty. It is also possible to find the 'branching ratios', the probabilities of decay of the resonance to the continuum of each target state. This helps in the accurate assignment of the resonance (particularly for core-excited shape resonances), reducing the extensive detective work that is often required. The usefulness of the time-delay matrix is demonstrated with two R-matrix electron-molecule scattering calculations: e(-)-H-2 and e(-)-H-2(+), although the method is not restricted to any particular type of calculation or target species. Resonance positions and widths are found for e(-)-H-2(+). For the case of e(-)-H-2, H-2(-) resonances with 2 Sigma(g) symmetry are tracked as a function of bondlength. Their changing character is discussed and an avoided crossing at short internuclear separation is reported for the first time. The parentage of the 12 eV resonance has been classified as a (3) Sigma(g) contrary to previous classifications. Evidence of the notoriously shy series b resonances has been found. C1 UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. RP Stibbe, DT (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOL PHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Tennyson, Jonathan/I-2222-2012 OI Tennyson, Jonathan/0000-0002-4994-5238 NR 29 TC 39 Z9 39 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD SEP 28 PY 1996 VL 29 IS 18 BP 4267 EP 4283 DI 10.1088/0953-4075/29/18/021 PG 17 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA VK016 UT WOS:A1996VK01600021 ER PT J AU McNamara, BR Jannuzi, BT Elston, R Sarazin, CL Wise, M AF McNamara, BR Jannuzi, BT Elston, R Sarazin, CL Wise, M TI U-band polarimetry of the radio-aligned optical continuum in the Abell 1795 cluster central galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies, clusters, individual (A1795); galaxies, structure; polarization ID BL LACERTAE OBJECTS; STAR-FORMATION; COOLING FLOWS; IMAGING POLARIMETRY; REDSHIFT; ALIGNMENT; SCATTERING; EMISSION; MORPHOLOGIES; NGC-1275 AB We have obtained U-band polarimetry of the lobes of blue optical continuum located along the z = 0.063 F-R I radio source in the Abell 1795 cluster central galaxy. We find an upper limit to the degree of polarization of the light emitted from the lobes of less than 7%. The accuracy of this measurement is limited by the presence of diluting background starlight. This limit is inconsistent with the lobes being scattered light that originated in an obscured, anisotropically radiating nucleus, unless the radiation is beamed and is viewed at an angle less than or similar to 22 degrees to the line of sight, which is unlikely. The absence of a polarized signal and detailed correspondence between the radio lobes and optical lobes is inconsistent with synchrotron light. The blue optical lobes are probably regions of recent star formation. If a burst of star formation were triggered by the expanding radio lobes, the age of the burst population should be similar to 10(7) yr. Then, the star formation rate in both lobes, assuming the local IMF, is similar to 20 M(circle dot)yr(-1), and the stellar mass of the lobes is similar to 10(8) M(circle dot). The material fueling the star formation and the radio source may have originated from the cooling how or accretion from one or more gaseous cluster galaxies. C1 NATL OPT ASTRON OBSERV, TUCSON, AZ 85726 USA. INST ADV STUDY, PRINCETON, NJ 08540 USA. CERRO TOLOLO INTERAMER OBSERV, LA SERENA, CHILE. UNIV VIRGINIA, DEPT ASTRON, CHARLOTTESVILLE, VA 22903 USA. MIT, CTR SPACE RES, CAMBRIDGE, MA 02139 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 57 TC 27 Z9 27 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1996 VL 469 IS 1 BP 66 EP 72 DI 10.1086/177758 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VG436 UT WOS:A1996VG43600008 ER PT J AU Ford, E Kaaret, P Tavani, M Harmon, BA Zhang, SN Barret, D Grindlay, J Bloser, P Remillard, RA AF Ford, E Kaaret, P Tavani, M Harmon, BA Zhang, SN Barret, D Grindlay, J Bloser, P Remillard, RA TI Anticorrelated hard/soft X-ray emission from the X-ray burster 4U 0614+091 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars, individual (4U 0614+091); stars, neutron; X-Rays, Stars ID EXOSAT OBSERVATIONS; COMPTONIZATION AB We have detected transient X-ray activity from the X-ray burster 4U 0614+091 simultaneously with BATSE on board the Compton Gamma Ray Observatory (20-100 keV) and the all-sky monitor (ASM) on board the Rossi X-Ray Timing Explorer (1-12 keV). The peak fluxes reach approximately 40 mcrab in both instruments over a period of about 20 days. The variable emission shows a clear anticorrelation of the hard X-ray flux with the soft X-ray count rate. The observed anticorrelation is another clear counterexample to the notion that only black hole binaries exhibit such correlations. The individual spectra during this period can be fitted by power laws with photon indices 2.2 +/- 0.3 (ASM) and 2.7 +/- 0.4 (BATSE), while the combined spectra can be described by a single power law with index 2.09 +/- 0.08. BATSE and the Rossi X-Ray Timing Explorer ASM are a good combination for monitoring X-ray sources over a wide energy band. C1 COLUMBIA UNIV,COLUMBIA ASTROPHYS LAB,NEW YORK,NY 10027. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,UNIV SPACE RES ASSOC,HUNTSVILLE,AL 35812. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. RP Ford, E (reprint author), COLUMBIA UNIV,DEPT PHYS,538 W 120TH ST,NEW YORK,NY 10027, USA. NR 28 TC 12 Z9 12 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1996 VL 469 IS 1 BP L37 EP L40 DI 10.1086/310265 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VG438 UT WOS:A1996VG43800010 ER PT J AU Travers, MJ McCarthy, MC Kalmus, P Gottlieb, CA Thaddeus, P AF Travers, MJ McCarthy, MC Kalmus, P Gottlieb, CA Thaddeus, P TI Laboratory detection of the linear cyanopolyyne HC11N SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, molecules; line, identification; molecular data; molecular processes; radio lines, ISM ID HC9N; IRC AB The cyanopolyyne HC11N, the largest claimed interstellar molecule, has been detected in the laboratory. Its nearest microwave rotational transitions lie 0.13% lower in frequency than the lines identified in IRC+10216 and TMC-1, so it is concluded that the astronomical lines are something else entirely. The 20 laboratory lines measured with our Fourier transform molecular-beam spectrometer allow the entire microwave spectrum of HC11N to be determined to much better than 1 km s(-1) in equivalent radial velocity. A search for HC11N at the correct frequencies in published and unpublished spectra of these sources has turned up no convincing candidate lines, but detection is probably possible with one of the existing large radio telescopes. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Travers, MJ (reprint author), HARVARD UNIV,DIV APPL SCI,29 OXFORD ST,CAMBRIDGE,MA 02138, USA. NR 13 TC 26 Z9 26 U1 2 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1996 VL 469 IS 1 BP L65 EP L68 DI 10.1086/310254 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VG438 UT WOS:A1996VG43800017 ER PT J AU Gingerich, O AF Gingerich, O TI History of the hour: Clocks and modern temporal orders - DohrnvanRossum,G SO NATURE LA English DT Book Review RP Gingerich, O (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD SEP 19 PY 1996 VL 383 IS 6597 BP 229 EP 230 DI 10.1038/383229a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VH315 UT WOS:A1996VH31500043 ER PT J AU Hussein, MS Kharchenko, V AF Hussein, MS Kharchenko, V TI Quantized Fermi accelerator: A soluble model for quantum friction SO ANNALS OF PHYSICS LA English DT Article AB The motion of a particle constrained to move inside a box with a movable wall is quantized. The semiclassical, adiabatic and exact solutions are worked out. The time-dependent density matrix is found in closed form. The motions of the heavy and the light parts of the system, described by appropriate reduced density matrices, are discussed. General comments about quantum Friction are made. (C) 1996 Academic Press, Inc. C1 MIT,CTR THEORET PHYS,NUCL SCI LAB,CAMBRIDGE,MA 02139. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. UNIV SAO PAULO,INST FIS,BR-05508 SAO PAULO,BRAZIL. RP Hussein, MS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 1 Z9 1 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0003-4916 J9 ANN PHYS-NEW YORK JI Ann. Phys. PD SEP 15 PY 1996 VL 250 IS 2 BP 352 EP 366 DI 10.1006/aphy.1996.0096 PG 15 WC Physics, Multidisciplinary SC Physics GA VH196 UT WOS:A1996VH19600003 ER PT J AU Aiello, A AF Aiello, A TI The thermal warriors: Strategies of insect survival - Heinrich,B SO LIBRARY JOURNAL LA English DT Book Review RP Aiello, A (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 1 TC 0 Z9 0 U1 2 U2 4 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 15 PY 1996 VL 121 IS 15 BP 90 EP 90 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VR884 UT WOS:A1996VR88400181 ER PT J AU Riley, SM AF Riley, SM TI Manchu palaces - Larsen,J SO LIBRARY JOURNAL LA English DT Book Review RP Riley, SM (reprint author), SMITHSONIAN INST LIBS,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 15 PY 1996 VL 121 IS 15 BP 97 EP 97 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VR884 UT WOS:A1996VR88400227 ER PT J AU Begg, AA AF Begg, AA TI Only twice I've wished for heaven - Trice,DT SO LIBRARY JOURNAL LA English DT Book Review RP Begg, AA (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 15 PY 1996 VL 121 IS 15 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VR884 UT WOS:A1996VR88400231 ER PT J AU Blair, WP Long, KS Raymond, JC AF Blair, WP Long, KS Raymond, JC TI A search for Fe III in SN 1006 using the Hopkins ultraviolet telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE shock waves; supernovae, individual (SN 1006); supernova remnants; ultraviolet, ISM ID SUPER-NOVA REMNANT; X-RAY-SPECTRUM; OSCILLATOR-STRENGTHS; ABSORPTION-LINES; PALOMAR-GREEN; SN-1006; WAVELENGTHS; EMISSION; HOT AB We have observed the 912-1840 Angstrom spectrum of the sdOB star known as the Schweizer-Middleditch star, which lies behind the remnant of SN 1006, to search for absorption lines due to the unshocked ejecta. We have also observed the sdB star PG 0839+399 for comparison. The spectra were obtained using the Hopkins Ultraviolet Telescope on the Astro-2 Space Shuttle mission in 1995 March. Assuming SN 1006 was a Type Ia supernova, 0.3-0.5 M. of iron should be present in the expanding remnant. The X-ray spectrum shows no evidence for this quantity of iron in the hot gas, indicating that this material may still be interior to the reverse shock. Broad absorption lines of Fe II have been seen in the spectrum of the Schweizer-Middleditch (SM) star previously but can only account for a small fraction of the expected iron. Our spectrum covers the region of the strongest expected Fe III resonance line at 1123 Angstrom. We use stellar model fits to the spectra to constrain the strength of Fe III and Fe II lines in the spectral level of only 1.0 Angstrom equivalent width, below the value of similar to 2.3 Angstrom predicted with the current best model provided by Hamilton & Fesen. However, the Hamilton & Fesen model is not precluded by the statistics in our data, which provide a 3 sigma upper limit of 3.4 Angstrom for the equivalent width of Fe III lambda 1123. Converting into mass, our best fit corresponds to only 0.016 M. of Fe++, and the 3 sigma limit corresponds to less than or equal to 0.054 M. of Fe++. This indicates that if the expected iron is present in the ejecta, it must be largely in ionization states higher than Fe++. No other absorption lines attributable to the supernova remnant are detected in the spectrum below Ly alpha. A faint excess in the spectrum near 1170 Angstrom is unexplained but might be due to Ly alpha emission from the nonradiative shock on the near side of the supernova remnant shell. This possibility is testable with improved optical data for SN 1006. C1 SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Blair, WP (reprint author), JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,CHARLES & 34TH ST,BALTIMORE,MD 21218, USA. NR 52 TC 13 Z9 13 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1996 VL 468 IS 2 BP 871 EP 882 DI 10.1086/177743 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VE596 UT WOS:A1996VE59600038 ER PT J AU Nicolls, A AF Nicolls, A TI African design - Heirs to the trans-Saharan Trade SO AFRICAN ARTS LA English DT Art Exhibit Review RP Nicolls, A (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD FAL PY 1996 VL 29 IS 4 BP 72 EP 73 DI 10.2307/3337399 PG 2 WC Art SC Art GA VV300 UT WOS:A1996VV30000011 ER PT J AU Geary, CM AF Geary, CM TI Pawa: Memoir from the Belgian Congo, 1945-1949 - Lambrecht,FL SO AFRICAN ARTS LA English DT Book Review RP Geary, CM (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD FAL PY 1996 VL 29 IS 4 BP 89 EP 90 DI 10.2307/3337407 PG 2 WC Art SC Art GA VV300 UT WOS:A1996VV30000018 ER PT J AU Loring, S AF Loring, S TI Diversity and complexity in prehistoric maritime societies: A Gulf of Maine perspective - Bourque,BJ SO AMERICAN ANTHROPOLOGIST LA English DT Book Review RP Loring, S (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD SEP PY 1996 VL 98 IS 3 BP 659 EP 660 DI 10.1525/aa.1996.98.3.02a00380 PG 2 WC Anthropology SC Anthropology GA VF013 UT WOS:A1996VF01300051 ER PT J AU Slusser, MS AF Slusser, MS TI Lord Vishnu and the kings of Nepal SO ASIAN ART & CULTURE LA English DT Article RP Slusser, MS (reprint author), SMITHSONIAN INST,ARTHUR M SACKLER GALLERY,WASHINGTON,DC 20560, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD, ENGLAND OX2 6DP SN 1352-2744 J9 ASIAN ART CULT JI Asian Art Cult. PD FAL PY 1996 VL 9 IS 3 BP 9 EP 29 PG 21 WC Art SC Art GA WH448 UT WOS:A1996WH44800002 ER PT J AU Barton, E Geller, MJ Ramella, M Marzke, RO daCosta, LN AF Barton, E Geller, MJ Ramella, M Marzke, RO daCosta, LN TI Compact group selection from redshift surveys SO ASTRONOMICAL JOURNAL LA English DT Article ID PISCES-PERSEUS SUPERCLUSTER; 21 CM SURVEY; LUMINOSITY FUNCTION; 21-CM SURVEY; GALAXIES; ZONE; +27.5-DEGREES; +33.5-DEGREES; +21.5-DEGREES AB For the first time, we construct a catalog of compact groups selected from a complete, magnitude-limited redshift survey. We select groups with N greater than or equal to 3 members based on projected separation and association in redshift space alone. We evaluate the characteristics of the Redshift Survey Compact Groups (RSCG's). Their physical properties (membership frequency, velocity dispersion, density) are similar to those of the Hickson [ApJ, 255, 382 (1982)] Compact Groups. Hickson's isolation criterion is a strong function of the physical and angular group radii and is a poor predictor of the group environment. In fact, most RSCG's are embedded in dense environments. The luminosity function for RSCG's is mildly inconsistent with the survey luminosity function - the characteristic luminosity is brighter and the faint end shallower for the RSCG galaxies. We construct a model of the selection function of compact groups. Using this selection function, we estimate the abundance of RSCG's; for groups with N greater than or equal to 4 members the abundance is 3.8 x 10(-5)h(3) Mpc(-3). For all RSCG's (N greater than or equal to 3) the abundance is 1.4x10(-4)h(3) Mpc(-3). (C) 1996 American Astronomical Society. C1 OSSERV ASTRON TRIESTE,I-34131 TRIESTE,ITALY. DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. EUROPEAN SO OBSERV,D-85748 GARCHING,GERMANY. RP Barton, E (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Ramella, Massimo/0000-0001-5446-4749 NR 49 TC 61 Z9 61 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1996 VL 112 IS 3 BP 871 EP & DI 10.1086/118060 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VG154 UT WOS:A1996VG15400003 ER PT J AU Franklin, FA AF Franklin, FA TI An examination of the relation between chaotic orbits and the Kirkwood gap at the 2:1 resonance .2. Escaping orbits SO ASTRONOMICAL JOURNAL LA English DT Article ID ORIGINAL DISTRIBUTION; ASTEROIDS; JUPITER; SATURN AB This paper has a very simple motivation: will an integration of especially chaotic orbits within the 2:1 mean motion resonance with Jupiter lead to an escape from this resonance in times less than the solar system's age? We chose for the very chaotic specimens three orbits with Lyapunov times near 1000 yr, all of which initially lay near secondary resonances, i.e., where the ratios of the libration to apsidal frequencies were small integers. All three clearly escaped from the mean motion resonance (apparently the first instance of this behavior) in slightly less than 10(9) yr. These integrations allow us to follow escaping orbits in some detail. Because objects can readily move into a secondary resonance, thereby becoming severely chaotic, escape may be far more common than one might at first suppose. A far less chaotic orbit, integrated for above time, remained in the 2:1 resonance. Eccentricities of the three escapers rose above 0.5 (i.e., the value required to cross Mars' orbit) only just prior to escape. Thus we suspect that a depopulation of this resonance to form the well-known Kirkwood gap is more closely related to dynamical instability than just to collisions with any terrestrial planet. (C) 1996 American Astronomical Society. RP Franklin, FA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 9 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1996 VL 112 IS 3 BP 1247 EP 1253 DI 10.1086/118095 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VG154 UT WOS:A1996VG15400038 ER PT J AU Carilli, CL Lane, W DeBruyn, AG Braun, R Miley, GK AF Carilli, CL Lane, W DeBruyn, AG Braun, R Miley, GK TI Redshifted H1 21 CM line observations of damped LY a absorption systems (vol 111, pg 1830, 1996) SO ASTRONOMICAL JOURNAL LA English DT Correction, Addition C1 LEIDEN OBSERV,NL-2300 RA LEIDEN,NETHERLANDS. RICE UNIV,DEPT PHYS,HOUSTON,TX 77005. NETHERLANDS FDN RES ASTRON,NL-7990 AA DWINGELOO,NETHERLANDS. RP Carilli, CL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 1 TC 9 Z9 9 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1996 VL 112 IS 3 BP 1317 EP 1317 DI 10.1086/118103 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VG154 UT WOS:A1996VG15400046 ER PT J AU vanOjik, R Rottgering, HJA Carilli, CL Miley, GK Bremer, MN Macchetto, F AF vanOjik, R Rottgering, HJA Carilli, CL Miley, GK Bremer, MN Macchetto, F TI A powerful radio galaxy at z=3.6 in a giant rotating Lyman alpha halo SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies, active; galaxies, individual, 1243+036; radio continuum, galaxies; galaxies, kinematics and dynamics; cosmology, observations ID EMISSION-LINE GAS; HIGH-REDSHIFT; OPTICAL-EMISSION; CYGNUS-A; IMAGING POLARIMETRY; STAR FORMATION; COOLING FLOWS; JETS; QUASARS; SPECTROSCOPY AB We present the discovery and detailed observations of the radio galaxy 1243+036 at a redshift of z = 3.57. The radio source was selected on the basis of its extremely steep radio spectrum, suggesting that it might be very distant. The radio source was identified with a galaxy of R magnitude 22.5. Subsequent spectroscopy showed strong Lyman alpha and [O III]lambda lambda 5007,4959 emission, indicating that the object is a radio galaxy at z = 3.57. High resolution (0.2'') radio maps show an FRII type radio source with a sharply bent radio structure. Strong depolarization of the radio emission indicates that the source is embedded in a magneto-ionic medium. The most spectacular feature of 1243+036 is the presence of a Ly alpha halo of luminosity similar to 10(44.5) erg s(-1) which extends over similar to 20'' (135 kPc), A 0.6'' resolution Ly alpha image shows that the emission line gas is aligned with the main axis of the radio source and has structure down to the scale of the resolution. High resolution spectra show that the Ly alpha emitting gas has complex kinematic structure. The gas contained within the radio structure has a relatively high velocity width (similar to 1500 km s(-1) FWHM). The component of the Ly alpha emission that coincides with the bend in the radio structure is blueshifted with respect to the peak of the emission by 1100 km s(-1). There is low surface brightness Ly alpha emission aligned with, but extending 40 kpc beyond both sides of the radio source, This halo has a narrow velocity width (similar to 250 km s(-1) FWHM) and a velocity gradient of 450 km s(-1) over the extent of the emission. The presence of the quiescent Ly alpha component aligned with the AGN axis, but outside the radio source, is strong evidence that photoionization by anisotropically emitted radiation from the active nucleus is occurring. Various mechanisms for the origin and kinematics of the Ly alpha halo are discussed, Because the halo extends beyond the radio structure with less violent and more ordered kinematics than inside the radio structure, we conclude that the outer halo and its kinematics must predate the radio source, The ordered motion may be large-scale rotation caused by the accretion of gas from the environment of the radio galaxy or by a merger. Although alternatively the halo may be caused by a massive outflow, we argue that bulk inflow of the emission line gas is inconsistent with the most likely orientation of the radio source. The large velocity-width of the Ly alpha gas contained within the radio source compared to that of the outer halo suggest a direct interaction of the radio source with the gas. The spatial correlation of enhanced, blue-shifted Ly alpha emission and the sharp bend of the radio structure suggest that the emission line gas could have deflected the radio jet. The impact of the jet could have accelerated the gas at this position and may have locally enhanced the Ly alpha emission. Extended faint optical continuum emission is aligned with the principal radio axis, a phenomenon commonly observed in high redshift radio galaxies, This emission does not follow the bending of the radio jet, indicating that, at least in 1243+036, models invoking scattering of continuum radiation from the AGN as the cause of this alignment are favoured. C1 LEIDEN OBSERV, NL-2300 RA LEIDEN, NETHERLANDS. MULLARD RADIO ASTRON OBSERV, CAVENDISH LAB, CAMBRIDGE CB3 0HE, ENGLAND. INST ASTRON, CAMBRIDGE CB3 0HA, ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. EUROPEAN SPACE AGCY, DEPT SPACE SCI, F-75738 PARIS 15, FRANCE. NR 90 TC 87 Z9 87 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP 1 PY 1996 VL 313 IS 1 BP 25 EP 44 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VG169 UT WOS:A1996VG16900006 ER PT J AU Randich, S Schmitt, JHMM Prosser, C AF Randich, S Schmitt, JHMM Prosser, C TI Coronal activity in the Coma Berenices open cluster SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE open clusters and associations, individual (Coma Berenices); stars, coronae; X-ray, stars ID X-RAY SURVEY; CHEMICAL-COMPOSITION; HYADES CLUSTER; STARS; SPECTROSCOPY; PLEIADES; ROSAT AB We present ROSAT PSPC observations of the similar to 500 Myr old Coma Berenices cluster. The X-ray survey in Coma consists of a) a raster scan of short duration PSPC pointings, b) ROSAT All-Sky Survey data, and c) a 16 ksec deep PSPC pointing. The raster scan and the survey data were merged together covering an area of about 36 square degrees, while the deep pointing was analyzed separately. No major differences were found between the two datasets. Our ROSAT observations indicate that Coma is much more similar in its X-ray properties to the coeval Hyades than to the also coeval Praesepe cluster. As in the Hyades, almost all late-F and G stars were detected, also showing a comparable range in X-ray luminosity. X-ray luminosity distribution functions (XLDFs) for solar-type members are in close agreement with those of the Hyades, confirming that the majority of Praesepe's members are less luminous than what one would expect for stars of their age. The Coma Berenices cluster is known for its apparent deficit of low mass stars of spectral type K and later. We present 12 new possible low-mass Coma candidates, identified through this X-ray survey. C1 MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. OI Randich, Sofia/0000-0003-2438-0899 NR 38 TC 30 Z9 30 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 1996 VL 313 IS 3 BP 815 EP 827 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VM333 UT WOS:A1996VM33300020 ER PT J AU Kim, DW Fabbiano, G Matsumoto, H Koyama, K Trinchieri, G AF Kim, DW Fabbiano, G Matsumoto, H Koyama, K Trinchieri, G TI ASCA spectra of the X-RAY faint S0 galaxy NGC 4382 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, elliptical and lenticular, cD; galaxies, individual (NGC 4382); X-rays, galaxies ID STATISTICAL-ANALYSIS; CLUSTERS; EMISSION; SAMPLE; M31 AB NGC 4382 is one of the E and SO galaxies detected with the lowest X-ray-to-optical luminosity ratio. These galaxies have a peculiar X-ray (0.1-3 keV) spectrum, with a significant excess of counts in the lowest spectral channels (<1 keV) relative to the spectral count distributions of X-ray brighter E and S0 galaxies. Analyzing the ROSAT Position Sensitive Proportional Counter observations of NGC 4382, it was unclear whether this soft excess were due to a real very soft component in a multicomponent spectrum or reflected an extremely low metal abundance in a isothermal hot gas. Our ASCA observations show that the low-abundance single-temperature model does not fit well the X-ray spectrum, in agreement with our previous suggestions. A better explanation is a composite spectrum with a very soft component (similar to 0.3 keV) in addition to a hard, likely stellar, component (similar to 5 keV). In this model, the abundance cannot be constrained. However, other more complex spectral models cannot be excluded. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OSSERVATORIO ASTROFIS BRERA,I-20121 MILAN,ITALY. RP Kim, DW (reprint author), CHUNGNAM NATL UNIV,TAEJON 305764,SOUTH KOREA. NR 30 TC 37 Z9 37 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1996 VL 468 IS 1 BP 175 EP 183 DI 10.1086/177679 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VE592 UT WOS:A1996VE59200015 ER PT J AU Orosz, JA Bailyn, CD McClintock, JE Remillard, RA AF Orosz, JA Bailyn, CD McClintock, JE Remillard, RA TI Improved parameters for the black hole binary system X-ray Nova Muscae 1991 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, spectroscopic; black hole physics; novae, cataclysmic variables stars, individual (Nova Muscae); X-rays, stars ID PHOTOMETRIC STANDARD STARS; CELESTIAL EQUATOR; ACCRETION DISKS; EMISSION-LINE; LIGHT CURVES; A0620-00; MASS; HERCULIS; SPECTROSCOPY; SECONDARY AB We have continued to observe the black hole binary X-ray Nova Muscae 1991 (GS 1124-683, GU Mus, hereafter XN Mus 91) in quiescence over the last 3 years. These observations have yielded refined values of the orbital period (P = 0(d).4326058 +/- 0(d).0000031) and the semiamplitude of the absorption line radial velocity curve (K-2 = 406 +/- 7 km s(-1)). The implied mass function is f(M) = 3.01 +/- 0.15 M., which represents the minimum mass of the compact primary star. A reasonable lower limit on the mass of the primary, based on the lack of observed X-ray and optical eclipses and a previous measurement of the binary mass ratio, is M(1) > 4.4 M.; this mass exceeds the maximum mass of a stable neutron star, reinforcing the argument that XN Mus 91 contains a black hole. The phase-averaged spectrum (Doppler corrected to account for the orbital motion of the secondary) shows strong absorption lines consistent with a dwarf main-sequence star, with an MK type of K3 V-K5 V. The disk spectrum, obtained by subtracting the spectrum of a K5 V template star from the averaged spectrum, shows strong Balmer emission lines, as well as emission lines of He I and Fe II, which are superimposed on a relatively flat continuum. Ellipsoidal modeling of the light curves indicates that the inclination is in the range 54 degrees less than or equal to i less than or equal to 65 degrees. Using the mass function and our previous estimate of the mass ratio, the primary mass is then in the range 5.0 less than or equal to M(1) less than or equal to 7.5 M.. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. MIT, CTR SPACE RES, CAMBRIDGE, MA 02139 USA. RP Orosz, JA (reprint author), YALE UNIV, DEPT ASTRON, POB 208101, NEW HAVEN, CT 06520 USA. NR 55 TC 61 Z9 62 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1996 VL 468 IS 1 BP 380 EP 390 DI 10.1086/177698 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VE592 UT WOS:A1996VE59200034 ER PT J AU Aschwanden, MJ Wills, MJ Hudson, HS Kosugi, T Schwartz, RA AF Aschwanden, MJ Wills, MJ Hudson, HS Kosugi, T Schwartz, RA TI Electron time-of-flight distances and flare loop geometries compared from CGRO and Yohkoh observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; radiation mechanisms, nonthermal; Sun, corona; Sun, flares; Sun, X-rays, gamma rays ID HARD X-RAY; 1991 NOVEMBER 15; SOLAR-A MISSION; MAGNETIC RECONNECTION; IMPULSIVE PHASE; PARTICLE-ACCELERATION; BULK ENERGIZATION; BURSTS; RADIATION; TELESCOPE AB The distance between the coronal acceleration site and the chromospheric hard X-ray (HXR) emission site can be determined from velocity-dependent electron time-of-flight (TOF) differences in the framework of the thick-target model. We determine these electron TOF distances l with relative time delay measurements in the 30-300 keV energy range, using 16 channel data from BATSE/CGRO for the eight largest flares simultaneously observed with Yohkoh. We filter the HXR fine structure from the smoothly varying HXR flux with a Fourier filter in order to separate competing time delays. In the Yohkoh/HXT images we identify the corresponding flare loops that show greater than or equal to 30 keV HXR footpoint emission and project the electron TOF distances into the loop plane, assuming a semicircular shape (with radius r). The flare loop radii vary in the range of r = 5600-17,000 km. In all eight flares we find that the projected electron TOF distance l' exceeds the loop half-length s = r(pi/2), with a scale-invariant ratio of l'/s = 1.3 +/- 0.2. Projecting the electron TOF distances onto an open field line that extends to the cusp region above the flare loop, we find an average ratio of h/r = 1.7 +/- 0.4 for the height h of the acceleration site. This geometry is compatible with acceleration mechanisms operating in the cusp region, perhaps associated with magnetic reconnection processes above the flare loop. Alternatively, acceleration sites inside the flare loop cannot be ruled out (since l'/s < 2), but they do not provide a natural explanation for the observed length ratio l'/s. Large-scale electric DC held acceleration mechanisms are found to be less suitable to explain the observed HXR timing and pulse durations. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV HAWAII MANOA,INST ASTRON,HONOLULU,HI 96822. NATL ASTRON OBSERV,MITAKA,TOKYO 181,JAPAN. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP Aschwanden, MJ (reprint author), UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742, USA. NR 56 TC 70 Z9 72 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1996 VL 468 IS 1 BP 398 EP 417 DI 10.1086/177700 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VE592 UT WOS:A1996VE59200036 ER PT J AU Herrnstein, JR Greenhill, LJ Moran, JM AF Herrnstein, JR Greenhill, LJ Moran, JM TI The warp in the subparsec molecular disk in NGC 4258 as an explanation for persistent asymmetries in the maser spectrum SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies, individual (NGC 4258); galaxies, nuclei; galaxies, Seyfert; masers ID ACTIVE GALACTIC NUCLEI; SPIRAL GALAXY NGC-4258; X-RAY; CONTINUUM EMISSION; ACCRETION DISKS; VARIABILITY; LUMINOSITY; NGC4258 AB Neufeld & Maloney have proposed a model in which the warp in the subparsec-scale molecular disk in NGC 4258 allows direct illumination of the disk by a central X-ray source, heating the gas to temperatures appropriate for collisional pumping of water vapor masers. One element of this model is the creation of a layer of warm atomic gas above the cooler molecular gas where the masing occurs. Here, we examine the effects of this warm atomic gas on the maser emission. We find that for a range of plausible warps, thermal free-free extinction in the atomic gas can generate opacities of 2-3 at a wavelength of 1.3 cm. Furthermore, because of the orientation of the warp with respect to the line of sight, we argue that this extinction will only occur on the blueshifted side of the disk. Thus, we demonstrate that such thermal absorption is a likely explanation for the persistent weakness of the blueshifted maser features relative to the redshifted ones. RP Herrnstein, JR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 42,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Moran, James/0000-0002-3882-4414 NR 23 TC 65 Z9 65 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1996 VL 468 IS 1 BP L17 EP L20 DI 10.1086/310227 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VE594 UT WOS:A1996VE59400005 ER PT J AU Kalkofen, W AF Kalkofen, W TI Chromospheric oscillations in K-2v bright points SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun, chromosphere; Sun, magnetic fields; Sun, oscillations; waves ID SOLAR CHROMOSPHERE; MAGNETIC-FIELDS; ACOUSTIC-WAVES; ATMOSPHERE; PROPAGATION; DYNAMICS; FEATURES AB The 3 minute waves observed in K-2v emission from bright points in the quiet solar chromosphere are shown to be oscillations of the atmosphere at the cutoff period of acoustic waves, implying impulsive excitation. Other interpretations of the period are shown not to be viable since they fail the dual requirement of spatial intermittence, in which most of the supergranulation cell interior is inert over the course of an hour, and temporal intermittence, in which the active locations in the cell interior are active at most half the time. It is speculated that the episodic excitation of the K-2v oscillations is due to collisions of granules with magnetic elements of mixed polarity with a field strength of at least 0.5 kG. RP Kalkofen, W (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 39 TC 25 Z9 25 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1996 VL 468 IS 1 BP L69 EP L72 DI 10.1086/310220 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VE594 UT WOS:A1996VE59400017 ER PT J AU Claussen, MJ Wilking, BA Benson, PJ Wootten, A Myers, PC Terebey, S AF Claussen, MJ Wilking, BA Benson, PJ Wootten, A Myers, PC Terebey, S TI A monthly survey of water masers associated with low-mass stars SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; masers; stars, pre-main-sequence; surveys ID HERBIG-HARO OBJECTS; RHO-OPHIUCHI CLOUD; SUBMILLIMETER-WAVELENGTH OBSERVATIONS; VELOCITY MOLECULAR GAS; FORMING DENSE CORES; IRAS SOURCES; H2O MASERS; DARK CLOUDS; RADIO-CONTINUUM; EXCITING SOURCE AB We have performed a multiepoch survey of water masers toward low-luminosity young stellar objects (YSOs). These objects were selected to be in an early phase of stellar evolution based on IRAS colors and association with molecular outflows or dense cores. The sample was restricted to YSOs in nearby clouds (d less than or equal to 450 pc) with luminosities <120 L.. Seven new sources of maser emission have been found resulting in a total of 22 YSOs with L <120 L, known to display maser activity. We present monitoring data (at least two epochs of observation) for 47 sources. Four objects were monitored On a semiregular basis for more than 5 years. Based on a coherent 13 month subset of this survey, we estimate that the maser phase in low-mass embedded sources occupies about one-third of the duration of the embedded phase of evolution. Some spectrally isolated water maser features are seen to appear and disappear on timescales less than about 2 months. This characteristic timescale is consistent with shock crossing times for reasonable values of the shock velocity and size and is thus suggestive that the masers originate in the shocked gas. Some embedded sources can have long periods of inactivity (similar to 5 yr) when no masers are seen to our detection limit. Sources with stronger masers and more complex spectra can maintain emission over this same time period. We determined threshold values of the CO mass-loss rate (4 x 10(-5) M. yr(-1)), 6 cm radio luminosity (0.25 kpc(2) mJy), and the IRAS in-band luminosity (25 L.) above which water masers were always detected. The isotropic luminosity of the water masers in any given source can vary over more than 2 orders of magnitude in a period of several months. Thus, a single epoch measurement of this luminosity may provide a misleading result, especially if compared to other physical parameters such as the bolometric luminosity. C1 UNIV MISSOURI, DEPT PHYS & ASTRON, ST LOUIS, MO 63121 USA. WELLESLEY COLL, WHITIN OBSERV, WELLESLEY, MA 02181 USA. NATL RADIO ASTRON OBSERV, CHARLOTTESVILLE, VA 22903 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. CALTECH, IPAC, PASADENA, CA 91125 USA. IPAC, JPL, PASADENA, CA 91125 USA. RP NATL RADIO ASTRON OBSERV, AOC, POB O, SOCORRO, NM 87801 USA. NR 87 TC 80 Z9 80 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 1996 VL 106 IS 1 BP 111 EP 132 DI 10.1086/192330 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VF415 UT WOS:A1996VF41500006 ER PT J AU Morton, ES Derrickson, KC AF Morton, ES Derrickson, KC TI Song ranging by the dusky antbird, Cercomacra tyrannina: Ranging without song learning SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE song ranging; song learning; song evolution; tropical suboscine; Cercomacra tyrannina ID CAROLINA WREN; UNDEGRADED SONGS; SAYORNIS-PHOEBE; EASTERN PHOEBE; PARUS-MAJOR; DISTANCE; DEGRADATION; FAMILIARITY; SIGNALS; SOUNDS AB In a population of dusky antbirds (Cercomacra tyrannina), less aggressive responses to distance-degraded playbacks than to undegraded playbacks of pair duets show that this tropical suboscine passerine uses sound degradation to range distance from singing conspecifics. This is the first example of song-ranging in a species that does not learn songs, supporting the hypothesis that ranging preceded the song learning that occurs in more recently evolved passerine birds (oscines). Both sexes sing and are able to use song degradation to range distance from singers when their sex-specific song is played back. RP Morton, ES (reprint author), SMITHSONIAN INST, NATL ZOOL PK, DEPT ZOOL RES, WASHINGTON, DC 20008 USA. NR 22 TC 50 Z9 50 U1 0 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD SEP PY 1996 VL 39 IS 3 BP 195 EP 201 DI 10.1007/s002650050281 PG 7 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA VK949 UT WOS:A1996VK94900006 ER PT J AU Gunter, A AF Gunter, A TI Statues from Ain-Ghazal at the Smithsonian SO BIBLICAL ARCHAEOLOGIST LA English DT Article RP Gunter, A (reprint author), SMITHSONIAN INST,SACKLER GALLERY,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU SCHOLARS PRESS PI ATLANTA PA PO BOX 15399, ATLANTA, GA 30333-0399 SN 0006-0895 J9 BIBLIC ARCHAEOL JI Biblic. Archeol. PD SEP PY 1996 VL 59 IS 3 BP 180 EP 180 PG 1 WC Archaeology SC Archaeology GA VT495 UT WOS:A1996VT49500006 ER PT J AU Perfecto, I Rice, RA Greenberg, R VanderVoort, ME AF Perfecto, I Rice, RA Greenberg, R VanderVoort, ME TI Shade coffee: A disappearing refuge for biodiversity SO BIOSCIENCE LA English DT Article ID RELATIVE DISTRIBUTIONS; CORDIA-ALLIODORA; ANT COMMUNITIES; PUERTO-RICO; LOS-TUXTLAS; FORESTS; AGROECOSYSTEMS; PLANTATIONS; DIVERSITY; FARMS C1 SMITHSONIAN MIGRATORY BIRD CTR,WASHINGTON,DC 20008. RP Perfecto, I (reprint author), UNIV MICHIGAN,SCH NAT RESOURCES & ENVIRONM,ANN ARBOR,MI 48109, USA. NR 65 TC 427 Z9 471 U1 9 U2 77 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD SEP PY 1996 VL 46 IS 8 BP 598 EP 608 DI 10.2307/1312989 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VD351 UT WOS:A1996VD35100011 ER PT J AU Smith, WJ Smith, AM AF Smith, WJ Smith, AM TI Vocal signalling of the great crested flycatcher, Myiarchus crinitus (Aves, Tyrannidae) SO ETHOLOGY LA English DT Article ID SONG; INFORMATION; BEHAVIOR; WARBLERS; BIRDS AB The singing and related vocalizing of great crested flycatchers, Myiarchus crinitus (Aves, Tyrannidae), included at least 12 different vocalizations. Each vocalization correlated with (and thus made information available about) a distinctive range of behaviour, from unassertive to more actively responsive, provocative or even confrontational. Four were used by individuals primarily when alone and not initiating close social encounters. ?The eight other vocalizations were uttered primarily in close encounters: one in preliminaries to such events, two predominantly in encounters with opponents, another in close associating of mates, two in duetting, and two infrequently, mostly in confrontations. The division of the repertoire into sets of vocalizations providing information about either low or elevated probabilities that a signaller will undertake the behavioural initiatives that precede, shape or sustain social interactions parallels a division found in other recently studied passerines. Such information is pertinent to individuals' decisions to forego or start close interactions with, for instance, competitors or mates. The information should be useful to a great many species, not just birds, but also mammals and various other animals - species in which individuals keep each other informed by singing when they are apart. C1 SMITHSONIAN TROP RES INST,PANAMA CITY,FL. RP Smith, WJ (reprint author), UNIV PENN,DEPT BIOL,PHILADELPHIA,PA 19104, USA. NR 30 TC 14 Z9 14 U1 0 U2 8 PU BLACKWELL WISSENSCHAFTS-VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0179-1613 J9 ETHOLOGY JI Ethology PD SEP PY 1996 VL 102 IS 9 BP 705 EP 723 PG 19 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA VP779 UT WOS:A1996VP77900001 ER PT J AU Smith, WJ Smith, AM AF Smith, WJ Smith, AM TI Playback interactions with great crested flycatchers, Myiarchus crinitus (Aves, Tyrannidae) SO ETHOLOGY LA English DT Article ID TURDUS-MERULA; SONG; INFORMATION AB Interactive playback was used to test observational findings that different vocalizations uttered by singing great crested flycatchers, Myiarchus crinitus (Aves, Tyrannidae), each provide distinctive information about behavior. We present the results of these tests and interpret their significance in combination with the observations. The following predictions were confirmed: 1. Few weep or weeuh songs, and no thrr, were uttered by subjects that approached playback; 2. Churr, common during observations of more active and changing behavior, often predominated during subjects' initial approaches and searches for simulated intruders; 3. Churr was succeeded by wit,which had been found during confrontational behavior, and weihp, which came with movement near opponents or playback; and 4. Quick answers to vocalizations of mates, opponents, and playback were with rreet,also uttered during attack behavior. Functionally, birds uttering the unassertive vocalizations (weep, weeuh and thrr) may have been taking only minimal initiative to interact, and simply advertising their presence and potential responsiveness. With increasing numbers of churr, subjects maintained social contact with mates or opponents or probed for responses from quieter birds. Wit and weihp may strongly provoke opponents to respond. Further escalation involved rreet,weer, and wi. In contrast, Eh-ec was a defensive threat This species sings with more vocalizations than do ether tyrannids we have studied. Its vocalizations correlate with relatively fine distinctions among behavioral categories. Yet the vocalizations, like those of the other species, provide information about different extents of initiative that a singer will show in interacting. Such information could be fundamentally important in shaping and stabilizing social relationships, not just of tyrannids but also of many other kinds of animals that use singing to interact with one another while at a distance. C1 SMITHSONIAN TROP RES INST,PANAMA CITY,FL. RP Smith, WJ (reprint author), UNIV PENN,DEPT BIOL,PHILADELPHIA,PA 19104, USA. NR 17 TC 9 Z9 10 U1 0 U2 4 PU BLACKWELL WISSENSCHAFTS-VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0179-1613 J9 ETHOLOGY JI Ethology PD SEP PY 1996 VL 102 IS 9 BP 724 EP 735 PG 12 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA VP779 UT WOS:A1996VP77900002 ER PT J AU Huber, BT Hodell, DA AF Huber, BT Hodell, DA TI Middle-Late Cretaceous climate of the southern high latitudes: Stable isotopic evidence for minimal equator-to-pole thermal gradients: Reply SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Letter ID JAMES-ROSS-ISLAND; PLANKTIC FORAMINIFERA; MARINE TEMPERATURES; SEDIMENTS; PALEOTEMPERATURES; ANTARCTICA; EVOLUTION; PACIFIC; EOCENE; OCEAN C1 UNIV FLORIDA,DEPT GEOL,GAINESVILLE,FL 32611. RP Huber, BT (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,MRC NHB121,WASHINGTON,DC 20560, USA. NR 30 TC 12 Z9 13 U1 0 U2 3 PU GEOLOGICAL SOC AMERICA PI BOULDER PA PO BOX 9140 3300 PENROSE PLACE, BOULDER, CO 80301 SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD SEP PY 1996 VL 108 IS 9 BP 1193 EP 1196 PG 4 WC Geosciences, Multidisciplinary SC Geology GA VG003 UT WOS:A1996VG00300010 ER PT J AU Zimbelman, JR Williams, SH AF Zimbelman, JR Williams, SH TI Wind streaks: Geological and botanical effects on surface albedo contrast SO GEOMORPHOLOGY LA English DT Article ID SEDIMENT TRANSPORT; MOJAVE-DESERT; MARS; EVOLUTION; CALIFORNIA; SHEETFLOOD; MARINER-9; FEATURES; MAGELLAN; EXAMPLE AB Two wind streaks in the eastern Mojave Desert of California were examined to gain insight into the origin of the surface brightness contrast that makes them visible, both on the ground and in remote sensing data. The two localities are: a 4-km-long dark streak oriented S43E from the Amboy cinder cone (34 degrees 32'N, 115 degrees 46'W), located on a Quaternary basalt flow covered with aeolian sand, and a 2-km-long dark streak oriented S22E from a low hill near the southwestern base of Sleeping Beauty Mountain (34 degrees 48'N, 116 degrees 20'W), located on a sand-covered alluvial surface. in both cases, the dark streaks have enhanced rock abundances on the streak surface, relative to the surroundings. At the Amboy streak, slope wash likely contributed to the rock concentration on the streak surface, shielded from burial under aeolian sand by the cinder cone. Ar the Sleeping Beauty streak, the relative albedo contrast is strongly emphasized by the presence of Big Galleta grass only outside of the streak. The albedo contrast of the Sleeping Beauty streak can be effectively eliminated by the seasonal presence of annual grass preferentially within the streak. Some plants may have reflectances that are strongly dependent upon viewing and illumination geometry, raising the possibility that certain terrestrial aeolian features may appear variable on a diurnal basis. Alluvial processes appear to have been important at both localities for redistributing surface materials, even given the infrequent rain conditions present in the Mojave Desert. C1 UNIV N DAKOTA,CTR AEROSP SCI,DEPT SPACE STUDIES,GRAND FORKS,ND 58202. RP Zimbelman, JR (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. NR 36 TC 5 Z9 5 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X J9 GEOMORPHOLOGY JI Geomorphology PD SEP PY 1996 VL 17 IS 1-3 BP 167 EP 185 DI 10.1016/0169-555X(95)00098-P PG 19 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA VE330 UT WOS:A1996VE33000013 ER PT J AU Tong, CYE Blundell, R Paine, S Papa, DC Kawamura, J Zhang, XL Stern, JA LeDuc, HG AF Tong, CYE Blundell, R Paine, S Papa, DC Kawamura, J Zhang, XL Stern, JA LeDuc, HG TI Design and characterization of a 250-350-GHz fixed-tuned superconductor-insulator-superconductor receiver SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article ID SIS RECEIVERS; MIXER; NOISE; JUNCTIONS AB A fixed-tuned superconductor-insulator-superconductor (SIS) receiver has been designed to operate in the 250-350-GHz frequency band, This receiver has a double-side-band noise temperature of between 35 and 45 K, or about 3hv/k(B), over its entire operating band, Extensive characterization of the receiver has been carried out using techniques developed for submillimeter waves. The input noise, side-band ratio, 1 dB compression point, optimum LO drive level, and vector near-field beam profile have all been measured experimentally, The measurement techniques and results are presented and discussed. C1 CALTECH,JET PROP LAB,CTR SPACE MICROELECT TECHNOL,PASADENA,CA 91109. RP Tong, CYE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Tong, Edward/0000-0002-7736-4203; Paine, Scott/0000-0003-4622-5857 NR 27 TC 32 Z9 32 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD SEP PY 1996 VL 44 IS 9 BP 1548 EP 1556 DI 10.1109/22.536603 PG 9 WC Engineering, Electrical & Electronic SC Engineering GA VH032 UT WOS:A1996VH03200005 ER PT J AU Spitzer, N AF Spitzer, N TI The producer-professor + Folklorist, Kenny Goldstein SO JOURNAL OF AMERICAN FOLKLORE LA English DT Item About an Individual RP Spitzer, N (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0021-8715 J9 J AM FOLKLORE JI J. Am. Folk. PD FAL PY 1996 VL 109 IS 434 BP 463 EP 463 DI 10.2307/541191 PG 1 WC Folklore SC Arts & Humanities - Other Topics GA XD720 UT WOS:A1996XD72000012 ER PT J AU Roth, TL Swanson, WF Collins, D Burton, M Garell, DM Wildt, DE AF Roth, TL Swanson, WF Collins, D Burton, M Garell, DM Wildt, DE TI Snow leopard (Panthera uncia) spermatozoa are sensitive to alkaline pH, but motility in vitro is not influenced by protein or energy supplements SO JOURNAL OF ANDROLOGY LA English DT Article DE felid; comparative biology; sperm culture medium; sperm function; capacitation; sodium bicarbonate ID CHEETAH ACINONYX-JUBATUS; CAT FELIS-BENGALENSIS; DOMESTIC CAT; FERTILIZATION INVITRO; SEMINAL PLASMA; ACROSOME REACTION; SPERM VIABILITY; EGGS INVITRO; IN-VITRO; CAPACITATION AB To better understand the biology of snow leopard spermatozoa and to facilitate developing assisted reproduction, a series of studies was conducted to: 1) identify the component(s) of complex culture media responsible for the detrimental effect on sperm survival in vitro, 2) optimize medium for supporting sperm viability, and 3) evaluate sperm capacitation in vitro. Constituents of complex media were added systematically to phosphate-buffered saline (PBS) to isolate the factor(s) influencing snow leopard sperm motility in vitro. Sperm capacitation was also assessed following incubation in PBS with bovine serum albumin (BSA), fetal calf serum (FCS), or heparin. For maintaining sperm motility, there was no benefit (P greater than or equal to 0.05) to supplementing PBS with low (5%) or high (20%) concentrations of snow leopard serum (SLS) versus FCS or BSA. Likewise, adding supplemental energy substrates (pyruvate, glucose, lactate, or glutamine) did not enhance or hinder (P greater than or equal to 0.05) sperm motility. However, motility rapidly decreased (P < 0.05) with the addition of NaHCO3 to PBS or Ham's F10 nutrient mixture. Surprisingly, Ham's F10 with no buffering component or with both NaHCO3 and N-Z-hydroxyethylpiperazine-N'-2-ethanesulfonic acid (HEPES) maintained sperm motility at levels similar (P greater than or equal to 0.05) to PBS. Although sperm motility in all treatments decreased with time, there was a strong inverse relationship (P < 0.01; r = 0.90) between motility and sample pH at 6 hours. Spermatozoa incubated in PBS containing FCS, BSA, or heparin did not undergo the acrosome reaction when exposed to calcium ionophore. In summary, alkaline pH has a profound detrimental effect on snow leopard sperm motility, and capacitation does not occur under conditions that normally promote this event in other felid species. These results clearly demonstrate a high degree of interspecific variation among felids in fundamental sperm function, and they provide evidence for the necessity of basic research when developing assisted reproduction in little-studied nondomestic species. C1 SMITHSONIAN INST,NATL ZOOL PK,NOAHS,CONSERVAT & RES CTR,FRONT ROYAL,VA. WOODLAND PK ZOO,SEATTLE,WA. CHEYENNE MT ZOOL PK,COLORADO SPRINGS,CO. SENECA PK ZOO,ROCHESTER,NY. FU NICHD NIH HHS [R01 HD 23853] NR 55 TC 5 Z9 5 U1 0 U2 6 PU AMER SOC ANDROLOGY, INC PI LAWRENCE PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 SN 0196-3635 J9 J ANDROL JI J. Androl. PD SEP-OCT PY 1996 VL 17 IS 5 BP 558 EP 566 PG 9 WC Andrology SC Endocrinology & Metabolism GA VV826 UT WOS:A1996VV82600014 PM 8957700 ER PT J AU Stanley, DJ Wingerath, JG AF Stanley, DJ Wingerath, JG TI Clay mineral distributions to interpret Nile cell provenance and dispersal .1. Lower river Nile to delta sector SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Aswan; clay minerals; Egyptian shell; High Aswan Dam; Lake Nasser; Levant margin; new lacustrine Nile delta; Nile delta; Nile littoral cell; Nile sediment transport ID SEDIMENT TRANSPORT; MEDITERRANEAN SEA; CONTINENTAL-SHELF; HEAVY MINERALS; EGYPT; EVOLUTION; STRATIGRAPHY; PATTERNS; HISTORY; LAGOON AB Clay minerals serve as petrological markers that can be used to measure and interpret ongoing changes in River Nile sedimentation, now largely affected by anthropogenic influences. Closure in 1964 of the High Dam at Aswan, in particular, has entrained marked changes of clay mineral assemblages along the Nile in Egypt. Size-sorting phenomena, for example, are noted in the Nile delta; reduced grain size of sediment carried by altered Nile water flow patterns across the delta plain in part accounts for increased proportions of smectite in this sector and at the coast. However, most clay assemblage changes between southern Lake Nasser and Cairo are primarily the result of recently altered source terrains and dispersal patterns along this fluvial system rather than textural factors. The new delta forming in southern Lake Nasser contains typical River Nile (smectite-rich) clay mineral assemblages. In contrast, central and northern Lake Nasser contains higher proportions of kaolinite, derived through wave erosion of the lake margin and from wind transported material. The highest proportion of kaolinite in the Nile assemblage is recorded at Aswan. This kaolinite is derived from suspended sediment in Lake Nasser waters dispersed through the High Dam and from scouring of kaolinite-rich pre-Holocene deposits by the river below the dam. These kaolinite assemblages are deposited at least as far as Middle Egypt, about 350 km north of the dam. Relative percentages of kaolinite below Qena likely decrease as a result of progressive downriver input from smectite-rich pre-dam Nile channel and bank deposits; these eroded materials attenuate important amounts of kaolinite transported northward by the Nile. It is predicted that enhanced proportions of kaolinite will be recorded downriver at Cairo within fifty years and to the Mediterranean coast of the Nile delta by the end of the next century. RP Stanley, DJ (reprint author), SMITHSONIAN INST, DELTAS GLOBAL CHANGE PROGRAM, E-206 NMNH, WASHINGTON, DC 20560 USA. NR 92 TC 24 Z9 24 U1 0 U2 4 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD FAL PY 1996 VL 12 IS 4 BP 911 EP 929 PG 19 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA VX661 UT WOS:A1996VX66100016 ER PT J AU Dudley, R Chai, P AF Dudley, R Chai, P TI Animal flight mechanics in physically variable gas mixtures SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE aerodynamics; biomechanics; density; flight; hummingbirds; insects ID INSECT FLIGHT; HUMMINGBIRDS; OXYGEN; POWER; AERODYNAMICS; PERFORMANCE; ENERGETICS; HELIOX; APIDAE AB Empirical studies of animal flight performance have generally been implemented within the contemporary Experimental alteration of the physical of gas mixtures, however, permits construction of novel flight media and the non-invasive manipulation of flight biomechanics, For example, replacement of atmospheric nitrogen with various noble gases results in a tenfold variation in air density at a constant oxygen concentration, Such variation in air density correspondingly elicits extraordinary biomechanical effort from flying animals; hummingbirds and euglossine orchid bees hovering in such low-density but normoxic mixtures have demonstrated exceptionally high values for the mechanical power output of aerobic flight muscle, As with mechanical power, lift coefficients during hovering increase at low air densities in spite of a concomitant decline in the Reynolds number of the wings, The physical effects of variable gas density may also be manifest in morphological and physiological adaptations of animals to flight across altitudinal gradients. Global variation in atmospheric composition during the late Paleozoic may also have influenced the initial evolution and subsequent diversification of ancestral pterygotes. For the present-day experimenter, the use of physically variable flight media represents a versatile opportunity to explore the range of kinematic and aerodynamic modulation available to flying animals. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RP Dudley, R (reprint author), UNIV TEXAS, DEPT ZOOL, AUSTIN, TX 78712 USA. NR 33 TC 31 Z9 31 U1 2 U2 10 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD SEP PY 1996 VL 199 IS 9 BP 1881 EP 1885 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA VK049 UT WOS:A1996VK04900001 ER PT J AU Houck, MM Ubelaker, D Owsley, D Craig, E Grant, W Fram, R Woltanski, T Sandness, K AF Houck, MM Ubelaker, D Owsley, D Craig, E Grant, W Fram, R Woltanski, T Sandness, K TI The role of forensic anthropology in the recovery and analysis of Branch Davidian compound victims: Assessing the accuracy of age estimations SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; forensic anthropology; physical anthropology; age-at-death estimation; Branch Davidian; compound ID OS-PUBIS AB Age-at-death estimations of 44 individuals (27 adults, 17 children) from the Branch Davidian sample were compared with their actual ages. Estimations were evaluated for bias and accuracy for the actual age at death. Although the overall average estimates correlated well with the actual ages (r = 0.946), several individuals displayed high residual requiring further analysis and review. These individuals displayed age-related features that did not correspond with the expected morphology for individuals of their ages. Several age estimation techniques scored these individuals with all bias in the same direction. These examples should serve as cautionary reminders that biology does not always correlate with expected outcomes, particularly in such multifaceted traits such as age. C1 NATL MUSEUM NAT HIST,SMITHSONIAN INST,DEPT ANTHROPOL,WASHINGTON,DC 20560. MED EXAMINERS OFF,FRANKFORT,KY. USA,CENT IDENTIFICAT LAB,HICKAM AFB,HONOLULU,HI. TARRANT CTY MED EXAMINERS OFF,CRIMINALIST LAB,FT WORTH,TX. RP Houck, MM (reprint author), FBI LAB,HAIRS & FIBERS UNIT,RM 3931,10TH & PENN AVE NW,WASHINGTON,DC 20535, USA. NR 30 TC 9 Z9 9 U1 1 U2 4 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD SEP PY 1996 VL 41 IS 5 BP 796 EP 801 PG 6 WC Medicine, Legal SC Legal Medicine GA VE526 UT WOS:A1996VE52600013 PM 8789840 ER PT J AU Sharma, RD Dothe, H vonEsse, F Kharchenko, VA Sun, Y Dalgarno, A AF Sharma, RD Dothe, H vonEsse, F Kharchenko, VA Sun, Y Dalgarno, A TI Production of vibrationally and rotationally excited NO in the nighttime terrestrial thermosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID POTENTIAL-ENERGY SURFACE; SPACE-SHUTTLE EXPERIMENT; NITRIC-OXIDE; ATOMIC OXYGEN; RATE COEFFICIENTS; RELAXATION; BAND AB A quantitative interpretation is given of the observed quiescent nighttime radiance of nitric oxide in the fundamental vibration-rotation band near 5.3 mu m. The radiance measured in the space shuttle experiment Cryogenic Infrared Radiance Instrumentation for Shuttle (CIRRIS-1A) is known to have two components, one characterized by a thermal population of rotational levels and the other by a highly excited rotational population. The analysis presented here confirms that the thermal population is due to impact excitation of NO by atomic oxygen and attributes the highly excited distribution to the reaction of N(S-4) atoms with O-2. The measured nighttime emission profile is compared with predictions for several model atmospheres. Both sources of excited NO depend upon the latitude, longitude, local time, and geomagnetic indices. The fraction of vibrationally excited NO produced by the reaction of N(S-4) with O-2 increases rapidly with altitude from 130 to 200 km and its contribution to cooling, though much less than that from inelastic excitation of NO(nu=0) is, at higher altitudes, comparable to cooling produced by the atomic oxygen fine-structure line at 63 mu m. C1 MEI TECHNOL CORP,LEXINGTON,MA 02173. HARVARD UNIV,SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Sharma, RD (reprint author), PHILLIPS LAB,GEOPHYS DIRECTORATE,OPT ENVIRONM DIV,BEDFORD,MA 01731, USA. NR 35 TC 31 Z9 31 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES JI J. Geophys. Res-Space Phys. PD SEP 1 PY 1996 VL 101 IS A9 BP 19707 EP 19713 DI 10.1029/96JA01004 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VF257 UT WOS:A1996VF25700007 ER PT J AU Habbal, SR Mossman, A Gonzalez, R Esser, R AF Habbal, SR Mossman, A Gonzalez, R Esser, R TI Radio, visible, and X ray emission preceding and following a coronal mass ejection SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-FLARE MYTH; NOISE STORM; MISSION; EVENT AB This study uses both disk and limb observations to examine the changing conditions of the low solar corona, below 1.5 R(S), preceding and following a coronal mass ejection observed on the west limb on April 12, 1993. The disk observations comprise 90 cm (333 MHz) radio and daily Yohkoh soft X ray measurements, while the limb observations include measurements of emission from X rays, Fe X 637.4 nm and Fe XIV 530.3 nm coronal lines, and broadband Thomson-scattered white light. The analysis of the disk and limb observations shows that throughout the 3 days of consecutive observations, the occurrence and persistence of nonthermal emission at 90 cm, also known as type I noise storm emission, were associated with large-scale magnetic structures where the coronal mass ejection eventually occurred. Other than a subsequent flare observed in X rays at the limb, the changes in the coronal emission preceding and following the event were not markedly different from changes in other neighboring structures. The analysis of this novel combination of data supports the current view that coronal mass ejections are a cause rather than a consequence of the ''classical'' solar activity in the low corona. The radio observations, on the other hand, suggest that a connection between a noise storm and a coronal mass ejection exists. However, they do not necessarily imply that the noise storm actually initiates the event. RP Habbal, SR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 36 TC 17 Z9 17 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES JI J. Geophys. Res-Space Phys. PD SEP 1 PY 1996 VL 101 IS A9 BP 19943 EP 19955 DI 10.1029/96JA01190 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VF257 UT WOS:A1996VF25700027 ER PT J AU Lorenzini, EC Bortolami, SB Rupp, CC Angrilli, E AF Lorenzini, EC Bortolami, SB Rupp, CC Angrilli, E TI Control and flight performance of tethered satellite small expendable deployment system-II SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID SUBSATELLITE AB The second mission of the small expendable deployment system (SEDS-II) followed the successful mission of SEDS-I, which deployed freely a small instrumented probe on a 20-km tether. Unlike SEDS-I, the deployment of SEDS-II was controlled to provide a small libration amplitude and tether velocity at the end of deployment, The preflight goal for SEDS-II was a maximum libration of less than 10 deg and a final velocity of less than 1 m/s. The control problem was made difficult by the limited capabilities of the SEDS sensors and onboard computer and the large uncertainties inherent in the response of the actuator (brake) and the plant (deployer). The nonlinear, nonautonomous control problem is divided in two parts by using a numerically formulated feedback linearization, i.e., by devising 1) a nonlinear control (reference) trajectory and 2) a linear control about the reference trajectory. An ad hoc feedback law that forces the perturbed system to follow the reference trajectory is derived by using a linearized variational model. The controller is then tested, through computer simulations, for large deviations of the model parameters on the nonlinear model. The relevant flight data are also presented and compared to the reference values to demonstrate the validity and robustness of the control law, which provided a maximum libration amplitude of less than 4 deg and a final tether velocity of less than 0.02 m/s. C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI & APPLICAT SYST OFF,HUNTSVILLE,AL 35812. UNIV PADUA,DEPT ENGN MECH,I-35100 PADUA,ITALY. RP Lorenzini, EC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,RADIO & GEOASTRON DIV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 37 Z9 43 U1 0 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD SEP-OCT PY 1996 VL 19 IS 5 BP 1148 EP 1156 DI 10.2514/3.21757 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA VE513 UT WOS:A1996VE51300022 ER PT J AU McDiarmid, RW Toure, T Savage, JM AF McDiarmid, RW Toure, T Savage, JM TI Proper name of the neotropical tree boa often referred to as Corallus enydris (Serpentes: Boidae) SO JOURNAL OF HERPETOLOGY LA English DT Article AB Confusion regarding the application of the proper scientific name for the common Neotropical tree boa has existed since Linnaeus described Boa enydris and Boa hortulana in 1758. We review the nomenclatural history of the species and point out the misapplication of scientific names that have characterized this form. Our review indicates that the proper scientific name for this highly variable, wide-ranging arboreal bold is Corallus hortulanus, not Corallus enydris, as has been used so frequently in recent years. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560. UNIV MIAMI,DEPT BIOL,CORAL GABLES,FL 33124. RP McDiarmid, RW (reprint author), NATL MUSEUM NAT HIST,NATL BIOL SERV,WASHINGTON,DC 20560, USA. NR 65 TC 3 Z9 4 U1 0 U2 2 PU SOC STUD AMPHIBIANS REPTILES PI OXFORD PA DEPT OF ZOOLOGY MIAMI UNIV, OXFORD, OH 45056 SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD SEP PY 1996 VL 30 IS 3 BP 320 EP 326 DI 10.2307/1565168 PG 7 WC Zoology SC Zoology GA VH539 UT WOS:A1996VH53900003 ER PT J AU Munson, L Brown, JL Bush, M Packer, C Janssen, D Reiziss, SM Wildt, DE AF Munson, L Brown, JL Bush, M Packer, C Janssen, D Reiziss, SM Wildt, DE TI Genetic diversity affects testicular morphology in free-ranging lions (Panthera leo) of the Serengeti Plains and Ngorongoro Crater SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID CONSEQUENCES; FLORIDA; CHEETAH; AFRICAN AB Reduced genetic variability is known to adversely affect ejaculate quality in inbred lions (Panthera leo) physically isolated in the Ngorongoro Crater compared with outbred lions inhabiting the adjacent Serengeti Plains in East Africa. This study compared the histomorphology of testicular biopsies from these two lion populations. Ngorongoro Crater lions had fewer (P<0.05) seminiferous tubules with spermiogenesis and fewer (P<0.05) spermatids per seminiferous tubular cross-section than Serengeti Plains lions, although seminiferous tubular diameter did not differ (P>0.05) between populations. Interstitial areas were greater (P<0.05) in Crater than in Plains lions, but no qualitative differences were evident, suggesting that proportionately less testicular area was occupied by seminiferous tubules in Crater lions. None of the lions ir,either population had evidence of testicular degeneration. Overall results suggest that inbred Crater lions have reduced spermiogenesis and less total seminiferous tubular area per testis. These data further support the premise that genetic homogeneity compromises reproductive traits in free-living, male African lions. C1 SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. UNIV MINNESOTA,MINNEAPOLIS,MN 55455. ZOOL SOC SAN DIEGO,DEPT VET SCI,SAN DIEGO,CA 92112. RP Munson, L (reprint author), UNIV TENNESSEE,COLL VET MED,DEPT PATHOL,POB 1071,KNOXVILLE,TN 37901, USA. NR 24 TC 21 Z9 22 U1 2 U2 22 PU J REPROD FERTIL INC PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE, ENGLAND CB5 8DT SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD SEP PY 1996 VL 108 IS 1 BP 11 EP 15 PG 5 WC Reproductive Biology SC Reproductive Biology GA VT285 UT WOS:A1996VT28500002 PM 8958822 ER PT J AU MacLeod, KG Irving, AJ AF MacLeod, KG Irving, AJ TI Correlation of cerium anomalies with indicators of paleoenvironment SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article ID RARE-EARTH ELEMENTS; REDOX CONDITIONS; SEA SEDIMENTS; SEAWATER; DISTRIBUTIONS; EXTINCTION; CALIFORNIA; OXIDATION; PARTICLES; CHEMISTRY AB Among 21 whole-rock samples of the Upper Cretaceous Niobrara Formation from Colorado, the abundance of cerium relative to other rare earth elements (Ce anomaly), the weight percent organic carbon (%C-org), and the intensity of bioturbation all covary. This covariation is provocative because %C-org and intensity of bioturbation track changes in the concentration of oxygen in the local water column at the time of deposition (Savrda and Bottjer 1989). Ce anomalies in apatite-rich fractions of the Maastrichtian Zumaya-Algorta Formation from France and Spain and the Miocene Monterey Formation from California show changes that also may coincide with changes in ancient oxygen levels, Our results for the Niobrara samples are the closest correspondence demonstrated between paleo-redox conditions and Ce anomalies, but we cannot yet determine whether the correspondence reflects a cause-and effect relationship, Variation in Ce anomalies is influenced by a number of factors, including terrigenous input, depositional environment, and diagenetic conditions. Potential interplay of these factors prevents a unique interpretation of our whole-rock data; dissecting whole-rock Ce anomalies through analysis of isolated sedimentary components, though, is a promising avenue of research. C1 UNIV WASHINGTON, DEPT GEOL SCI, SEATTLE, WA 98195 USA. RP MacLeod, KG (reprint author), SMITHSONIAN INST, DEPT PALEOBIOL, MRC NHB 121, WASHINGTON, DC 20560 USA. RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 NR 48 TC 35 Z9 37 U1 2 U2 6 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 1527-1404 EI 1938-3681 J9 J SEDIMENT RES JI J. Sediment. Res. PD SEP PY 1996 VL 66 IS 5 BP 948 EP 955 PN A PG 8 WC Geology SC Geology GA VM107 UT WOS:A1996VM10700010 ER PT J AU Bush, M Beck, BB Dietz, J Baker, A James, AE Pissinatti, A Phillips, LG Montali, RJ AF Bush, M Beck, BB Dietz, J Baker, A James, AE Pissinatti, A Phillips, LG Montali, RJ TI Radiographic evaluation of diaphragmatic defects in golden lion tamarins (Leontopithecus rosalia rosalia): Implications for reintroduction SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE golden lion tamarin; Leontopithecus rosalia rosalia; inverted contrast peritonealogram; diaphragmatic defect; eventration; reintroduction; free living ID PRENATAL-DIAGNOSIS; HERNIA; MARMOSETS; HEPATITIS; GENE AB Diaphragmatic defects of suspected familial origin have been documented in captive golden lion tamarins (Leontopithecus rosalia rosalia). This defect was of concern to a multidisciplinary reintroduction program. Plain radiographs taken prior to reintroduction failed to identify an individual with a hernia. A radiographic technique using an inverted contrast peritonealogram was developed using an i.p. injection of radiopaque contrast medium to outline the abdominal contour of-the diaphragm when the anesthetized tamarin was in an inverted (head down) position. The inverted contrast peritonealogram was used to evaluate the diaphragmatic contours of 260 golden lion tamarins (155 from the National Zoological Park, Washington, D.C., 10 from the Rio de Janeiro Primate Center, and 95 free-living in the Poco das Antas Reserve, Brazil). The diaphragmatic contours ranged from smooth and symmetrical to variations of a wavy appearance, out-pocketing, and/or differential elevations of the hemidiaphragm. No true diaphragmatic hernias were detected, but the more severe abnormalities in the diaphragmatic contour were consistent with eventration of the diaphragm. The diaphragmatic contours were graded from 0 to 5 based on the type and degree of irregularity present. The highest grade observed in the 95 free-living golden lion tamarins was 3, seen in only two individuals (3%) compared with 55 individuals (35%) with a grade 3 at the National Zoological Park. This comparison precipitated the decision that no golden lion tamarin with a diaphragmatic contour of grade 4 or 5 (considered a major defect) would be reintroduced. This decision was made in an attempt to minimize the effect of the potential deleterious diaphragmatic defect on survival of this species in the wild. C1 SMITHSONIAN INST,DEPT MAMMAL,WASHINGTON,DC 20008. SMITHSONIAN INST,DEPT PATHOL,WASHINGTON,DC 20008. UNIV MARYLAND,COLLEGE PK,MD 20742. PHILADELPHIA ZOOL GARDEN,DEPT ZOOL,PHILADELPHIA,PA 19104. NATL ACAD SCI,INST MED,WASHINGTON,DC 20428. FDN ESTADUAL ENGN RIO DE JANEIRO,CTR PRIMATOL,RIO JANEIRO,BRAZIL. SMITHSONIAN INST,DEPT ANIM HLTH,WASHINGTON,DC 20008. NR 39 TC 4 Z9 4 U1 1 U2 11 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD SEP PY 1996 VL 27 IS 3 BP 346 EP 357 PG 12 WC Veterinary Sciences SC Veterinary Sciences GA VN204 UT WOS:A1996VN20400006 ER PT J AU Bush, M AF Bush, M TI A technique for endotracheal intubation of nondomestic bovids and cervids SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE nondomestic bovid and cervid; endotracheal intubation; endotracheal tube exchanger; ''Murphy eye'' endotracheal tube AB A simple, rapid method of endotracheal intubation of nondomestic bovids and cervids uses a human endotracheal tube exchanger (19 Fr. X 80 cm) placed in the trachea during direct visualization with a straight long-bladed laryngoscope. A ''Murphy eye'' endotracheal tube can be placed into the trachea by placing the exchanger through the ''eye'' of the tube. The lubricated tube is passed along the exchanger toward the trachea. Passage into the trachea is facilitated by advancing and slightly rotating the endotracheal tube when the animal exhales. RP Bush, M (reprint author), SMITHSONIAN INST,CONSERVAT & RES CTR,NATL ZOOL PK,1500 REMOUNT RD,FRONT ROYAL,VA 22630, USA. NR 9 TC 7 Z9 9 U1 0 U2 1 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD SEP PY 1996 VL 27 IS 3 BP 378 EP 381 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA VN204 UT WOS:A1996VN20400010 ER PT J AU Bush, M Raath, JP deVos, V Stoskopf, MK AF Bush, M Raath, JP deVos, V Stoskopf, MK TI Serum oxytetracycline levels in free-ranging male African elephants (Loxodonta africana) injected with a long-acting formulation SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE African elephants (Loxodonta africana); long-acting oxytetracycline; body measurements; therapeutic serum concentrations ID PHARMACOKINETICS AB Thirteen adult free-living male African elephants (Loxodonta africana) were anesthetized and given 20-100 g of a long-acting oxytetracycline (OTC) preparation either i.m. or i.v. Five dosages were established based on body measurements (the sum of the body length and the girth in centimeters). Serum concentrations of OTC were measured 48 hr after injection. Serum concentrations greater than or equal to 0.5 mu g/ml were measured in 11 of 12 elephants receiving OTC dosages of 52-133 mg/cm either i.v. or i.m. The i.m. administration route produced serum concentrations from 0.75-1.6 mu g/ml in four of four elephants. A dosage of 60-80 mg/cm i.m. or i.v. should provide a therapeutic serum concentration of OTC for at least 48 hr. The use of an i.v. catheter avoids multiple i.m. injections of large drug volumes. C1 KRUGER NATL PK,NATL PK BOARD,ZA-1350 SKUKUZA,SOUTH AFRICA. N CAROLINA STATE UNIV,ENVIRONM MED CONSORTIUM,RALEIGH,NC 27606. RP Bush, M (reprint author), SMITHSONIAN INST,CONSERVAT & RES CTR,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. NR 16 TC 10 Z9 10 U1 0 U2 4 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD SEP PY 1996 VL 27 IS 3 BP 382 EP 385 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA VN204 UT WOS:A1996VN20400011 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI The essential Gombrich: Selected writings on art and culture - Woodfield,R SO LIBRARY JOURNAL LA English DT Book Review RP Kalfatovic, MR (reprint author), SMITHSONIAN INST LIB,ARLINGTON,VA, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 1996 VL 121 IS 14 BP 174 EP 174 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VF870 UT WOS:A1996VF87000043 ER PT J AU Riley, SM AF Riley, SM TI Letting loose - Leland,CT SO LIBRARY JOURNAL LA English DT Book Review RP Riley, SM (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 1996 VL 121 IS 14 BP 210 EP 210 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VF870 UT WOS:A1996VF87000231 ER PT J AU Peled, S Jolesz, FA Tseng, CH Nascimben, L Albert, MS Walsworth, RL AF Peled, S Jolesz, FA Tseng, CH Nascimben, L Albert, MS Walsworth, RL TI Determinants of tissue delivery for Xe-129 magnetic resonance in humans SO MAGNETIC RESONANCE IN MEDICINE LA English DT Article DE xenon; MRI; NMR ID XENON; BLOOD; GAS; NMR; LIQUIDS; HE-3 AB Magnetic resonance imaging using laser-polarized Xe-129 is a new technique first demonstrated by Albert et al, (Nature 370, 1994) who obtained a Xe-129 image of an excised mouse lung, This paper describes the factors influencing the accumulation of inhaled, polarized Xe-129 in human tissue, The resulting model predicts the Xe-129 magnetization in different tissues as a function of the time from the start of inhalation, the tissue perfusion rate and partition coefficient for xenon, and the relevant T-1 decay times, The relaxation times of Xe-129 in biological tissues are not yet known precisely, Substitution of estimated values for these parameters results in an expected signal-to-noise ratio (SNR) from polarized Xe-129 MR in the brain of approximately 2% of the equivalent SNR from proton MR. C1 MIT,DIV HLTH SCI & TECHNOL,BOSTON,MA. HARVARD SMITHSONIAN CTR ASTROPHYS,BOSTON,MA. HARVARD UNIV,SCH MED,DEPT RADIOL,BOSTON,MA 02115. HARVARD UNIV,SCH MED,DEPT INTERNAL MED,BOSTON,MA 02115. RI Peled, Sharon/F-8590-2015 NR 29 TC 49 Z9 50 U1 0 U2 3 PU WILLIAMS & WILKINS PI BALTIMORE PA 351 WEST CAMDEN ST, BALTIMORE, MD 21201-2436 SN 0740-3194 J9 MAGNET RESON MED JI Magn.Reson.Med. PD SEP PY 1996 VL 36 IS 3 BP 340 EP 344 DI 10.1002/mrm.1910360303 PG 5 WC Radiology, Nuclear Medicine & Medical Imaging SC Radiology, Nuclear Medicine & Medical Imaging GA VE627 UT WOS:A1996VE62700002 PM 8875402 ER PT J AU Herrera, A Jackson, JBC Hughes, DJ Jara, J Ramos, H AF Herrera, A Jackson, JBC Hughes, DJ Jara, J Ramos, H TI Life-history variation in three coexisting cheilostome bryozoan species of the genus Stylopoma in Panama SO MARINE BIOLOGY LA English DT Article ID CORAL-REEF COMMUNITIES; COMPETITIVE NETWORKS; ENCRUSTING ORGANISMS; ABUNDANCE; ECOLOGY; ENVIRONMENTS; INVERTEBRATES; STRATEGIES; FORM AB Life-history variation was studied in three sympatric species of Stylopoma Levinsen [S. spongites (Pallas), S. projecta Canu and Bassler and Stylopoma n. sp. 15] in Panama. Bryozoan colonies were collected from 27 reefs along 300 km of the Caribbean coast of Panama. The distribution and abundance of each species were very patchy, but with broad overlap in occurrence among localities and depths. Nevertheless, species differed considerably in colony size, size at first reproduction and numbers of brooding larvae; implying that interspecific differences in life-history traits may contribute to their coexistence. To examine closely this variation in life-history patterns, we grew, in a common garden experiment, the offspring of the two most common species that were obtained from parent colonies collected from several reefs. There were highly significant differences in growth rates and the timing and extent of sexual reproduction which corresponded well to patterns observed in individuals from the field. Other factors, including size of larvae, extent of secondary zooidal calcification and numbers of avicularia were also correlated with differences in life histories. Despite this additional complexity, however, ecological consequences of trade-offs in life history among modular species such as Stylopoma spp. appear very similar to those among unitary species. C1 DUNSTAFFNAGE MARINE RES LAB, OBAN PA34 4AD, ARGYLL, SCOTLAND. FUNDACIENCIA, CUMANA 6101, VENEZUELA. RP SMITHSONIAN TROP RES INST, APARTADO 2072, BALBOA, PANAMA. NR 32 TC 7 Z9 7 U1 0 U2 3 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD SEP PY 1996 VL 126 IS 3 BP 461 EP 469 DI 10.1007/BF00354628 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA VK870 UT WOS:A1996VK87000012 ER PT J AU Marvin, UB AF Marvin, UB TI Ernst Florens Friedrich Chladni (1756-1827) and the origins of modern meteorite research SO METEORITICS & PLANETARY SCIENCE LA English DT Review AB In 1794, Ernst F. F. Chladni published a 63-page book Uber den Ursprung der von Pallas gefundenen und anderer ihr anlicher Eisenmassen en und uber einige damit in Verbindung stehende Naturer-scheinungen in which he proposed that meteor-stones and iron masses enter the atmosphere from cosmic space and form fireballs as they plunge to Earth. These ideas violated two strongly held contemporary beliefs: (1) fragments of rock and metal do not fall from the sky, and (2) no small bodies exist in space beyond the Moon. From the beginning, Chladni was severely criticised for basing his hypotheses on historical eyewitness reports of falls which others regarded as folk tales and for taking gross liberties with the laws of physics. Eight years later, the study of fallen stones and irons was established as a valid field of investigation. Today, some scholars credit Chladni with founding meteoritics as a science; others regard his contributions as scarcely worthy of mention. Writings by his contemporaries suggest that Chladni's book alone would not have led to changes of prevailing theories; thus, he narrowly escaped the fate of those scientists who propose valid hypotheses prematurely. However between 1794 and 1798, four falls of stones were witnessed and widely publicized. There followed a series of epoch-making analyses of fallen stones and ''native irons'' by the chemist Edward C. Howard and the mineralogist Jacques-Louis de Bournon. They showed that all the stones were much alike in texture and composition but significantly different from the Earth's known crustal rocks. Of primary importance was Howard's discovery of nickel in the irons and the metal grains of the stones. This linked the two as belonging to the same natural phenomenon. The chemical results, published in 1802 February, persuaded leading scientists in England, France, and Germany that bodies fall from the sky. Within a few months, chemists in France reported similar results and a new field of study was inaugurated internationally-although opposition lingered on until 1803 April, when nearly 3,000 stones fell at L'Aigle in Normandy and transformed the last skeptics into believers. Chladni immediately received full credit for his hypothesis of falls, but decades passed before his linking of falling bodies with fireballs received general acceptance. His hypothesis of their origin met with strong resistance from those who argued that stones formed within the Earth's atmosphere or were ejected by lunar volcanoes, After 1860, when both of these hypotheses were abandoned, there followed a century of debate between proponents of an interstellar vs. a planetary origin. Not until the 1950s did conclusive evidence of their elliptical orbits establish meteorite parent bodies as members of the solar system. Thus, nearly 200 years passed before the questions of origin that Chladni raised finally were resolved. RP Marvin, UB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 151 TC 21 Z9 21 U1 1 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 1996 VL 31 IS 5 BP 545 EP 588 PG 44 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA VJ141 UT WOS:A1996VJ14100003 ER PT J AU Ivanov, AV MacPherson, GJ Zolensky, ME Kononkova, NN Migdisova, LF AF Ivanov, AV MacPherson, GJ Zolensky, ME Kononkova, NN Migdisova, LF TI The Kaidun meteorite: Composition and origin of inclusions in the metal of an enstatite chondrite clast SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CHEMISTRY; BEARING AB Metal nodules are one of the major textural components of Kaidun sample #01.3.06 EH3-4. In terms of structure, the nodules are of three types: (1) globular, (2) zoned with a massive core and globular mantle, and (3) nodules with no internal structure. The size and composition of the globules in the nodules and grains of metal of the matrix are almost identical: no greater than 20 mu m and Ni, 5.95; Si, 3.33 wt%. The nodules contain small (usually <5 mu m) inclusions of SiO2; albitic glass; enstatite; roedderite; and a mixture of SiO2 and Na2S2. This is the first reported occurrence of a simple sulfide of an alkaline metal in nature. The formation of the inclusions appears to be related to condensation of material onto the surfaces of metal grains. The nodules appear to have formed by aggregation of separate grains (globules) of metal, with conservation of condensates on the grain surfaces as inclusions. The inclusions probably condensed over a significant temperature range from 1400 to 600 K. The aggregation of metal grains and formation of the nodules probably occurred simultaneously with condensation. C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. NASA,LYNDON B JOHNSON SPACE CTR,DIV EARTH SCI & SOLAR SYST EXPLORAT,HOUSTON,TX 77058. RP Ivanov, AV (reprint author), RUSSIAN ACAD SCI,VI VERNADSKII INST GEOCHEM & ANALYT CHEM,MOSCOW 117975,RUSSIA. NR 23 TC 19 Z9 20 U1 2 U2 4 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 1996 VL 31 IS 5 BP 621 EP 626 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA VJ141 UT WOS:A1996VJ14100006 ER PT J AU Wood, JA AF Wood, JA TI Processing of chondritic and planetary material in spiral density waves in the nebula SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID PRIMITIVE SOLAR NEBULA; MAIN-SEQUENCE STARS; TURBULENT CONVECTION; CHONDRULE FORMATION; DISKS; SHOCK; DUST AB A widely held view of nebular evolution is that during the similar to 0.5 Ma while interstellar material was collapsing onto the disk, the latter grew in mass to the point of gravitational instability. It responded to this by losing axial symmetry, growing spiral arms that had the capacity to tidally redistribute disk mass (inward) and angular momentum (outward) and prevent further increase in the disk/protosun mass ratio. The spiral arms (density waves) rotated differently than the substance of the nebula, and in some parts of the disk, nebular material may have encountered the arms at supersonic velocities. The disk gas, and solid particles entrained in it, would have been heated to some degree when they passed through shock fronts at the leading edges of the spiral arms. The present paper proposes this was the energetic nebular setting or environment that has long been sought, in which the material now in the planets and chondritic meteorites was thermally processed. RP Wood, JA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 35 TC 40 Z9 40 U1 1 U2 3 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 1996 VL 31 IS 5 BP 641 EP 645 PG 5 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA VJ141 UT WOS:A1996VJ14100009 ER PT J AU Simon, C Nigro, L Sullivan, J Holsinger, K Martin, A Grapputo, A Franke, A McIntosh, C AF Simon, C Nigro, L Sullivan, J Holsinger, K Martin, A Grapputo, A Franke, A McIntosh, C TI Large differences in substitutional pattern and evolutionary rate of 12S ribosomal RNA genes SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE rate variation; 12S rRNA; Drosophila; Magicicada ID MITOCHONDRIAL-DNA EVOLUTION; ORIENTAL SPECIES SUBGROUPS; NUCLEOTIDE-SEQUENCE; RESTRICTION ENDONUCLEASES; PHYLOGENETIC ANALYSIS; MAXIMUM-LIKELIHOOD; DROSOPHILA; DIVERGENCE; MELANOGASTER; RELIABILITY AB We demonstrate using Drosophila, periodical cicadas, and hominid primates, that the molecular clock based on animal mitochondrial small-subunit (12S) rRNA genes ticks at significantly different relative rates depending on which taxa and which region of the gene are examined. Drosophila, which are commonly used as model taxa, are evolving in a highly peculiar manner with the majority of sites in the 3' half of the 12S gene apparently invariant. The analogous 3' half of the mitochondrial large-subunit rRNA gene (16S) appears to be similarly constrained. It is surprising that these regions that are already highly constrained in all animals should be even more constrained in Drosophila, especially when the Drosophila mitochondrial genome as a whole does not display a similar rate slowdown. This extreme 12S rate slowdown is not apparent in periodical cicadas or hominid primates and appears to be related to strong structural and functional constraints rather than a depressed mutation rate. Finally, the slow average rate of evolution in the third domain of Drosophila does not imply that the few variable sites lack multiple hits. C1 UNIV PADUA,DEPT BIOL,PADUA,ITALY. UNIV NEVADA,DEPT BIOL SCI,RENO,NV 89557. CANC RES CTR HAWAII,HONOLULU,HI 96813. SMITHSONIAN INST,WASHINGTON,DC 20560. RP Simon, C (reprint author), UNIV CONNECTICUT,DEPT ECOL & EVOLUTIONARY BIOL,U-43,STORRS,CT 06269, USA. RI Holsinger, Kent/A-7435-2009; OI Holsinger, Kent/0000-0003-4312-3804 NR 69 TC 35 Z9 37 U1 0 U2 3 PU SOC MOLECULAR BIOLOGY EVOLUTION PI LAWRENCE PA PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD SEP PY 1996 VL 13 IS 7 BP 923 EP 932 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA VE169 UT WOS:A1996VE16900004 PM 8752001 ER PT J AU Gargas, A DePriest, PT AF Gargas, A DePriest, PT TI A nomenclature for fungal PCR primers with examples from intron-containing SSU rDNA SO MYCOLOGIA LA English DT Article DE 18S rDNA; Eumycota; fungi ID 18S RIBOSOMAL-RNA; GROUP-I INTRONS AB We present a compilation of polymerase chain reaction primers (oligonucleotides) used to amplify and sequence the small subunit of nuclear ribosomal DNA. To simplify use of these primers we designed a nomenclature that defines the location of each relative to Saccharomyces cerevisiae. With these primers we have developed strategies for selectively amplifying the diverse ribosomal DNA repeat types found in lichens; either between symbionts or between ribosomal DNA repeats (often the product of optional group I introns) within an individual fungus. A diversity of primers allows a choice of which small subunit ribosomal DNA repeat is amplified or sequenced from a complex extract such as that derived from lichens. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560. RI DePriest, Paula/K-6633-2015 NR 10 TC 110 Z9 111 U1 0 U2 10 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 SN 0027-5514 J9 MYCOLOGIA JI Mycologia PD SEP-OCT PY 1996 VL 88 IS 5 BP 745 EP 748 DI 10.2307/3760969 PG 4 WC Mycology SC Mycology GA VN242 UT WOS:A1996VN24200009 ER PT J AU Rieger, JF AF Rieger, JF TI Body size, litter size, timing of reproduction, and juvenile survival in the Uinta ground squirrel, Spermophilus armatus SO OECOLOGIA LA English DT Article DE Spermophilus armatus; timing of reproduction; maternal allocation; juvenile mass; litter size ID CLUTCH-SIZE; NUMBER; WEIGHT; MASS AB The timing of reproduction affected litter size, offspring mass, and offspring survival in the Uinta ground squirrel, Spermophilus armatus, in Grand Teton National Park, Wyoming. Survival of juvenile females to yearling age varied negatively with date of weaning and positively with individual offspring mass. At the same time, juveniles weaned early in the season were lighter, and juveniles weaned later in the season were heavier. The coefficient of variation for juvenile body mass, originally measured at weaning, significantly decreased by the time juveniles entered hibernation, indicating that individuals weaned early and light ''caught up'' in body mass to individuals weaned later and heavier. From the perspective of the mother's investment in the litter, litter size (corrected for mother's mass) decreased with later weaning dates, while the relationship of weaning date to litter mass (corrected for mother's mass) was significant in only one year. Maternal allocation of resources in litters changed over the season so that mothers produced many, small offspring early in the season, and fewer, large offspring late in the season. C1 NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. NR 30 TC 31 Z9 36 U1 1 U2 11 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD SEP PY 1996 VL 107 IS 4 BP 463 EP 468 DI 10.1007/BF00333936 PG 6 WC Ecology SC Environmental Sciences & Ecology GA VH672 UT WOS:A1996VH67200007 PM 28307388 ER PT J AU Forrey, RC You, L Kharchenko, V Dalgarno, A AF Forrey, RC You, L Kharchenko, V Dalgarno, A TI Index of refraction of noble gases for sodium matter waves SO PHYSICAL REVIEW A LA English DT Article AB We present a theoretical study of the index of refraction of the light noble gases He and Ne for the propagation of sodium matter waves. Our approach is based on the well known multiple scattering theory inside a medium, which leads to an approximation for the index of refraction that depends only on the single forward scattering amplitude and the density distribution functions for the atoms of the medium. The forward scattering amplitude between a sodium atom and a noble gas atom is calculated from molecular potential curves using the eikonal approximation. An explicit phase space average is performed over the noble gas atom distribution in the medium. Our results show very good agreement with the recent interferometry measurements of Schmiedmayer er al. [Phys. Rev. Lett. 74, 1043 (1995)]. Our calculations provide an interpretation of the experimental data, and may shed some light on possibilities for obtaining improved interatomic potentials through atomic interferometry measurements. RP Forrey, RC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 14 TC 25 Z9 25 U1 0 U2 2 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD SEP PY 1996 VL 54 IS 3 BP 2180 EP 2184 DI 10.1103/PhysRevA.54.2180 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA VH090 UT WOS:A1996VH09000058 ER PT J AU Reiss, HR AF Reiss, HR TI Energetic electrons in strong-field ionization SO PHYSICAL REVIEW A LA English DT Article ID NONSEQUENTIAL DOUBLE-IONIZATION; HELIUM; HE AB A strong-field theory is extended to the description of energetic photoelectron spectra. Experimental spectra are accurately described for both linear and circular polarizations, subject only to a single adjustment of reported peak laser intensities. Examined are single and (sequential) double ionization of helium, to energies of about 1 keV. An approximation of the spectrum as a Maxwellian distribution yields a temperature dependent on the spectrometer viewing angle. Final-state Coulomb effects in circular polarization are examined. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. RP Reiss, HR (reprint author), AMERICAN UNIV,DEPT PHYS,WASHINGTON,DC 20016, USA. RI Reiss, Howard/B-6538-2014 OI Reiss, Howard/0000-0003-1023-1462 NR 12 TC 38 Z9 38 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD SEP PY 1996 VL 54 IS 3 BP R1765 EP R1768 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA VH090 UT WOS:A1996VH09000006 ER PT J AU Fern, A AF Fern, A TI The Prime-Ministers: An irreverent political history in cartoons - Baker,K SO PRINT QUARTERLY LA English DT Book Review RP Fern, A (reprint author), SMITHSONIAN INST,NATL PORTRAIT GALLERY,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PRINT QUART LTD PI LONDON PA 80 CARLTON HILL, LONDON, ENGLAND NW8 0ER SN 0265-8305 J9 PRINT Q JI Print Q. PD SEP PY 1996 VL 13 IS 3 BP 325 EP 327 PG 3 WC Art SC Art GA VN530 UT WOS:A1996VN53000008 ER PT J AU Lubar, S AF Lubar, S TI Beyond the history standards + The state of National History Standards SO PUBLIC HISTORIAN LA English DT Article RP Lubar, S (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FAL PY 1996 VL 18 IS 4 BP 145 EP 152 PG 8 WC History SC History GA VZ637 UT WOS:A1996VZ63700008 ER PT J AU Washburn, WE AF Washburn, WE TI The public trust and the first Americans - Knudson,R, Keel,BC SO PUBLIC HISTORIAN LA English DT Book Review RP Washburn, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FAL PY 1996 VL 18 IS 4 BP 153 EP 155 PG 3 WC History SC History GA VZ637 UT WOS:A1996VZ63700009 ER PT J AU Multhauf, RP AF Multhauf, RP TI Operational practice and the emergence of modern chemical concepts SO SCIENCE IN CONTEXT LA English DT Article; Proceedings Paper CT Workshop on Fundamental Concepts of Early Modern Chemistry CY 1995 CL MAX PLANCK INSTITUTE, BERLIN, GERMANY HO MAX PLANCK INSTITUTE AB Both ''early chemistry'' and ''modern concepts'' are imprecise. The earliest references to the materials involved in metallurgy, painting, ceramics, and the like, reveal an awareness that one group of materials were called ''salts'' because of their similarities. I consider this a chemical ''concept.'' Seeking another example I claim to have found it in the so-called ''mineral acids.'' The evidence for the existence of this concept is cumulative during the period just before the emergence of ''modern chemistry,'' of which it may be considered a cause. That evidence is particularly found in the literature of pharmacy and of medicine, both of which belong to the practical arts. C1 SMITHSONIAN INST,WASHINGTON,DC 20560. NR 25 TC 3 Z9 3 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0269-8897 J9 SCI CONTEXT JI Sci. Context PD FAL PY 1996 VL 9 IS 3 BP 241 EP 249 PG 9 WC History & Philosophy Of Science SC History & Philosophy of Science GA WP073 UT WOS:A1996WP07300003 PM 11623475 ER PT J AU Gingevich, O AF Gingevich, O TI Neptune, Velikovsky and the name of the game SO SCIENTIFIC AMERICAN LA English DT Editorial Material RP Gingevich, O (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 2 U2 2 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 SN 0036-8733 J9 SCI AM JI Sci.Am. PD SEP PY 1996 VL 275 IS 3 BP 181 EP & PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VC941 UT WOS:A1996VC94100051 ER PT J AU HEYMAN, IM AF HEYMAN, IM TI SMITHSONIAN PERSPECTIVES + COINS FROM SMITHSON,JAMES BEQUEST CREATED THE INSTITUTION, COMMEMORATIVE COINS FROM THE UNITED-STATES-MINT WILL HELP IT TO CONTINUE SO SMITHSONIAN LA English DT Editorial Material RP HEYMAN, IM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD SEP PY 1996 VL 27 IS 6 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA VF040 UT WOS:A1996VF04000001 ER PT J AU Flint, OS AF Flint, OS TI Studies of neotropical caddisflies LV: Trichoptera of Trinidad and Tobago SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article ID COSTA-RICA; HYDROPTILIDAE; GENUS; HYDROPSYCHIDAE; SMICRIDEA; REVISION; AMERICA AB The caddisfly fauna of these islands now stands at 61 species. Trinidad contains 53 species of which 10 (19%) are endemic, Tobago 33 species of which 7 (21%) are limited to the island, and an additional 6 species (10%) are found on both islands, but not elsewhere. Twelve species are described as new: Cernotina hastilis (Tobago), Austrotinodes adamsae (Tobago), Xiphocentron piscicaudum (Tobago, Venezuela), X. stenotum (Tobago), X. prolixum (Trinidad),Leucotrichia botosaneanui (Trinidad, Tobago), L. tritoven (Trinidad, Tobago, Venezuela), Alisotrichia cyanolenos (Trinidad, Venezuela), Rhyacopsyche duplicispina (Tobago), Ochrotrichia (O.) trinitatis (Trinidad), Ochrotrichia (Metrichia) geminata (Trinidad, Tobago), and Marilia spinosula (Trinidad). Of the insular fauna, 38% is endemic to one or the other or both of the islands, another 5% is shared only with other Antillean islands, a further 18% is shared only with the Paria Peninsula, Venezuela, and the final 39% are more widespread on the Antillean islands and mainland. RP Flint, OS (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 47 TC 22 Z9 22 U1 0 U2 1 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD SEP PY 1996 VL 122 IS 2-3 BP 67 EP 113 PG 47 WC Entomology SC Entomology GA VV422 UT WOS:A1996VV42200001 ER PT J AU Behling, H AF Behling, H TI First report on new evidence for the occurrence of Podocarpus and possible human presence at the mouth of the Amazon during the Late-glacial SO VEGETATION HISTORY AND ARCHAEOBOTANY LA English DT Article DE Late Quaternary; Amazon rain forest; Podocarpus; early Amerindians; sea-level change ID LATE PLEISTOCENE; LAST; VEGETATION; MAXIMUM; BRAZIL AB Palynological studies on late Quaternary lake sediments from the region of the Amazon estuary, 100 km north-east of Belem, Para State, Brazil, enable reconstruction of lowland Amazonian rain forest during the Late-glacial and Holocene periods. Late-glacial forests included populations of Podocarpus which suggests a distinct climatic cooling. Ilex was abundant in the early Holocene. Records of the mangrove taxon, Rhizophora, indicate rapid Atlantic sea-level rise in the beginning of the Holocene. High charcoal representation may reflect the first arrival of Amerindians in the Amazon coastal area, probably about 10 800 B.P. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 26 TC 65 Z9 67 U1 2 U2 4 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0939-6314 J9 VEG HIST ARCHAEOBOT JI Veg. Hist. Archaeobot. PD SEP PY 1996 VL 5 IS 3 BP 241 EP 246 DI 10.1007/BF00217501 PG 6 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA VL609 UT WOS:A1996VL60900005 ER PT J AU Yan, ZC Drake, GWF AF Yan, ZC Drake, GWF TI On the evaluation of two-electron integrals in Hylleraas coordinates SO CHEMICAL PHYSICS LETTERS LA English DT Article ID EXPANSION AB A unified approach is presented for the evaluation of integrals which arise from variational calculations of two-electron atomic systems in Hylleraas coordinates. A scheme is given for calculating the most singular integrals. Our approach is simple to apply, and it significantly improves the numerical stability of existing methods. Some numerical results are tabulated as examples. C1 UNIV WINDSOR,DEPT PHYS,WINDSOR,ON N9B 3P4,CANADA. RP Yan, ZC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Yan, Zong-Chao/F-6668-2014 NR 15 TC 40 Z9 40 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD AUG 30 PY 1996 VL 259 IS 1-2 BP 96 EP 102 DI 10.1016/0009-2614(96)00706-3 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA VE448 UT WOS:A1996VE44800014 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI THE UNREDEEMED CAPTIVE - A FAMILY STORY FROM EARLY AMERICA - DEMOS,J SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TIMES NEWSPAPERS LTD PI LONDON PA PO BOX 479 VIRGINIA ST, LONDON, ENGLAND E1 9XU SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD AUG 30 PY 1996 IS 4874 BP 30 EP 30 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA VE833 UT WOS:A1996VE83300059 ER PT J AU Coats, DW Adam, EJ Gallegos, CL Hedrick, S AF Coats, DW Adam, EJ Gallegos, CL Hedrick, S TI Parasitism of photosynthetic dinoflagellates in a shallow subestuary of Chesapeake Bay, USA SO AQUATIC MICROBIAL ECOLOGY LA English DT Article DE dinoflagellate; parasitism; red tide ID VIRAL MORTALITY; GROWTH-RATES; LIFE-CYCLE; PHYTOPLANKTON; POPULATIONS; SUCCESSION; CERATIUM; ESTUARY; VIRUSES; BLOOMS AB Rhode River (USA) populations of the red-tide dinoflagellates Gymnodinium sanguineum Hirasaka, 1922, Gyrodinium uncatenum Hulburt, 1957, and Scrippsiella trochoidea (Stein) Loeblich III, 1976, were commonly infected by their parasitic relative Amoebophrya ceratii Cachon, 1964, during the summer of 1992. Mean infection levels were relatively low, with data for vertically integrated samples averaging 1.0, 1.9, and 6.5 % for G. sanguineum, G. uncatenum, and S. trochoidea, respectively. However, epidemic outbreaks of A, ceratii (20 to 80 % hosts parasitized) occurred in G. uncatenum and S. trochoidea on several occasions, with peak levels of parasitism associated with decreases in host abundance. Estimates for parasite induced mortality indicate that A. ceratii is capable of removing a significant fraction of dinoflagellate biomass, with epidemics in the upper estuary cropping up to 54 % of the dominant bloom-forming species, G. uncatenum, daily. However, epidemics were usually geographically restricted and of short duration, with daily losses for the 3 host species due to parasitism averaging 1 to 3 % over the summer. Thus, A. ceratii appears capable of exerting a controlling influence on bloom-forming dinoflagellates of the Rhode River only when conditions are suitable for production of epidemic infections. Interestingly, epidemics failed to occur in multiple dinoflagellate taxa simultaneously, even when alternate host species were present at high densities. This observation, along with laboratory experiments demonstrating that parasites isolated from G. sanguineum were unable to infect G. uncatenum, S. trochoidea, and Ceratium furca, suggests that the dinoflagellate taxon A. ceratii may represent a cluster of relatively host-specific species. RP Coats, DW (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. OI Gallegos, Charles/0000-0001-5112-0166 NR 35 TC 68 Z9 73 U1 3 U2 9 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0948-3055 J9 AQUAT MICROB ECOL JI Aquat. Microb. Ecol. PD AUG 29 PY 1996 VL 11 IS 1 BP 1 EP 9 DI 10.3354/ame011001 PG 9 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA VF810 UT WOS:A1996VF81000001 ER PT J AU Zhang, T Yan, ZC Drake, GWF AF Zhang, T Yan, ZC Drake, GWF TI QED corrections of O(mc(2)alpha(7)ln alpha) to the fine structure splittings of helium and He-like ions SO PHYSICAL REVIEW LETTERS LA English DT Article ID STATES; ENERGIES AB A reformulation of the external potential Bethe-Salpeter formalism is developed for two-electron atoms. QED and relativistic corrections to energy levels of order alpha(7)mc(2)In alpha are derived and expressed in terms of expectation values of nonrelativistic operators. Corrections of order alpha(7)mc(2) from exchange diagrams are also found. The total contributions of order alpha(7)mc(2)In alpha to the 1s2p P-3(j) fine structure intervals of helium are Delta nu(01) = 82.6 kHz and Delta nu(12) = - 10.0 kHz. Results are given for He-like ions up to Z = 12 and compared with experiment. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOL PHYS,CAMBRIDGE,MA 02138. RP Zhang, T (reprint author), UNIV WINDSOR,DEPT PHYS,WINDSOR,ON N9B 3P4,CANADA. RI Yan, Zong-Chao/F-6668-2014 NR 26 TC 57 Z9 57 U1 0 U2 4 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 26 PY 1996 VL 77 IS 9 BP 1715 EP 1718 DI 10.1103/PhysRevLett.77.1715 PG 4 WC Physics, Multidisciplinary SC Physics GA VD430 UT WOS:A1996VD43000014 ER PT J AU Tuross, N AF Tuross, N TI Distribution and patterning of proteins and amino acids in paleolithic soils: A study across space and time SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20008. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 25 PY 1996 VL 212 BP 42 EP GEOC PN 1 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA VA915 UT WOS:A1996VA91501982 ER PT J AU Baker, MT Bezur, A AF Baker, MT Bezur, A TI Micro-ATR analysis of polyurethane binders in museum videotape collections: Natural aging reactions in archive tapes SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 25 PY 1996 VL 212 BP 44 EP POLY PN 2 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA VB009 UT WOS:A1996VB00900897 ER PT J AU Bi, SP Correll, DL AF Bi, SP Correll, DL TI A review of the determination of aluminium in food and drinking waters SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 NANJING UNIV,DEPT CHEM,NANJING 210093,PEOPLES R CHINA. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 25 PY 1996 VL 212 BP 44 EP AGFD PN 1 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA VA915 UT WOS:A1996VA91500044 ER PT J AU Campbell, BA Shepard, MK AF Campbell, BA Shepard, MK TI Lava flow surface roughness and depolarized radar scattering SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PISGAH VOLCANIC FIELD; CALIFORNIA; IMAGES; MODEL; CALIBRATION; INVERSION; VENUS AB Surface roughness has a strong controlling influence on radar scattering and other types of remote sensing observations. We compare field measurements of surface topography and dielectric constant for a range of lava flow textures to aircraft multipolarization radar observations at 5.7, 24, and 68 cm (C, L, and P band) wavelengths. The roughness is found to vary with scale in a;self-affine (fractal) manner for scale lengths between 25 cm (the smallest horizontal step size) and 3-5 m. This result is used to demonstrate that a two-component surface description, consisting of the fractal dimension and rms height or slope at some reference scale, can resolve some of the ambiguities in previous efforts to quantify roughness. At all three radar wavelengths, the HV backscatter cross section is found to vary in an approximately exponential fashion with the rms height or Allan deviation at some reference scale, up to a saturation point, where the surface appears entirely diffusely scattering to the radar. Based on these observations, we use a parameter, gamma, defined as the ratio of rms height to the particular scale of measurement. Backscatter values at 24-cm wavelength and the topographic profile data were used to derive expressions which link the HV radar cross section to gamma or to the analogous wavelength-scale rms slope. These equations provide a reasonable fit to 24- and 68-cm echoes and for rough surfaces at 5.7 cm, but yield poor results for 5.7-cm echoes on smooth terrain. We conclude that the roughness at the two larger scales is well described by a single fractal dimension and rms height, but that texture at very small scales is characterized by different statistics. This inference is supported by analysis of 5-cm horizontal spacing topographic profiles. The relationships defined here allow determination of the surface rms height or slope at the scale of the radar wavelength. Given radar data at additional wavelengths, a more complete view of the statistical properties of the surface can be developed. Such techniques may be useful in analyses of synthetic aperture radar images for terrestrial volcanic areas, Magellan data for Venus, and other planetary radar observations. C1 BLOOMSBURG UNIV,DEPT GEOG & EARTH SCI,BLOOMSBURG,PA 17815. RP Campbell, BA (reprint author), SMITHSONIAN INST,CTR EARTH & PLANETARY STUDIES,MRC 315,WASHINGTON,DC 20560, USA. NR 30 TC 47 Z9 49 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 25 PY 1996 VL 101 IS E8 BP 18941 EP 18951 DI 10.1029/95JE01804 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA VE400 UT WOS:A1996VE40000005 ER PT J AU Dingus, BL Bertsch, DL Digel, SW Esposito, JA Fichtel, CE Fierro, JM Hartman, RC Hunter, SD Kanbach, G Kniffen, DA Lin, YC Mattox, JR MayerHasselwander, HA Michelson, PF vonMontigny, C Mukherjee, R Nolan, PL Schneid, E Sreekumar, P Thompson, DJ Willis, TD AF Dingus, BL Bertsch, DL Digel, SW Esposito, JA Fichtel, CE Fierro, JM Hartman, RC Hunter, SD Kanbach, G Kniffen, DA Lin, YC Mattox, JR MayerHasselwander, HA Michelson, PF vonMontigny, C Mukherjee, R Nolan, PL Schneid, E Sreekumar, P Thompson, DJ Willis, TD TI Egret observations of gamma rays from point sources with galactic latitude -30 degrees 1 to 3 million years later still, Because Mg-26*-containing and Mg-26*-free chondrules are both found in Chainpur, which was not heated to more than similar to 400 degrees C, it follows that parent body metamorphism cannot explain the absence of Mg-26* in some of these chondrules. Rather, its absence indicates that the lifetime of the solar nebula over which CAls and chondrules formed extended over similar to 5 million years. C1 CALTECH,DIV GEOL & PLANETARY SCI,LUNAT ASYLUM,PASADENA,CA 91125. RP Russell, SS (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT MINERAL SCI,MRC NHB-119,WASHINGTON,DC 20560, USA. RI WASSERBURG, GERALD /F-6247-2011 NR 35 TC 192 Z9 195 U1 0 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD AUG 9 PY 1996 VL 273 IS 5276 BP 757 EP 762 DI 10.1126/science.273.5276.757 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA VB429 UT WOS:A1996VB42900030 ER PT J AU Morse, JA Blair, WP Dopita, MA Hughes, JP Kirshner, RP Long, KS Raymond, JC Sutherland, RS Winkler, PF AF Morse, JA Blair, WP Dopita, MA Hughes, JP Kirshner, RP Long, KS Raymond, JC Sutherland, RS Winkler, PF TI Hubble Space Telescope observations of oxygen-rich supernova remnants in the Magellanic cloud .1. Narrow-band imaging of N132D in the LMC SO ASTRONOMICAL JOURNAL LA English DT Article ID X-RAY; SHOCK-WAVES; INTERSTELLAR CLOUDS; NOVA REMNANT; YOUNG; EMISSION; SPECTROSCOPY; CASSIOPEIA; KINEMATICS; DISTANCE AB We present Hubble Space Telescope (HST) WFPC2 images of the young, oxygen-rich supernova remnant N132D in the Large Magellanic Cloud in the [O III]lambda 5007, [O II]lambda lambda 3727 and [S II]lambda lambda 6724 emission lines, plus a visible continuum band. The similar to 0.'' 1 resolution of HST allows us to analyze structure within N132D at scales comparable to ground based images of nearby remnants such as Cas A. The oxygen-rich filaments (seen in [O III] and [O II] emission) are easily distinguished from shocked circumstellar clouds (seen in all three emission lines). Characteristic knots sizes and filament widths are similar to 0.'' 2-0.'' 5 (similar to 1.5-4x10(17) cm), at least partially resolved in our images. For the first time, we discern ionization structure within the shocked interstellar clouds and filaments, reminiscent of filaments in galactic SNRs that are thought to arise from recent shock/interstellar cloud encounters where the full cooling and recombination zone has not yet formed throughout the structure. Conversely, there appears to be fairly uniform ionization in the O-rich filaments. We also observe highly ionized, diffuse emission extending all the way around the outer edges of the remnant, as previously seen in ground-based studies. We compare our HST optical emission-line images of N132D to the ROSAT HRI soft X-ray image and find that the X-ray emission is closely traced optically by shocked circumstellar clouds; the O-rich filaments do not appear to be emitting X-rays. The limb-brightened X-ray shell aligns remarkably precisely along the inner edge of the diffuse outer rim. The diffuse emission probably represents ambient molecular gas that is being dissociated and photoionized by high-energy photons originating in the fast SNR shocks. We have used the MAPPINGS II code to model the X-ray producing main blast wave as an similar to 800 km s(-1) shock moving into a circumstellar medium of density N-0 approximate to 3 cm(-3). The preshock ISM density of N-0 approximate to 3 cm(-3) inferred from our shock model agrees with the preshock density estimated from the [O III]lambda 5007 surface brightness in the diffuse outer rim. We also model the [O III]/[S II] emission-line ratios in the photoionized outer rim as a function of distance ahead of the main blast wave using the radiation field produced by fast shocks in the remnant as the ionizing source. According to our models, the ionizing radiation from the similar to 800 km s(-1) main blast wave is not sufficient to generate the observed optical emission from the outer rim precursor. An extra source of EUV photons appears necessary to achieve the observed ionization of the preshock gas. We estimate that EUV photons produced in slower shocks moving into QSF-type clouds around the outer rim can probably contribute enough ionizing photons to achieve the observed ionization. Radiative shocks moving through the O-rich filaments may also be an important source of EUV photons. (C) 1996 American Astronomical Society. C1 UNIV COLORADO,DEPT ASTROPHYS PLANETARY & ATMOSPHER SCI,BOULDER,CO 80309. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,WESTON,ACT 2611,AUSTRALIA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. NATL INST STAND & TECHNOL,BOULDER,CO 80309. MIDDLEBURY COLL,DEPT PHYS,MIDDLEBURY,VT 05753. RP Morse, JA (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. RI Dopita, Michael/P-5413-2014 OI Dopita, Michael/0000-0003-0922-4986 NR 52 TC 50 Z9 50 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1996 VL 112 IS 2 BP 509 EP 533 DI 10.1086/118031 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ553 UT WOS:A1996UZ55300014 ER PT J AU Prosser, CF Randich, S Stauffer, JR AF Prosser, CF Randich, S Stauffer, JR TI Photometry in the open clusters IC 2602 and NGC 6475 SO ASTRONOMICAL JOURNAL LA English DT Article ID STANDARD STARS; X-RAY; COUSINS AB CCD photometry has been obtained in the regions of the open clusters IC 2602 and NGC 6475 for the purpose of identifying likely optical counterparts to x-ray sources. Photometry has also been obtained for relatively bright stars in both clusters in order to improve upon previous photometry and to assess membership. In IC 2602, the new candidate members associated with x-ray sources include two visual binary systems with the secondary components being the lowest-mass candidate members identified to date. In NGC 6475, several possible optical counterparts to the strongest x-ray source in the field of the cluster have been given, though the true optical counterpart remains unknown. (C) 1996 American Astronomical Society. C1 EUROPEAN SO OBSERV,D-85748 GARCHING,GERMANY. RP Prosser, CF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS-66,CAMBRIDGE,MA 02138, USA. OI Randich, Sofia/0000-0003-2438-0899 NR 15 TC 26 Z9 26 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1996 VL 112 IS 2 BP 649 EP 654 DI 10.1086/118040 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ553 UT WOS:A1996UZ55300023 ER PT J AU Carney, BW Laird, JB Latham, DW Aguilar, LA AF Carney, BW Laird, JB Latham, DW Aguilar, LA TI A survey of proper motion stars .13. The halo population(s) SO ASTRONOMICAL JOURNAL LA English DT Review ID METAL-POOR STARS; UVBY-BETA-PHOTOMETRY; HORIZONTAL-BRANCH STARS; RR-LYRAE STARS; INTERMEDIATE-BAND PHOTOMETRY; GALACTIC GLOBULAR-CLUSTERS; OXYGEN ABUNDANCES; HIGH-VELOCITY; CHEMICAL-COMPOSITION; IRON ABUNDANCES AB Based on our expanded sample of metallicities and kinematics for a large sample of stars selected from the Lowell Proper Motion Catalog, we study several questions relating to the halo stellar population(s) in our Galaxy. For [m/H] less than or equal to -1.4, there does not seem to be any variation with [m/H] in the mean values of the V velocity (i,e., angular momentum related to that in the disk) or the Galactic orbital eccentricities. Further, in spite of the strong kinematical biases in our sample, stars with very low metallicities are found that have small V velocities (high orbital angular momenta) and low orbital eccentricities. These results contradict the model that the metal-poor stars are a single population that is only the relic of the earliest stages of the Galaxy's collapse. There are signs that some of the metal-poor stars in the solar neighborhood are due to accretion events and, perhaps, also to the earliest stages of the formation of the Galactic disk. Regarding accretion, we confirm Majewski's [ApJS, 78, 87 (1992)] finding of a retrograde rotation among stars that reach 5 kpc or more from the plane. These stars do not show any radial metallicity gradient, and may be younger on average than dynamically hot, metal-poor stars closer to the plane. These latter stars show net prograde rotation and a radial metallicity gradient, suggestive of a dissipative process in the earliest stages of disk formation. The correlation between metallicity and perigalacticon found by Ryan & Norris [AJ, 101, 1835 (1991a)] disappears when care is taken to exclude the stars that may have been accreted by our Galaxy, The field star results complement those for globular clusters found by other workers, notably Zinn (1993), who argued for two populations of metal-poor clusters, one apparently in retrograde rotation with no radial metallicity gradient and slightly younger ages, and the other with prograde rotation, a weak radial metallicity gradient, and slightly older ages, The field stars and globular clusters do differ slightly, however. Their metallicity distributions differ, with the field stars showing a larger fraction of the most metal-poor stars. This could be caused by accretion of Draco dwarf galaxy-like objects, with very low metallicities and no globular clusters, We see in our data, particularly in the V vs [R(apo)] plane, possible signs of large-scale kinematic substructure suggestive of specific accretion events. We also see signs for the Preston er al. [AJ, 108, 538 (1994)] low-metallicity,intermediate kinematics, and younger age stellar population. However, the strength of the signal in our data suggests that a fairly large fraction of its stars may be old. On the other hand, the ''away'' versus ''toward'' mystery of Croswell et al. [AJ, 93, 1445 (1987)] has disappeared: the numbers of stars approaching and receding from the plane agree with expectations. Finally, we point out that the model of Norris [ApJ, 431, 645 (1994)] for a proto-disk population that is hotter dynamically than the accreted halo components does not agree with our expanded data sample. We suggest that the proto-disk component was dynamically cooler when the mean metallicity was very low. (C) 1996 American Astronomical Society. C1 BOWLING GREEN STATE UNIV, DEPT PHYS & ASTRON, BOWLING GREEN, OH 43403 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NATL ASTRON OBSERV, ENSENADA, BAJA CALIFORNIA, MEXICO. RP Carney, BW (reprint author), UNIV N CAROLINA, DEPT PHYS & ASTRON, CHAPEL HILL, NC 27599 USA. NR 118 TC 141 Z9 142 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1996 VL 112 IS 2 BP 668 EP 692 DI 10.1086/118042 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ553 UT WOS:A1996UZ55300025 ER PT J AU Chen, H Ohashi, N Umemoto, T AF Chen, H Ohashi, N Umemoto, T TI High-resolution millimeter imaging of L1641N: Multiple cores with a young stellar group SO ASTRONOMICAL JOURNAL LA English DT Article ID STAR-FORMATION; MOLECULAR CLOUD; IRAS SOURCES; FRAGMENTATION; POPULATION; OUTFLOWS; CLUSTER; DISKS AB We report interferometric imaging of a young stellar group L1641N (IRAS 05338-0624) in the CS J = 3-2 line and the 2-mm continuum. Seven line emission peaks are identified within 0.1 pc of the IRAS position. The physical properties of these peaks (central velocity, linewidth, mass, and density) have been used to infer their nature. We conclude that three of these peaks (1-3) are likely to be real molecular gas condensations. These three cores are closely associated with the stellar group in which young stars have been continuously forming over the last few Myr. They are also more massive than the gas clumps detected interferometerically toward the well-known star forming cores in Taunts, and are thus capable of forming young stellar objects. The different core characteristics (mass, density, and the association with young stellar objects) suggest that these cores are at difference stages of dense core evolution with cores ranging from quiescent preprotostellar to turbulent starless, and to actively star forming. (C) 1996 American Astronomical Society. C1 NATL ASTRON OBSERV,VSOP PROJECT OFF,MITAKA,TOKYO 181,JAPAN. RP Chen, H (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 29 TC 9 Z9 9 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1996 VL 112 IS 2 BP 717 EP 722 DI 10.1086/118046 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ553 UT WOS:A1996UZ55300029 ER PT J AU Evans, NR Teays, TJ AF Evans, NR Teays, TJ TI Temperatures of delta Cep and nonvariable supergiants SO ASTRONOMICAL JOURNAL LA English DT Article ID CEPHEID VARIABLES; ANGULAR DIAMETERS; STARS; ATMOSPHERES; SCALE; DISTRIBUTIONS; CALIBRATION; NITROGEN; CARBON; OXYGEN AB This study is a comparison of the energy distributions of nonvariable supergiants and delta Cep with model atmospheres. The data include IUE spectra from 1700 to 3200 Angstrom, and broadband B, V, R(C), I-C, J, H, and K. The model atmosphere comparisons cover a range of temperatures, gravities, and microturbulence. Both the nonvariables and delta Cep are a good fit to the Kraft (B-V)(0)-temperature relation. The delta Cep observations match energy distributions using reasonable values of gravity and microturbulence. For the hotter phases, a larger gravity is required than for the cooler phases, but this value results in a good fit to energy distribution, including the excess ultraviolet flux found previously. Similarly, the energy distribution for the piston phase can also be reproduced, but a large value of microturbulence (larger than similar or equal to 6 km s(-1)) would be very difficult to accommodate. The most interesting result concerns the nonradiative flux found by Morossi et al. [A&A, 277, 173 (1993)] at the shortest wavelengths. It is found in nonvariable supergiants, however it is nonexistent or much reduced in the delta Cep observations. This suggests an alteration to the atmospheric structure caused by pulsation. This is in agreement with and explains the recent ROSAT observation of the Cepheid zeta Gem by Sasselov & Sabbey [RMxA&A, 29, 215 (1994)]. It was not detected, meaning that it's x-ray flux is at least 20 times less than comparable nonvariable supergiants. Pulsation apparently inhibits upper atmosphere heating, so that a hot corona is not formed. (C) 1996 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. COMP SCI CORP,SCI PROGRAM,LANHAM,MD 20706. RP Evans, NR (reprint author), YORK UNIV,DEPT PHYS & ASTRON,4700 KEELE ST,N YORK,ON M3J 1P3,CANADA. NR 33 TC 12 Z9 12 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1996 VL 112 IS 2 BP 761 EP 771 DI 10.1086/118051 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ553 UT WOS:A1996UZ55300034 ER PT J AU Boulanger, F Abergel, A Bernard, JP Burton, WB Desert, FX Hartmann, D Lagache, G Puget, JL AF Boulanger, F Abergel, A Bernard, JP Burton, WB Desert, FX Hartmann, D Lagache, G Puget, JL TI The dust/gas correlation at high Galactic latitude SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM, atoms; ISM, dust, extinction; ISM, molecules; ISM, general; infrared, interstellar, continuum ID INTERSTELLAR GRAINS; SPECTRAL OBSERVATIONS; OPTICAL-PROPERTIES; INFRARED-EMISSION; GALAXY; CLOUDS; COBE; HYDROGEN AB We have correlated the far-infrared emission from dust as measured by the DIRBE and FIRAS experiments with the 21-cm emission from gas as measured by the Leiden/Dwingeloo survey of HI in our Galaxy. A tight correlation is observed at high [b] at wavelengths ranging from 100 mu m to 1 mm. The dust emission spectrum derived from the correlation is fit well by a single Planck curve characterized by T = 17.5 K and an emissivity proportional to nu(2). The dust emissivity tau/N-H = 1.0 10(-25) (lambda/250 mu m)(-2) cm(2) is remarkably close to the value in the Draine and Lee (1984) dust model and is much smaller than values predicted Eor porous or fractal grains. In the emission from HI gas, we exclude the presence of a very cold dust component with comparable emissivity, unless its temperature is significantly smaller than 7 K. We also discuss the contribution from Galactic molecular and ionized gas to the global IR emission. C1 STERREWACHT LEIDEN, NL-2300 RA LEIDEN, NETHERLANDS. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV PARIS 11, INST ASTROPHYS SPATIALE, BAT 121, F-91405 ORSAY, FRANCE. NR 32 TC 276 Z9 276 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 1996 VL 312 IS 1 BP 256 EP 262 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VC218 UT WOS:A1996VC21800030 ER PT J AU Ramella, M Focardi, P Geller, MJ AF Ramella, M Focardi, P Geller, MJ TI The redshift-space neighborhoods of 13 SSRS groups of galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies, general; galaxies, clusters of; galaxies, redshifts ID 36 LOOSE GROUPS; VELOCITY DISPERSIONS; DENSE CLUSTERS; NEARBY GROUPS; KINEMATICS; CATALOG AB The Southern Sky Redshift Survey includes 13 groups of 5 or more members with velocities greater than or equal to 2000 km s(-1). By measuring redshifts and accumulating data from the literature, we increase the total number of known group members from 89 to 218. We also measured new redshifts for 59 foreground/background galaxies superimposed on the group neighborhoods. The velocity dispersions of the groups are remarkably stable.(1) C1 UNIV BOLOGNA, DIPARTIMENTO ASTRON, I-40126 BOLOGNA, ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Ramella, M (reprint author), OSSERV ASTRON TRIESTE, VIA GB TIEPOLO 11, I-34131 TRIESTE, ITALY. NR 26 TC 13 Z9 13 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 1996 VL 312 IS 3 BP 745 EP 750 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VE344 UT WOS:A1996VE34400008 ER PT J AU Kochanek, CS AF Kochanek, CS TI Is there a cosmological constant? SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology, observations; galaxies, distances and redshifts; galaxies, kinematics and dynamics; galaxies, structure; gravitational lensing ID GRAVITATIONAL LENS SURVEY; ELLIPTICAL POTENTIAL WELLS; NEUTRAL-HYDROGEN CONTENT; MULTIPLY IMAGED QUASARS; HUBBLE SPACE TELESCOPE; EARLY-TYPE GALAXIES; COLD DARK MATTER; INTERSTELLAR MATTER; LUMINOSITY FUNCTION; REDSHIFT SURVEY AB We present limits on the cosmological constant from the statistics of gravitational lenses using newly completed quasar surveys, new lens data, and a range of lens models. The formal limits are lambda(0) < 0.66 at 95% confidence in flat cosmologies (Omega(0) + lambda(0) = 1) and Omega(0) > 0.15 at 90% confidence in open universes (lambda(0) = 0), including the statistical uncertainties in the number of lenses, galaxies, and quasars and the parameters relating galaxy luminosities to dynamical variables. The limit holds for either softened isothermal or de Vaucouleurs models of the lens galaxies, suggesting that the radial mass distribution in the lens galaxy is not a significant systematic uncertainty. The cosmological limits are unaffected by adding a small core radius to the isothermal lens models or by the luminosity of the lens galaxy. Inconsistent models of the effects of a core radius make significant errors in the cosmological constraints. Extinction in E/S0 galaxies can significantly reduce the limits on the cosmological constant, but changing the expected number of lenses by a factor of 2 requires a minimum of 100 times more dust than is observed locally in E/S0 galaxies. Rapid evolution of the lenses is the most promising means of evading these limits. However, a viable model must not only reduce the expected number of lenses but do so without significantly altering the average image separations, magnitudes, and redshifts and the relative properties of optically and radio selected lenses. RP Kochanek, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 110 TC 336 Z9 337 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1996 VL 466 IS 2 BP 638 EP 659 DI 10.1086/177538 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ546 UT WOS:A1996UZ54600004 ER PT J AU Gammie, CF Ostriker, EC AF Gammie, CF Ostriker, EC TI Can nonlinear hydromagnetic waves support a self-gravitating cloud? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, clouds; MHD; stars, formation; waves ID MAGNETIC INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; STAR FORMATION; DARK CLOUDS; ALFVENIC TURBULENCE; EVOLUTION; OPHIUCHUS; (CO)-C-13; MODEL; MAGNETOHYDRODYNAMICS AB Using self-consistent magnetohydrodynamic (MHD) simulations, we explore the hypothesis that nonlinear MHD waves dominate the internal dynamics of galactic molecular clouds. Our models employ an isothermal equation of state and allow for self-gravity. We adopt ''slab symmetry,'' which permits motions upsilon(perpendicular to) and fields B-perpendicular to perpendicular to the mean field, but permits gradients only parallel to the mean field. This is the simplest possible geometry that relies on waves to inhibit gravitational collapse along the mean field. In our simulations, the Alfven speed upsilon(A) exceeds the sound speed c(s) by a factor 3-30, which is realistic for molecular clouds. We simulate the free decay of a spectrum of Alfven waves, both with and without self-gravity. We also perform simulations with and without self-gravity that include small-scale stochastic forcing, meant to model the mechanical energy input from stellar outflows. Our major results are as follows: (1) We confirm that the pressure associated with fluctuating transverse fields can inhibit the mean held collapse of clouds that are unstable by Jeans's criterion. Cloud support requires the energy in Alfven-like disturbances to remain comparable to the cloud's gravitational binding energy. (2) We characterize the turbulent energy spectrum and density structure in magnetically dominated clouds. The perturbed magnetic and transverse kinetic energies are nearly in equipartition and far exceed the longitudinal kinetic energy. The turbulent spectrum evolves to a power-law shape, approximately upsilon(perpendicular to,k)(2) approximate to B-perpendicular to,B-k/4 pi rho proportional to k(-s) with s similar to 2, i.e., approximately consistent with a ''line width-size'' relation sigma(upsilon)(R) proportional to R(1/2). The simulations show large density contrasts, with high-density regions confined in part by the pressure of the huctuating magnetic field. (3) We evaluate the input power required to offset dissipation through shocks, as a function of c(s)/upsilon(A), the velocity dispersion sigma(upsilon), and the characteristic scale lambda of the forcing. In equilibrium, the volume dissipation rate is approximate to 5.5(c(s)/upsilon(A))(1/2)(lambda/L)(-1/2) x rho sigma(upsilon)(3)/L, for a cloud of linear size L and density rho. (4) Somewhat speculatively, we apply our results to a ''typical'' molecular cloud. The mechanical power input required for equilibrium (tens of L.), and the implied star formation efficiency (similar to 1%), are in rough agreement with observations. Because this study is limited to slab symmetry and excludes ion-neutral friction, the dissipation rate we calculate probably provides a lower limit on the true value. RP Gammie, CF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, MS 51, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 80 TC 115 Z9 115 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1996 VL 466 IS 2 BP 814 EP 830 DI 10.1086/177556 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ546 UT WOS:A1996UZ54600022 ER PT J AU Eastman, RG Schmidt, BP Kirshner, R AF Eastman, RG Schmidt, BP Kirshner, R TI The atmospheres of Type II supernovae and the expanding photosphere method SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; stars, atmospheres; stars, distances; supernovae, general ID EXTRAGALACTIC DISTANCE SCALE; LOW-DENSITY PHOTOSPHERES; SPHERICALLY SYMMETRIC FLOWS; LARGE MAGELLANIC CLOUD; LIGHT CURVES; SPECTRAL FLUX; CEPHEID VARIABLES; HUBBLE CONSTANT; MASSIVE STARS; SN-1993J AB The Expanding Photosphere Method (EPM) determines distances to Type II supernova (SNe II) by comparing the photospheric angular size with the expansion velocity measured from spectral lines. The photospheres of SNe II are low density and are dominated by electron scattering, and consequently the photospheric flux is dilute relative to a Planck function at the best-fitting continuum color temperature The reliability of EPM distances depends on understanding how the dilution is related to physical properties of the supernova atmosphere. To study this, we have calculated 63 different model atmospheres relevant to SNe II. The excitation, ionization, and thermal structure are described for the case of high effective temperature in which the atmosphere is completely ionized, and for the case of cooler effective temperatures in which the photosphere is formed in a region of recombining hydrogen. The general spectral features of both cases are discussed. We explore how the computed spectrum changes with density structure, helium abundance, metallicity, expansion rate, and luminosity or effective temperature. The most important variable in determining spectral appearance is the effective temperature. The amount by which the emergent flux is dilute relative to the best-fitting blackbody depends on a number of factors, most important of which are the temperature and, in short-wavelength bandpasses, density at the photosphere. For each of the models we derive distance correction factors for application in EPM, using the four filter combinations {BV}, {VIc}, {BVIc}, and {JHK}. The main differences may be expressed in terms of the observable color temperature and a slowly varying dependence on density. Functional fits to the distance correction factor are provided which can be used to estimate the photospheric angular size from broadband photometry. The effect of uncertain dust extinction on angular size is shown to be small. This work places EPM on a firm theoretical foundation and substantiates the Hubble constant measurement by Schmidt et al. of H-0 = 73 +/- 7. C1 AUSTRALIAN NATL UNIV, MT STROMLO & SIDING SPRING OBSERV, WESTON, ACT 2611, AUSTRALIA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Eastman, RG (reprint author), LAWRENCE LIVERMORE NATL LAB, GEN STUDIES GRP, LIVERMORE, CA 94550 USA. OI Schmidt, Brian/0000-0001-6589-1287 NR 64 TC 122 Z9 124 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1996 VL 466 IS 2 BP 911 EP 937 DI 10.1086/177563 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ546 UT WOS:A1996UZ54600029 ER PT J AU Ohashi, N Hayashi, M Ho, PTP Momose, M Hirano, N AF Ohashi, N Hayashi, M Ho, PTP Momose, M Hirano, N TI Possible infall in the gas disk around L1551-IRS 5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; circumstellar matter; ISM, molecules; ISM, structure; stars, formation; stars, individual (L1551-IRS5); stars, pre-main sequence ID MOLECULAR OUTFLOW; CIRCUMSTELLAR GAS; LINE FORMATION; BIPOLAR FLOWS; DENSE CORES; DM-TAURI; HL TAURI; IRS-5; CO; NGC-2071 AB We report observations of (CO)-C-13(J = 1-0) emission from L1551-IRS5 carried out with the Nobeyama Millimeter Array. We detected a strong and compact condensation associated with L1551-IRS5, and weaker extended components with ''U''-like features with a spatial resolution of 5.'' 1 x 3.'' 9 (P.A. = 159 degrees). The U-like features delineate the edges of the molecular outflow as well as the 2.2 mu infrared reflection nebula. This suggests that the extended component may be a dense shell swept up by the molecular outflow. The compact component was marginally resolved with the present angular resolution. The estimated deconvolved size is similar to 1200 x 670 AU with a position angle perpendicular to the optical jet. This elongated structure is very similar to the compact gaseous disk observed in (CO)-O-18 (J = 1-0). The (CO)-C-13 elongated structure may be more extended than the actually measured size, suggesting that the compact (CO)-C-13 gas is most probably the inner part of the gaseous disk around L1551-IRS5. The (CO)-C-13 disk has a velocity gradient along its minor axis, which can be explained in terms of infalling motion in the plane of the disk with a central mass of 0.5 M.. We estimate the mass accretion rate at 600 AU in radius to be 1.3-2.6 x 10(-5) M. yr(-1). The derived accretion rate might be larger than the accretion rate onto the star estimated from the bolometric luminosity of L1551-IRS5 on the assumption of steady accretion, which suggests that the accretion around L1551-IRS5 may also be nonsteady as was the case for HL Tau. C1 NATL ASTRON OBSERV,SUBARU PROJECT OFF,MITAKA,TOKYO 181,JAPAN. GRAD UNIV ADV STUDIES,NOBEYAMA RADIO OBSERV,DEPT ASTRON SCI,MINAMISA KU,NAGANO 38413,JAPAN. HITOTSUBASHI UNIV,LAB ASTRON & GEOPHYS,KUNITACHI,TOKYO 186,JAPAN. RP Ohashi, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 42 TC 56 Z9 56 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1996 VL 466 IS 2 BP 957 EP & DI 10.1086/177566 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ546 UT WOS:A1996UZ54600032 ER PT J AU Long, KS Blair, WP Hubeny, I Raymond, JC AF Long, KS Blair, WP Hubeny, I Raymond, JC TI Observations of the dwarf nova VW Hydri in quiescence with the Hopkins Ultraviolet Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, close; novae; cataclysmic variables; stars, individual (VW Hydri); ultraviolet, stars ID HUBBLE-SPACE-TELESCOPE; X-RAY-EMISSION; WHITE-DWARF; CATACLYSMIC VARIABLES; U-GEMINORUM; ACCRETION DISKS; RESOLUTION SPECTROSCOPY; BOUNDARY-LAYER; OUTBURSTS; PERFORMANCE AB The dwarf nova VW Hydri was in quiescence when it was observed in 1995 March with the Hopkins Ultraviolet Telescope on the Astro-2 space shuttle mission. The far-UV (820-1840 Angstrom) spectra are punctuated by broad Ly alpha and Ly beta absorption profiles and narrow absorption lines which can be identified with transitions expected in the atmosphere of a moderate-temperature white dwarf. There is no detectable emission shortward of 980 Angstrom. The only emission line seen is C IV lambda lambda 1548, 1551. If the emission from VW Hyi is due to a uniform-temperature white dwarf, then our spectra suggest that the temperature of the white dwarf was similar to 17,000 K at the time of our observations and that abundances in the atmosphere were subsolar. Improved fits to the data are obtained using models in which the far-UV emission arises in part from a white dwarf with near-solar abundances and in part from the accretion disk. However, given the uncertainties in model spectra of metal-enriched atmospheres in this temperature range and our limited knowledge of quiescent accretion disks, higher S/N spectra are needed to unambiguously assess the disk contribution to the far-UV spectrum of VW Hyi in quiescence. C1 JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Long, KS (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 38 TC 9 Z9 9 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1996 VL 466 IS 2 BP 964 EP 972 DI 10.1086/177567 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ546 UT WOS:A1996UZ54600033 ER PT J AU Wang, LF Wheeler, JC Kirshner, RP Challis, PM Filippenko, AV Fransson, C Panagia, N Phillips, MM Suntzeff, N AF Wang, LF Wheeler, JC Kirshner, RP Challis, PM Filippenko, AV Fransson, C Panagia, N Phillips, MM Suntzeff, N TI Hubble Space Telescope spectroscopic observations of the ejecta of SN 1987A at 2000 days SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, individual (SN 1987A); supernova remnants; ultraviolet, stars ID O-I LAMBDA-LAMBDA-6300; FAINT OBJECT CAMERA; SUPERNOVA 1987A; EMISSION-LINES; ULTRAVIOLET OBSERVATIONS; SN-1987A; SATELLITE; PROFILES; CO-57 AB We have used the Faint Object Spectrograph on the Hubble Space Telescope (HST) to observe the spectra of SN 1987A over the wavelength range 2000-8000 Angstrom on dates 1862 and 2210 days after the supernova outburst. Even these pre-COSTAR observations avoid much of the contamination from the bright stars nearby and provide a very useful set of line strengths and shapes for analysis. The spectrum is formed in an unusual physical setting: cold gas that is excited and ionized by energetic electrons from the radioactive debris of the supernova explosion. The spectra of SN 1987A at this phase are surprisingly similar to those of the nova shells of CP Puppis and T Pyxidis decades after outburst. SN 1987A and the novae are characterized by emission from material with electron temperatures of only a few hundred kelvins and show narrow Balmer continuum emission and strong emission Lines from O+. The Balmer continuum shape requires the electron temperature in the supernova ejecta to be as low as 500 K on day 1862 and 400 K on day 2210 after outburst. The [O II] lambda lambda 3726, 3728 doublet is surprisingly strong and is plausibly powered by collisional ionization of neutral oxygen to excited states of O+. The line intensity ratio of the [O I] lambda lambda 6300, 6364 doublet obtained from Gaussian fits of the line profiles is 1.8 +/- 0.2, contrary to the optically thin limit of 3. This ratio is not due to an optical depth effect but, rather, is an artifact of assuming a Gaussian profile to fit the [O I] lambda lambda 6300, 6364 doublet profile. Specifying the line ratio R = F([O I] lambda 6300)/F([O I] lambda 6364) = 3 is consistent with the data and allows a calculation of the decomposed line profile. All the observed strong lines are found to be blueshifted by a similar amount of 400 km s(-1). The line profiles are quite similar for lines arising from different chemical elements. The profiles are all asymmetric, showing redshifted extended tails with velocities up to 10,000 km s(-1) in some strong lines. The blueshift of the line peaks is attributed to dust that condensed from the SN 1987A ejecta that is still distributed in dense opaque clumps. The strongest ultraviolet lines are those of Mg I lambda 2852 and Mg II lambda lambda 2795, 2802. The Mg I lambda 2852 line is significantly broader than most lines in the optical, which provides a natural explanation for the size differences in the optical and ultraviolet of the SN 1987A ejecta derived from HST direct images. C1 UNIV TEXAS,MCDONALD OBSERV,AUSTIN,TX 78712. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. STOCKHOLM OBSERV,S-13300 SALTSJOBADEN,SWEDEN. NATL OPT ASTRON OBSERV,CERRO TOLOLO INTER AMER OBSERV,LA SERENA,CHILE. BEIJING ASTRON OBSERV,BEIJING 100080,PEOPLES R CHINA. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. EUROPEAN SPACE AGCY,DEPT SPACE SCI,DIV ASTROPHYS,NOORDWIJK,NETHERLANDS. RP Wang, LF (reprint author), UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712, USA. NR 51 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1996 VL 466 IS 2 BP 998 EP 1010 DI 10.1086/177570 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ546 UT WOS:A1996UZ54600036 ER PT J AU Ho, LC Filippenko, AV AF Ho, LC Filippenko, AV TI Dynamical evidence for a massive, young globular cluster in NGC 15691 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, individual (NGC 1569); galaxies, irregular; galaxies, starburst; galaxies, star clusters; globular clusters, general ID SPACE-TELESCOPE OBSERVATIONS; STARBURST GALAXY NGC-1569; MERGER REMNANT NGC-7252; STAR-FORMING REGION; INTERSTELLAR-MEDIUM; SPECTRA; MACROTURBULENCE; DISCOVERY; PECULIAR; PROFILES AB Recent high-resolution observations with the Hubble Space Telescope (HST) reveal that star clusters of extraordinary luminosity and compactness are commonly found in a variety of starburst systems. There has been much speculation that these clusters represent present-day analogs of young globular clusters. Using the HIRES echelle spectrograph on the Keck 10 m telescope, we obtained high-dispersion optical spectra of one of the ''super star clusters'' (cluster ''A'') in the nearby dwarf galaxy NGC 1569. The size of the cluster is known from published HST images. The line-of-sight velocity dispersion (sigma* = 15.7 +/- 1.5 km s(-1)) has been measured from a cross-correlation analysis of its integrated spectrum at visual wavelengths. If the cluster is gravitationally bound and the velocities are isotropic, application of the virial theorem implies that the cluster has a total stellar mass of (3.3 +/- 0.5) x 10(5) M(.). This object's mass, mass density, and probable mass-to-light ratio after aging 10-15 Gyr are fully consistent with the typical values of Galactic globular clusters. Our result strongly suggests that at least some of the luminous, compact, young star clusters being discovered with HST will indeed evolve into normal globular clusters of the type seen in the Milky Way. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. RP Ho, LC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 45 TC 51 Z9 51 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1996 VL 466 IS 2 BP L83 EP L86 DI 10.1086/310181 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ547 UT WOS:A1996UZ54700008 ER PT J AU Murphy, EM Lockman, FJ Laor, A Elvis, M AF Murphy, EM Lockman, FJ Laor, A Elvis, M TI Galactic H I column densities toward quasars and active galactic nuclei SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE Galaxy, structure; radio lines, ISM; X-rays, general AB We have determined accurate values of the Galactic neutral hydrogen column density, N-H, toward 220 quasars and active galactic nuclei from 21 cm H I measurements made on the 140 Foot Telescope (42.7 m). Accurate values of N-H have now been obtained for the whole PG bright quasar sample and most quasars that have been observed by ROSAT and the Hobble Space Telescope through mid-1993. The spectra were corrected for stray 21 cm radiation yielding values of N-H with a typical uncertainty of 1 x 10(19) cm(-2) for high Galactic latitude directions. The H I column densities will be useful for correcting for interstellar opacity at UV and soft X-ray wavelengths, and for estimating the reddening and extinction toward these objects. C1 NATL RADIO ASTRON OBSERV,CHARLOTTESVILLE,VA 22903. NATL RADIO ASTRON OBSERV,GREEN BANK,WV 24944. TECHNION ISRAEL INST TECHNOL,DEPT PHYS,IL-32000 HAIFA,ISRAEL. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Murphy, EM (reprint author), UNIV VIRGINIA,520 EDGEMONT RD,CHARLOTTESVILLE,VA 22903, USA. NR 13 TC 173 Z9 173 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 1996 VL 105 IS 2 BP 369 EP 373 DI 10.1086/192319 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VB173 UT WOS:A1996VB17300008 ER PT J AU Dowling, S AF Dowling, S TI Good words on Gussin SO CD-ROM PROFESSIONAL LA English DT Letter RP Dowling, S (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER ART,NEW MEDIA LEARNING ENVIRONM,8TH & G ST NW,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PEMBERTON PRESS INC PI WILTON PA 462 DANBURY RD, WILTON, CT 06897-2126 SN 1049-0833 J9 CD-ROM PROF JI CD-ROM Prof. PD AUG PY 1996 VL 9 IS 8 BP 8 EP 8 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA UY236 UT WOS:A1996UY23600002 ER PT J AU Greenberg, R Reitsma, R Angon, AC AF Greenberg, R Reitsma, R Angon, AC TI Interspecific aggression by Yellow Warblers in a sun coffee plantation SO CONDOR LA English DT Article DE Dendroica petechia; interspecific aggression; competition; winter habitat use; coffee RP Greenberg, R (reprint author), SMITHSONIAN MIGRATORY BIRD CTR,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 8 TC 12 Z9 13 U1 1 U2 2 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0010-5422 J9 CONDOR JI Condor PD AUG PY 1996 VL 98 IS 3 BP 640 EP 642 DI 10.2307/1369579 PG 3 WC Ornithology SC Zoology GA VG525 UT WOS:A1996VG52500021 ER PT J AU Miththapala, S Seidensticker, J OBrien, SJ AF Miththapala, S Seidensticker, J OBrien, SJ TI Phylogeographic subspecies recognition in leopards (Panthera pardus): Molecular genetic variation SO CONSERVATION BIOLOGY LA English DT Article ID MITOCHONDRIAL-DNA; HETEROZYGOSITY; HYBRIDIZATION; CONSERVATION; DIVERSITY; CHEETAH; NUMBER; WOLF AB The incorporation of precise definitions for taxonomic units into wildlife legislation has necessitated the reevaluation of the taxonomy of endangered and threatened species. We used the subspecies recognition criteria proposed by Avise and Ball (1990) and O'Brien and Mayr (1991) to examine the infraspecific taxonomy of the leopard, Panthera pardus, a geographically widespread species with 27 currently recognized trinomial designations. Samples from named subspecies revealed appreciable genetic diversity using three molecular methods: allozymes, mitochondrial DNA restriction sites, and feline-specific minisatellites. Continental populations and subspecies from Africa and Asia possessed the highest amount of molecular genetic variation, whereas relatively lower amounts of diversity were present in island populations. Molecular data were analyzed using three phylogenetic methods (distance-matrix, maximum parsimony, and maximum likelihood) to resolve genetic differentiation below the species level. The combined results revealed phylogenetic distinction of six geographically isolated groups of leopards: (1) African (2) central Asian, (3) Indian, (4) Sir Lankan, (5) Javan, and (6) east Asian. Based on the combined molecular analyses and supporting morphological data (Miththapala 1992), we recommend that subspecific leopard taxonomy be revised to comprise eight subspecies: (1) P. p. pardus, Africa; (2) P. p. saxicolor, central Asia; (3) P. p. fusca, Indian subcontinent; (4) P. p. kotiya, Sri Lanka; (5) P. p. melas, Java; (6) P. p. orientalis, Amur; (7) P. p. japonensis, northern China; and (8) P. p. delacouri, southern China. In most cases, designated subspecies conform to historic geological barriers that would have facilitated allopatric genetic divergence. C1 NCI, FREDERICK CANC RES & DEV CTR, BIOL CARCINOGENESIS & DEV PROGRAM, PROGRAM RESOURCES INC, FREDERICK, MD 21702 USA. SMITHSONIAN INST, NATL ZOOL PK, WASHINGTON, DC 20008 USA. NCI, NIH, VIRAL CARCINOGENESIS LAB, FREDERICK CANC RES & DEV CTR, FREDERICK, MD 21702 USA. NR 80 TC 45 Z9 55 U1 0 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD AUG PY 1996 VL 10 IS 4 BP 1115 EP 1132 DI 10.1046/j.1523-1739.1996.10041115.x PG 18 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA VC103 UT WOS:A1996VC10300029 ER PT J AU Carmichael, ISE Lange, RA Luhr, JF AF Carmichael, ISE Lange, RA Luhr, JF TI Quaternary minettes and associated volcanic rocks of Mascota, western Mexico: A consequence of plate extension above a subduction modified mantle wedge SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY LA English DT Review ID NATURAL SILICATE LIQUIDS; SIERRA-LA-PRIMAVERA; EAST PACIFIC RISE; HIGH-MAGNESIAN ANDESITES; OXIDATION-STATE; BAJA-CALIFORNIA; CALC-ALKALINE; TRACE-ELEMENT; RIVERA PLATE; CHEMICAL CHARACTERISTICS AB Pleistocene-Holocene volcanism in the Jalisco block of western Mexico is confined to two conspicuous grabens, where potassic eruptives range from absarokites (48-52% SiO2) and minettes (49-54% SiO2) through basaltic andesites (53-57% SiO2), the most voluminous type, to andesites and their lamprophyric equivalent spessartite (58-62% SiO2); there are no contemporary rhyolitic rocks. This suite has high concentrations of Mg, Cr (<550 ppm) and Ni (<450 ppm) accompanied by large concentrations of K, P, Ba (<3000 ppm) and Sr (<5000 ppm) and elements such as LREE and Zr (<600 ppm). No combination of crystal fractionation and/or crustal contamination can reproduce the compositional range of these magmas, which nevertheless are believed to be genetically related because of their proximity in time and space. Hydrous minerals in the lamprophyres and the typical absence of plagioclase phenocrysts in both basaltic andesites and andesites reflect the relatively high concentrations of water in the magmas, which suppressed the crystallisation of feldspar. Experimental verification of the minimal amounts of water required to reproduce the phenocryst assemblages in selected rocks range from 3.5 to 6%. During ascent in a volcanic conduit, andesitic magma may lose water and consequently precipitate plagioclase, or it may ascend more rapidly, retaining more of its initial water, which stabilises phenocrysts of hornblende at the expense of plagioclase. Our estimates of water concentrations, which are consistent with the various low pressure phenocryst assemblages, will be minimal for the magmas in their source regions, and the process of magmatic dewatering on ascent may be typical in well established volcanic conduits. In accord with the compositions of phenocrystic olivine in the basaltic andesites and the minettes, the values of FeO and Fe2O3 of the bulk lavas and scoriae are demonstrably pristine. As a consequence, are two characteristic features of the Mascota the high range of relative oxygen fugacities (Delta NNO=1-5) and the high Mg # (MgO/MgO+FeO) that ranges from 0.70 to 0.91 (with only one andesite as low as 0.66). From the evidence of phlogopite phenocrysts, a partial melt involving phlogopite would have a higher Mg # than one from olivine (Fo(90)) and pyroxene alone. As the Mascota series shows a correlation between K2O and Mg #, we conclude that it was generated by partial fusion of the mantle wedge, with a variable contribution of phlogopite and apatite from veins throughout the lherzolitic assemblage. In conformity with an origin by varying increments of partial fusion of a phlogopite-bearing mantle, all incompatible elements vary linearly with Ti (or K) as if phlogopite (+apatite) in the source dominated their contribution to the partial melts. Fluids from dehydration of the subducting slab presumably deposit hydrous and other minerals in veins in the mantle wedge and also increase its redox state. As the Mascota volcanism occurs in grabens closer to the trench than the main andesite are, it is concluded that the eruption of these small volumes of hydrous magmas require the tectonically favored ascent paths offered by the extensional grabens to reach the surface from their mantle sources. C1 SMITHSONIAN INST,DEPT MINERAL SCI,NHB 119,WASHINGTON,DC 20560. RP Carmichael, ISE (reprint author), UNIV CALIF BERKELEY,DEPT GEOL & GEOPHYS,BERKELEY,CA 94720, USA. NR 115 TC 107 Z9 108 U1 0 U2 6 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0010-7999 J9 CONTRIB MINERAL PETR JI Contrib. Mineral. Petrol. PD AUG PY 1996 VL 124 IS 3-4 BP 302 EP 333 DI 10.1007/s004100050193 PG 32 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA VH533 UT WOS:A1996VH53300006 ER PT J AU Burns, JR Weitzman, SH AF Burns, JR Weitzman, SH TI Novel gill-derived gland in the male swordtail characin, Corynopoma riisei (Teleostei: Characidae: Glandulocaudinae) SO COPEIA LA English DT Article ID MORPHOLOGY AB Sexually mature males of Corynopoma riisei possess structures in the anterior part of the gill cavity that are secretory and consist of a series of chambers lined with tall columnar epithelium. These structures, referred to as gill glands, were present in all 11 mature males and absent in the four immature males and nine mature females, analyzed histologically. Thus, the gland appears to be a male secondary sex character that develops as sexual maturity is attained. A gill gland in the process of development was present in a male whose testes were undergoing early stages of maturation. The gland appears to develop from the anterior 8-13 gill filaments of the first gill arches. The gill secondary lamellae shorten such that their only remnants in most of the mature gill gland are capillaries at the bases of the columnar cells that line the chambers. The edges of adjacent gill filaments must fuse to form the chambers that open into the gill cavity through antero-ventrally oriented apertures. Skeletal muscle and cartilage from the original gill filaments remain within the chamber walls. Degree of expansion and secretory activity of the glands varied among the 11 mature males. Based on histological characteristics of the gland, its location, and the complex courtship behavior of this species, we hypothesize that the gill gland is producing some type of female attractant (pheromone). C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560. RP Burns, JR (reprint author), GEORGE WASHINGTON UNIV,DEPT BIOL SCI,WASHINGTON,DC 20052, USA. NR 18 TC 28 Z9 31 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS BUSINESS OFFICE PI CARBONDALE PA SOUTHERN ILLINOIS UNIV, DEPT ZOOLOGY, CARBONDALE, IL 62901-6501 SN 0045-8511 J9 COPEIA JI Copeia PD AUG 1 PY 1996 IS 3 BP 627 EP 633 PG 7 WC Zoology SC Zoology GA VB033 UT WOS:A1996VB03300012 ER PT J AU Parenti, LR AF Parenti, LR TI Phylogenetic systematics and biogeography of phallostethid fishes (Atherinomorpha, Phallostethidae) of northwestern Borneo, with description of a new species SO COPEIA LA English DT Article ID PLATE-TECTONICS; SARAWAK; TELEOSTEI AB Until recently, the distinctive phallostethid genus Phallostethus was known from a single collection made in 1902 from Johor on the Malay Peninsula, described in 1913 by Regan as Phallostethus dunckeri. In 1991 and 1993, specimens of Phallostethus were collected from disjunct coastal localities in sarawak and Brunei, northwestern Borneo. These Borneo specimens differ from Phallostethus dunckeri in morphology of the priapium (a complex, bilaterally asymmetric, subcephalic copulatory organ), pigmentation, and paradentary bone dentition. They are described herein as Phallostethus lehi, bringing the number of recognized phallostethid species to 20. Phenacostethus smithi Myers, 1928, previously unknown from Borneo has been collected from Sarawak, Brunei, and Kalimantan, bringing the total number of Bornean phallostethid species recognized currently to six. The phallostethids of Borneo do not form a monophyletic group but, instead, have complex, repeated sets of relationships with species on the Malay Peninsula and in the Philippines. Components of their biogeographic relationships are shared with other members of the stream biota. Composite biotic relationships are consistent with a composite geological origin of modern Borneo. RP Parenti, LR (reprint author), SMITHSONIAN INST, NATL MUSEUM NAT HIST, DIV FISHERIES, NHB MRC 159, WASHINGTON, DC 20560 USA. NR 43 TC 12 Z9 13 U1 0 U2 3 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD AUG 1 PY 1996 IS 3 BP 703 EP 712 PG 10 WC Zoology SC Zoology GA VB033 UT WOS:A1996VB03300021 ER PT J AU Harris, JD Johnson, KR Hicks, J Tauxe, L AF Harris, JD Johnson, KR Hicks, J Tauxe, L TI Four-toed theropod footprints and a paleomagnetic age from the Whetstone Falls Member of the Harebell Formation (Upper cretaceous: Maastrichtian), northwestern Wyoming SO CRETACEOUS RESEARCH LA English DT Article DE Harebell Formation; Whetstone Falls Member; Exallopus; ichnology; theropod Cretaceous; Maastrichtian; magnetostratigraphy; Wyoming ID BIRDS AB The Harebell Formation is a syntectonic sequence of conglomeratic sediments deposited in a narrow, rapidly subsiding trough that formed in the latest Cretaceous along the eastern margin of the ancestral uplift of what are today the Teton and Gros Ventre Mountains of northwestern Wyoming. On at least two occasions subsidence temporarily exceeded the rate of sediment supply and the area was flooded by a brackish or marine incursion from the Western Interior Seaway that lay to the east. The age of the Harebell Formation is Maastrichtian, corroborated by K-40/Ar-40 isotropic ages, vertebrate and palynomorph biostratigraphy, and a preliminary magnetostratigraphic analysis which correlates it to the geomagnetic reversal time scale from the upper part of C31R to the base of C30N. Sandstone slabs collected from the lower Whetstone Falls Member contain nine partial and complete footprints attributable to a theropod (Dinosauria: Saurischia). The footprints were formed as surface tracks in the tabular-bedded sandstone by dinosaurs that roamed the burrowed and leaf-littered sand flats and shallow waters along the margins of a low-energy, brackish-water embayment. Eight of the nine footprints represent a hitherto unknown ichnogenus, representing a four-toed pedal morphology for a theropod dinosaur which is unprecedented in the Late Cretaceous. The theropod nature of the tracks is implied by the length and narrowness of the digits and the sharp claw impressions. The tracks have clearly defined impressions of four toes, none of which appears to be a hallux in the traditional theropod sense of a small, retroverted hallux. The metapodial impression is also unlike that of other known theropod tracks: greater in relief than the digits but quite small in area. The tracks represent at least two individuals, although no clear trackways are available. Exallopus lovei, gen. et sp. nov., represents a type of theropod not currently recognized from body fossils. (C) 1996 Academic Press Limited C1 DENVER MUSEUM NAT HIST,DEPT EARTH SCI,DENVER,CO 80205. SMITHSONIAN INST,MUSEUM NAT HIST,WASHINGTON,DC 20560. SCRIPPS INST OCEANOG,LA JOLLA,CA 92093. NR 51 TC 15 Z9 19 U1 2 U2 4 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0195-6671 J9 CRETACEOUS RES JI Cretac. Res. PD AUG PY 1996 VL 17 IS 4 BP 381 EP 401 DI 10.1006/cres.1996.0024 PG 21 WC Geology; Paleontology SC Geology; Paleontology GA VB487 UT WOS:A1996VB48700001 ER PT J AU Tudge, CC Jamieson, BGM AF Tudge, CC Jamieson, BGM TI Spermatophore and spermatozoal morphology in the Porcellanidae .2. The genera Petrolisthes and Polyonyx (Decapoda: Anomura) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB The porcellanid genera Petrolisthes and Polyonyx are shown to have differing spermatozoal morphology reflecting an apparently natural division of the family previously suggested on adult and larval somatic morphology. Species investigated in the genus Petrolisthes have spermatozoa with a globular nucleus and autapomorphic opercular ridge and tubular ring structure within the acrosomal vesicle. Spermatozoa of Polyonyx transversus (Haswell) have a long ''taillike'' nucleus penetrated throughout by a central microtubular core. This latter spermatozoal morphology is shared with other members investigated in the ''Porcellana-group,'' (Aliaporcellana and Pisidia). All the Porcellanidae investigated share a suite of spermatozoal characters that unite them (superior acrosomal vesicle; broad, centrally perforate operculum; 4 or more external microtubular arms; perforatorial chamber wall folded into corrugations or septa; dense perforatorial cone; posterior perforatorial ring and divided inner acrosome zone). A unique spermatophore morphology, consisting of a tubular extension of the anterior end of the ampulla, is described for representatives in the genus Petrolisthes. C1 UNIV QUEENSLAND,DEPT ZOOL,BRISBANE,QLD 4072,AUSTRALIA. RP Tudge, CC (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 15 TC 12 Z9 13 U1 0 U2 3 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD AUG PY 1996 VL 16 IS 3 BP 535 EP 546 DI 10.2307/1548744 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA VA952 UT WOS:A1996VA95200014 ER PT J AU Ferrari, FD AF Ferrari, FD TI Thomas Elliot Bowman III (1918-1995) - Obituary SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Item About an Individual RP Ferrari, FD (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD AUG PY 1996 VL 16 IS 3 BP 633 EP 635 PG 3 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA VA952 UT WOS:A1996VA95200025 ER PT J AU Condit, R Hubbell, SP Lafrankie, JV Sukumar, R Manokaran, N Foster, RB Ashton, PS AF Condit, R Hubbell, SP Lafrankie, JV Sukumar, R Manokaran, N Foster, RB Ashton, PS TI Species-area and species-individual relationships for tropical trees: A comparison of three 50-ha plots SO JOURNAL OF ECOLOGY LA English DT Article DE tropical forest; species-area curve; species-individual curve ID SHORT-TERM DYNAMICS; NEOTROPICAL FOREST; DENSITY-DEPENDENCE; ISLAND SIZE; DIVERSITY; RICHNESS; BIODIVERSITY; EXTRAPOLATION; COMMUNITY; DROUGHT AB 1 Species-accumulation curves for woody plants were calculated in three tropical forests, based on fully mapped 50-ha plots in wet, old-growth forest in Peninsular Malaysia, in moist, old-growth forest in central Panama, and in dry, previously logged forest in southern India. A total of 610 000 stems were identified to species and mapped to < Im accuracy. Mean species number and stem number were calculated in quadrats as small as 5 m x 5 m to as large as 1000 m x 500 m, for a variety of stem sizes above 10 mm in diameter. Species-area curves were generated by plotting species number as a function of quadrat size; species-individual curves were generated from the same data, but using stem number as the independent variable rather than area. 2 Species-area curves had different forms for stems of different diameters, but species-individual curves were nearly independent of diameter class. With < 10(4) stems, species-individual curves were concave downward on log-log plots, with curves from different forests diverging, but beyond about 104 stems, the log-log curves became nearly linear, with all three sites having a similar slope. This indicates an asymptotic difference in richness between forests: the Malaysian site had 2.7 times as many species as Panama, which in turn was 3.3 times as rich as India. 3 Other details of the species-accumulation relationship were remarkably similar between the three sites. Rectangular quadrats had 5-27% more species than square quadrats of the same area, with longer and narrower quadrats increasingly diverse. Random samples of stems drawn from the entire 50 ha had 10-30% more species than square quadrats with the same number of stems. At both Pasoh and BCI, but not Mudumalai. species richness was slightly higher among intermediate-sized stems (50-100mm in diameter) than in either smaller or larger sizes, These patterns reflect aggregated distributions of individual species, plus weak density-dependent forces that tend to smooth the species abundance distribution and 'loosen' aggregations as stems grow. 4 The results provide support for the view that within each tree community, many species have their abundance and distribution guided more by random drift than deterministic interactions. The drift model predicts that the species-accumulation curve will have a declining slope on a log-log plot, reaching a slope of O.1 in about 50 ha. No other model of community structure can make such a precise prediction. 5 The results demonstrate that diversity studies based on different stem diameters can be compared by sampling identical numbers of stems. Moreover, they indicate that stem counts < 1000 in tropical forests will underestimate the percentage difference in species richness between two diverse sites. Fortunately, standard diversity indices (Fisher's sc, Shannon-Wiener) captured diversity differences in small stem samples more effectively than raw species richness, but both were sample size dependent. Two nonparametric richness estimators (Chao. jackknife) performed poorly, greatly underestimating true species richness. C1 PRINCETON UNIV, DEPT ECOL & EVOLUT BIOL, PRINCETON, NJ 08544 USA. NANYANG TECHNOL UNIV, NATL INST EDUC, CTR TROP FOREST SERV, SINGAPORE 1025, SINGAPORE. INDIAN INST SCI, CTR ECOL SCI, BANGALORE 560012, KARNATAKA, INDIA. FOREST RES INST MALAYSIA, KUALA LUMPUR 52109, MALAYSIA. FIELD MUSEUM NAT HIST, DEPT BOT, CHICAGO, IL 60605 USA. HARVARD UNIV, INST INT DEV, CAMBRIDGE, MA 02138 USA. HARVARD UNIV, ARNOLD ARBORETUM, CAMBRIDGE, MA 02138 USA. RP Condit, R (reprint author), SMITHSONIAN TROP RES INST, CTR TROP FOREST SCI, UNIT 0948, APO, AA 34002 USA. RI Raman, Sukumar/C-9809-2013 NR 61 TC 275 Z9 299 U1 8 U2 131 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD AUG PY 1996 VL 84 IS 4 BP 549 EP 562 DI 10.2307/2261477 PG 14 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA VH804 UT WOS:A1996VH80400006 ER PT J AU Faust, MA AF Faust, MA TI Morphology and ecology of the marine benthic dinoflagellate Scrippsiella subsalsa (Dinophyceae) SO JOURNAL OF PHYCOLOGY LA English DT Article DE benthic dinoflagellate; detritus; Dinophyceae; ecology; Iriomote Island, Japan; mangrove; morphology; Oshigaki Island, Japan; sand; scanning electron microscopy; Scrippsiella subsalsa; taxonomy; Twin Cays, Belize ID SP-NOV DINOPHYCEAE; PERIDINIUM-GREGARIUM; POOL DINOFLAGELLATE; MANGROVE-ISLAND; TWIN CAYS; COMB-NOV; REDESCRIPTION; BELIZE; CYST AB The thecal surface morphology of Scrippsiella subsalsa (Ostenfeld) Steidinger et Balech was examined using the scanning electron microscope. This species is distinguished by a number of morphological characteristics. Apical plate 1' is wide, asymmetric, and pentagonal, and it ends at the anterior margin of the cingulum. Intercalary plates 2a and 3a are separated by apical plate 3'. The apical pore complex includes a large P-o plate with a raised dome at the center and a deep canal plate with thickened margins at plates 2', 3', and 4'. The intercalary bands are wide and deeply striated. The cingulum is deep, formed by six cingular plates; its surface is transversely striated and aligned with a row of minute pores. The cingular list continues around postcingular plate 1 ''' to form a sulcal list. The sulcal list is a flexible ribbon with a rounded tip that protrudes posteriorly, partially covering the sulcal plates. The hypotheca is lobed, and the antapical plates are irregularly shaped and wide in antapical view. The thecal surface is vermiculate to reticulate. A comparison in morphology and ecology is presented between S. subsalsa and other known Scrippsiella species. RP Faust, MA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,4201 SILVER HILL RD,SUITLAND,MD 20746, USA. NR 34 TC 14 Z9 16 U1 1 U2 4 PU PHYCOLOGICAL SOC AMER INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD AUG PY 1996 VL 32 IS 4 BP 669 EP 675 DI 10.1111/j.0022-3646.1996.00669.x PG 7 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA VD568 UT WOS:A1996VD56800023 ER PT J AU Park, K Nolt, IG Steele, TC Zink, LR Evenson, KM Chance, KV Murray, AG AF Park, K Nolt, IG Steele, TC Zink, LR Evenson, KM Chance, KV Murray, AG TI Pressure broadening of the 50.873 and 83.469 cm(-1) molecular oxygen lines SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article ID N2; O2 AB We report pressure broadening measurements of the 50.873 and 83.469 cm(-1) molecular oxygen lines at 293 K. Air broadening coefficients are determined with 13% accuracy. Published by Elsevier Science Ltd. C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. NATL INST STAND & TECHNOL,BOULDER,CO 80303. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV LONDON QUEEN MARY & WESTFIELD COLL,LONDON E1 4NS,ENGLAND. RP Park, K (reprint author), UNIV OREGON,DEPT PHYS,EUGENE,OR 97403, USA. OI Chance, Kelly/0000-0002-7339-7577 NR 8 TC 10 Z9 10 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD AUG PY 1996 VL 56 IS 2 BP 315 EP 316 DI 10.1016/0022-4073(96)00026-X PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA VD019 UT WOS:A1996VD01900013 ER PT J AU Cannon, MS Davis, RW Weldon, PJ AF Cannon, MS Davis, RW Weldon, PJ TI Dorsal glands of Alligator mississippiensis: A histological and histochemical study SO JOURNAL OF ZOOLOGY LA English DT Article AB Several investigators have described in some crocodilians a row of round or oval organs, called dorsal glands, lying under scutes on each side of the dorsal midline. The function of these glands is unknown, but they are hypothesized to produce skin-conditioning secretions. We investigated the anatomy and histochemistry of the dorsal glands of adult American alligators (Alligator mississippiensis). Twenty to 22 pairs of glands containing a viscous, often black, material were observed lying from the mid-cervical to the anterior caudal regions in the axial musculature or on the inner surface of the dermis. The capsule of each gland consists of dense collagenous fibres and numerous short elastic fibres, and is surrounded by skeletal muscle. The single lumen is lined by one to several layers of cuboidal to columnar epithelium in varying stages of degeneration, indicating a holocrine secretory mode. The epithelial cell membranes often interdigitate and tight junctions and desmosomes occasionally are observed between them. The epithelial cells and secretory product contain slight to considerable amounts of lipid; glycoproteins may be present. Crystals exhibiting a dense core and/or layering occur in the epithelial cells and secretory product. Energy-dispersive X-ray analysis demonstrates calcium, copper, iron, lead, potassium, and zinc in the crystals. Mitochondria, vacuoles, and short segments of rough endoplasmic reticulum also occur in the cells. C1 TEXAS A&M UNIV,DEPT BIOL,COLLEGE STN,TX 77843. SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. RP Cannon, MS (reprint author), TEXAS A&M UNIV,HLTH SCI CTR,COLL MED,DEPT HUMAN ANAT & MED NEUROBIOL,COLLEGE STN,TX 77843, USA. NR 8 TC 3 Z9 3 U1 0 U2 3 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0952-8369 J9 J ZOOL JI J. Zool. PD AUG PY 1996 VL 239 BP 625 EP 631 PN 4 PG 7 WC Zoology SC Zoology GA VC582 UT WOS:A1996VC58200001 ER PT J AU Nickle, DA Heymann, EW AF Nickle, DA Heymann, EW TI Predation on orthoptera and other orders of insects by tamarin monkeys, Saguinus mystax mystax and Saguinus fuscicollis nigrifrons (Primates: Callitrichidae), in north-eastern Peru SO JOURNAL OF ZOOLOGY LA English DT Article ID AERIAL LEAF LITTER; FEEDING ECOLOGY; MOUSTACHED TAMARINS; AMAZONIA; BEHAVIOR; DIET; PLATYRRHINI; FOREST AB Katydids and related insects are an important component in the diets of moustached (Saguinus mystax mystax) and saddle back tamarins (Saguinus fuscicollis nigrifrons). Based on preliminary data of captured prey, trends suggest that partitioning occurs regarding orthopterans as a limited food resource. Of species captured as prey, only three were shared by both tamarin species. Saddle-back tamarins appeared to specialize more on understorey species (0-4 m), concentrating on pseudophylline katydids. Moustached tamarins incorporated a greater percentage of phaneropterine katydids from the lower to middle canopy into their diet of insects. Although most prey species were exposed to view during the diurnal feeding period of the tamarins, only the saddle-back tamarin fed on katydids that spend the dal concealed from view within dead curled leaves. Differentiation of the prey spectrum may represent a critical pattern of niche differentiation in these two sympatric tamarin species, which show a high overlap in their plant food resources. C1 DEUTSCH PRIMATENZENTRUM GMBH,AG VERHALTENFORSCH OKOL,D-37077 GOTTINGEN,GERMANY. SMITHSONIAN INST,US NATL MUSEUM NAT HIST,SYSTEMAT ENTOMOL LAB,USDA,ARS,PSI,WASHINGTON,DC 20560. NR 83 TC 36 Z9 37 U1 0 U2 14 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0952-8369 J9 J ZOOL JI J. Zool. PD AUG PY 1996 VL 239 BP 799 EP 819 PN 4 PG 21 WC Zoology SC Zoology GA VC582 UT WOS:A1996VC58200014 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI William Glackens - Gerdts,WH SO LIBRARY JOURNAL LA English DT Book Review RP Kalfatovic, MR (reprint author), SMITHSONIAN INST LIB,ARLINGTON,VA, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 1996 VL 121 IS 13 BP 67 EP 67 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA VC477 UT WOS:A1996VC47700062 ER PT J AU Dowd, A Levine, M AF Dowd, A Levine, M TI Calibrate vector modulators for phase modulation SO MICROWAVES & RF LA English DT Article AB VECTOR modulators readily support phase modulation. By driving the modulation ports of the vector modulator with a pair of computer-controlled digital-to-analog converters (DACs), it is possible to produce an extremely accurate phase shift on a carrier. Systematic errors in the vector modulator and DAC can be corrected via calibration and by using the computer to apply a complementary modulation function. This results in improved phase accuracy, lower amplitude modulation (AM) noise, and better sideband rejection compared to conventional vector modulators. In addition, the calibration method allows an increase in the modulator's effective operating bandwidth. RP Dowd, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MAIL STOP 78,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PENTON PUBL INC PI CLEVELAND PA 1100 SUPERIOR AVE, CLEVELAND, OH 44114 SN 0745-2993 J9 MICROWAVES RF JI Microw. RF PD AUG PY 1996 VL 35 IS 8 BP 101 EP & PG 6 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA WE765 UT WOS:A1996WE76500030 ER PT J AU Nusser, JA Goto, RM Ledig, DB Fleischer, RC Miller, MM AF Nusser, JA Goto, RM Ledig, DB Fleischer, RC Miller, MM TI RAPD analysis reveals low genetic variability in the endangered light-footed clapper rail SO MOLECULAR ECOLOGY LA English DT Article DE clapper rail; conservation genetics; genetic diversity; Rallus langirostris levipes; Rallus longirostris yumanensis; RAPD ID AMPLIFIED POLYMORPHIC DNA; SOUTHERN-CALIFORNIA; NATURAL-POPULATIONS; ARBITRARY PRIMERS; MARKERS; HABITAT; DIFFERENTIATION; INDIVIDUALS; DIVERSITY; MOVEMENTS AB Numbers of light-footed clapper rails Rallus longirostris levipes, an endangered bird inhabiting southern California salt marshes, have substantially declined from historic levels. RAPD (randomly amplified polymorphic DNA) analysis was employed to assess the genetic variability within and among four of the largest remaining light-footed clapper rail populations. A single, larger population of the endangered Yuma clapper rail Rallus longirostris yumanensis was used for comparison. A total of 325 RAPD primers were tested on DNA from a subset of five clapper rails composed of a single representative for each of the four light-footed clapper rail populations and a representative for the single Yuma clapper rail population. Of the 1338 amplified bands (loci) surveyed in these five representative birds, approximately 1% were polymorphic, indicating the level of differentiation across all loci is quite low. Nine primers yielding these 16 polymorphic bands were used to analyse 48 individuals from five populations. Five of these bands were polymorphic in both subspecies, six were polymorphic only within the light-footed clapper rails, and five were polymorphic only within the Yuma clapper rail samples. Considering the few bands that were polymorphic among the light-footed clapper rail populations, a surprisingly high level of population differentiation (G(ST) = 0.28) was found. This is in accord with the results of AMOVA analyses which show that a fairly high percentage of the limited variability among the rails is due to either differences between subspecies or differences between the light-footed rail populations. Because inbreeding depression is suspected and overall genetic distances between populations are low, movement of light-footed clapper rails from larger populations into smaller ones might be considered as a management strategy. Employing RAPDs as one of a series of assays is useful in revealing the population structure of genetically depauperate species. C1 CITY HOPE NATL MED CTR,BECKMAN RES INST,DEPT MOL BIOCHEM,DUARTE,CA 91010. UNIV CALIF SANTA BARBARA,DEPT BIOL SCI,SANTA BARBARA,CA 93106. SMITHSONIAN INST,NATL ZOOL PK,MOL GEN PROGRAM,WASHINGTON,DC 20008. NR 54 TC 42 Z9 45 U1 1 U2 11 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD AUG PY 1996 VL 5 IS 4 BP 463 EP 472 PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA VF478 UT WOS:A1996VF47800001 PM 8794557 ER PT J AU Ebeling, H Voges, W Bohringer, H Edge, AC Huchra, JP Briel, UG AF Ebeling, H Voges, W Bohringer, H Edge, AC Huchra, JP Briel, UG TI Properties of the X-ray-brightest Abell-type clusters of galaxies (XBACs) from ROSAT all-sky survey data .1. The sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies, clusters, general; cosmology, observations; large-scale structure of Universe; X-rays, galaxies ID SOUTHERN RICH CLUSTERS; OPTICAL SPECTROSCOPY; VELOCITY DISPERSIONS; LUMINOSITY FUNCTIONS; SPATIAL-DISTRIBUTION; HYDRA-CENTAURUS; ACO CLUSTERS; REDSHIFTS; CATALOG; EVOLUTION AB We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (\b\ greater than or equal to 20 degrees), the nominal redshift range of the ACO catalogue oft less than or equal to 0.2, and X-ray fluxes above 5.0 x 10(-12) erg cm(-2) s(-1) in the 0.1-2.4 keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe. C1 MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 95 TC 393 Z9 394 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 1996 VL 281 IS 3 BP 799 EP 829 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VB271 UT WOS:A1996VB27100013 ER PT J AU vanDokkum, PG Franx, M AF vanDokkum, PG Franx, M TI The fundamental plane in CL 0024 at z=0.4: Evolution of the mass-to-light ratio SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies, clusters, individual, CL 0024; galaxies, elliptical and lenticular, cD; galaxies, evolution; galaxies, structure ID PHOTOMETRIC STANDARD STARS; DN-SIGMA RELATION; ELLIPTICAL GALAXIES; DISTANT CLUSTERS; COMA CLUSTER; REDSHIFT SURVEY; S0 GALAXIES; SPECTROSCOPY; POPULATION; KINEMATICS AB We present results on the Fundamental Plane of early-type galaxies in the rich cluster CL0024+16 at z=0.39. The internal velocity dispersions of the galaxies have been measured from a 19-h integration at the MMT. The photometric parameters of the galaxies have been measured from deep HST images. The galaxies satisfy a tight Fundamental Plane relation which is similar to that at low redshift. The scatter is 15 per cent in log r(e), also very similar to that at low redshift. The data show that massive early-type galaxies existed at z=0.4, and extend earlier studies of the luminosities and colours of early-types in rich clusters. The evolution of the M/L ratio is derived from the Fundamental Plane, by a comparison with Coma. The M/L ratio increases by 31+/-12 per cent between z=0.39 and z=0.023. The evolution is low when compared with models for stellar populations. The expected evolution depends on the IMF, q(0), and the formation redshift of the galaxies. The data are in agreement with high formation redshifts. The modelling is still uncertain, however, because of various possible biases. The most serious bias may be the progenitor bias: if the progenitors of some current-day early-types were spirals at z=0.4, they would not be included in the sample, and the sample would be biased towards the oldest galaxies. More data are needed to measure the evolution of the Fundamental Plane more precisely, and its scatter. There is a hint that the form of the Fundamental Plane changes with redshift, and this needs to be determined better. Deeper samples on more clusters would be valuable. Studies of the richest nearby clusters may help to test the underlying hypothesis that the Fundamental Plane is identical in all clusters. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP vanDokkum, PG (reprint author), KAPTEYN ASTRON INST,POB 800,NL-9700 AV GRONINGEN,NETHERLANDS. NR 70 TC 224 Z9 224 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 1996 VL 281 IS 3 BP 985 EP 1000 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VB271 UT WOS:A1996VB27100027 ER PT J AU Jeffries, RD Buckley, DAH James, DJ Stauffer, JR AF Jeffries, RD Buckley, DAH James, DJ Stauffer, JR TI 2RE J0241-525: A nearby post-T Tauri visual binary system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars, activity; stars, individual, 2RE J0241; 525; stars, late-type stars, pre-main-sequence; stars, rotation; X-rays, stars ID MAIN-SEQUENCE STARS; ALPHA-PERSEI CLUSTER; ALL-SKY SURVEY; LOW-MASS STARS; X-RAY; M-DWARFS; CHROMOSPHERIC ACTIVITY; LOCAL ASSOCIATION; UBVRI PHOTOMETRY; LITHIUM AB We present high-spatial-resolution X-ray observations, photometry and spectroscopy of the two low-mass, active stars proposed as optical counterparts to the extreme ultraviolet source 2RE J0241-525 (=EUVE J0241-530). It is confirmed that both stars, which are of types dK7e and dM3e and separated by 22 arcsec, are sources of soft X-ray emission and exhibit substantial chromospheric activity. Radial velocity measurements indicate that the two components are physically associated and most probably single. The projected equatorial velocities are measured as 75+/-3 and 11.7+/-0.7 km s(-1) for the hotter and cooler components respectively and, whilst the hotter component has a relatively high photospheric lithium abundance, log N(Li)=1.5+/-0.2, we are unable to detect any lithium in the cooler star. Isochrone fitting to this 'mini-cluster' yields an age of 3-70 Myr and a distance of 19-60 pc. An empirical comparison of the lithium abundances with those for similar stars in young clusters and associations suggests a narrower age range of 5-30 Myr and a corresponding distance of 26-50 pc. We conclude that this object is a nearby post-T Tauri system, but we cannot locate any possible birth site, It appears unlikely that the system can have been ejected from a nearby open cluster in a two-or three-body encounter. C1 S AFRICAN ASTRON OBSERV,ZA-7935 CAPE TOWN 7935,SOUTH AFRICA. UNIV BIRMINGHAM,SCH PHYS & SPACE RES,BIRMINGHAM B15 2TT,W MIDLANDS,ENGLAND. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP Jeffries, RD (reprint author), UNIV KEELE,DEPT PHYS,KEELE ST5 5BG,STAFFS,ENGLAND. NR 89 TC 9 Z9 9 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 1996 VL 281 IS 3 BP 1001 EP 1015 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VB271 UT WOS:A1996VB27100028 ER PT J AU Hershkovitz, MA Zimmer, EA AF Hershkovitz, MA Zimmer, EA TI Conservation patterns in angiosperm rDNA ITS2 sequences SO NUCLEIC ACIDS RESEARCH LA English DT Article ID INTERNAL TRANSCRIBED SPACER-2; PRECURSOR RIBOSOMAL-RNA; SACCHAROMYCES-CEREVISIAE; SPECIES COMPLEX; DNA-SEQUENCES; PHYLOGENY; EVOLUTION; CHLOROPHYTA; CONSTRAINTS; PLANTS AB The two internal transcribed spacers (ITS1 and ITS2) of nuclear ribosomal DNA have become commonly exploited sources of informative variation for interspecific-/intergeneric-level phylogenetic analyses among angiosperms and other eukaryotes, We present an alignment in which one-third to one-half of the ITS2 sequence is alignable above the family level in angiosperms and a phenetic analysis showing that ITS2 contains information sufficient to diagnose lineages at several hierarchical levels. Base compositional analysis shows that angiosperm ITS2 is inherently CC-rich, and that the proportion of T is much more variable than that for other bases, We propose a general model of angiosperm ITS2 secondary structure that shows common pairing relationships for most of the conserved sequence tracts. Variations in our secondary structure predictions for sequences from different taxa indicate that compensatory mutation is not limited to paired positions. C1 SMITHSONIAN INST,LAB MOL SYSTEMAT,WASHINGTON,DC 20560. RI Zimmer, Elizabeth/G-3890-2011 NR 49 TC 126 Z9 129 U1 0 U2 4 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0305-1048 J9 NUCLEIC ACIDS RES JI Nucleic Acids Res. PD AUG 1 PY 1996 VL 24 IS 15 BP 2857 EP 2867 DI 10.1093/nar/24.15.2857 PG 11 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA VB832 UT WOS:A1996VB83200001 PM 8760866 ER PT J AU Yan, ZC McKenzie, DK Drake, GWF AF Yan, ZC McKenzie, DK Drake, GWF TI Variational calculations of the Fermi contact term for the 2(2)S, 2(2)P, and 3(2)S states of Li and the 2(2)S state of Be+ SO PHYSICAL REVIEW A LA English DT Article ID HARTREE-FOCK CALCULATIONS; 2S GROUND-STATE; HYPERFINE-STRUCTURE; LITHIUM ATOM; MATRIX-ELEMENTS; RYDBERG STATES; MOMENTS; P-2; SPECTROSCOPY; CONSTANTS AB The Fermi contact term for the 2(2)S, 2(2)P, and 3(2)S states of Li and the 2(2)S state of Be+ are calculated using high-precision variational wave functions in Hylleraas coordinates. The nonrelativistic Fermi contact terms obtained for these states are 2.905 922(50), -0.214 783(50), 0.673 405(50), and 12.497 57(30) a.u., respectively. Estimates of corrections for finite nuclear size, relativistic effects, and QED effects are shown to yield satisfactory agreement with experiment for the 2(2)S state of Li and Be+, but there remains a substantial disagreement with experiment for the 3(2)S state of Li. C1 UNIV WINDSOR,DEPT PHYS,WINDSOR,ON N9B 3P4,CANADA. RP Yan, ZC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Yan, Zong-Chao/F-6668-2014 NR 44 TC 35 Z9 35 U1 1 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD AUG PY 1996 VL 54 IS 2 BP 1322 EP 1327 DI 10.1103/PhysRevA.54.1322 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA VD676 UT WOS:A1996VD67600034 ER PT J AU Greene, CS AF Greene, CS TI Exploring the three ''Little Bluffs'' of the Kiowa SO PLAINS ANTHROPOLOGIST LA English DT Article DE Kiowa; Southern Plains history; naming practices; material culture; Little Bluff AB Three Kiowa men who bore the name Tohausen, or Little Bluff, in the nineteenth century are frequently confused with each other in the literature, contributing to the difficulty of identifying the role of individual agency in Southern Plains history. Each of the Tohausens is here identified and their genealogical relationships are established. Distinguishing roles and events by which they can be differentiated are defined, and the passage of significant items of material culture among them is traced including shield and tipi designs. A discussion of Kiowa naming practices provides background for understanding how the name originated and was transmitted. RP Greene, CS (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ANTHROPOL,WASHINGTON,DC 20560, USA. NR 34 TC 3 Z9 3 U1 0 U2 0 PU PLAINS ANTHROPOLOGICAL SOC PI LINCOLN PA 410 WEDGEWOOD DRIVE, LINCOLN, NE 68510 SN 0032-0447 J9 PLAINS ANTHROPOL JI Plains Anthropol. PD AUG PY 1996 VL 41 IS 157 BP 221 EP 242 PG 22 WC Anthropology SC Anthropology GA VG675 UT WOS:A1996VG67500002 ER PT J AU NesmeRibes, E Baliunas, SL Sokoloff, D AF NesmeRibes, E Baliunas, SL Sokoloff, D TI The stellar dynamo SO SCIENTIFIC AMERICAN LA English DT Article C1 NATL CTR SCI RES,PARIS,FRANCE. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MT WILSON OBSERV,PASADENA,CA. MOSCOW MV LOMONOSOV STATE UNIV,DEPT PHYS,MOSCOW,RUSSIA. RP NesmeRibes, E (reprint author), OBSERV PARIS,PARIS,FRANCE. NR 4 TC 4 Z9 4 U1 0 U2 1 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 SN 0036-8733 J9 SCI AM JI Sci.Am. PD AUG PY 1996 VL 275 IS 2 BP 46 EP 52 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UX611 UT WOS:A1996UX61100029 ER PT J AU Hagedorn, M Hsu, EW Pilatus, U Wildt, DE Rall, WF Blackband, SJ AF Hagedorn, M Hsu, EW Pilatus, U Wildt, DE Rall, WF Blackband, SJ TI Magnetic resonance microscopy and spectroscopy reveal kinetics of cryoprotectant permeation in a multicompartmental biological system SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE zebrafish; yolk syncytial layer; conservation; cryopreservation ID YOLK SYNCYTIAL LAYER; NMR MICROSCOPY; DIFFUSION; CELLS; PERMEABILITY; FUNDULUS; ECHO AB Successful cryopreservation of most multicompartmental biological systems has not been achieved. One prerequisite for success is quantitative information on cryoprotectant permeation into and amongst the compartments, This report describes direct measurements of cryoprotectant permeation into a multicompartmental system using chemical shift selective magnetic resonance (MR) microscopy and MR spectroscopy. We used the developing zebrafish embryo as a model For studying these complex systems because these embryos are composed of two membrane-limited compartments: (i) a large yolk (surrounded by the yolk syncytial layer) and (ii) differentiating blastoderm cells (each surrounded by a plasma membrane). MR images of the spatial distribution of three cryoprotectants (dimethyl sulfoxide, propylene glycol, and methanol) demonstrated that methanol permeated the entire embryo within 15 min, In contrast, the other cryoprotectants exhibited little or no permeation over 2.5 h. MR spectroscopy and microinjections of cryoprotectants into the yolk inferred that the yolk syncytial layer plays a critical role in limiting the permeation of some cryoprotectants throughout the embryo. This study demonstrates the power of MR technology combined with micromanipulation for elucidating key physiological factors in cryobiology. C1 SMITHSONIAN INST,CONSERVAT & RES CTR,WASHINGTON,DC 20008. JOHNS HOPKINS UNIV,SCH MED,DEPT BIOMED ENGN,BALTIMORE,MD 21205. JOHNS HOPKINS UNIV,SCH MED,DEPT RADIOL,BALTIMORE,MD 21205. NATL CTR RES RESOURCES,VET RESOURCES PROGRAM,NIH,BETHESDA,MD 20892. UNIV HULL,DEPT MED PHYS,KINGSTON HULL HU3 2JZ,N HUMBERSIDE,ENGLAND. RP Hagedorn, M (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. FU NCRR NIH HHS [R29 RR08769] NR 24 TC 76 Z9 82 U1 0 U2 11 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 23 PY 1996 VL 93 IS 15 BP 7454 EP 7459 DI 10.1073/pnas.93.15.7454 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UY930 UT WOS:A1996UY93000007 PM 8755494 ER PT J AU Ohashi, N Hayashi, M Kawabe, R Ishiguro, M AF Ohashi, N Hayashi, M Kawabe, R Ishiguro, M TI The Nobeyama millimeter array survey of young stellar objects associated with the Taurus molecular cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM, individual (Taurus molecular cloud); ISM, molecules; radio lines, ISM; stars, pre-main-sequence ID SUBMILLIMETER-WAVELENGTH OBSERVATIONS; SMALL-SCALE STRUCTURE; FORMING DENSE CORES; MAIN-SEQUENCE STARS; T-TAURI; CIRCUMSTELLAR GAS; DARK CLOUDS; L1551 IRS-5; HL-TAURI; R-MONOCEROTIS AB We have carried out an interferometric survey of 3 mm continuum and CS (J = 2-1) line emissions from 13 optically invisible protostar candidates and six young T Tauri stars associated with the Taurus molecular cloud. The survey was made using the Nobeyama Millimeter Array with a spatial resolution of 2.'' 18-10 ''. The continuum emission was detected from two protostar candidates and five T Tauri stars and was well coincident with optical or infrared objects. It was not spatially resolved and most probably originated from compact circumstellar disks. The CS emission was detected around 11 protostar candidates and two T Tauri stars. The detected CS condensations are extended, with a typical size and mass of similar to 2000 AU and 0.01 M., respectively. Among the eleven protostar candidates with detectable CS emission, seven sources, i.e., IRAS 04016+2610 (L1489), IRAS 04169+2702, IRAS 04191+1503, IRAS 04239+2436, L1551-IRS 5, IRAS 04325+2402, and IRAS 04365+2535, have the CS emission well coincident with infrared sources, while the other four show the CS emission separated away from known infrared sources. Most of the CS emission for the former sources may arise from the innermost part of their protostellar envelopes, while that for the latter sources may originate from compact, dense gas in the vicinity of the infrared sources. The CS gases toward L1489 and IRAS 04365+2535 have disklike structures of similar to 1500 and similar to 500 AU in radius, respectively, with velocity gradients along their major axes. The velocity gradient of the disklike structure around L1489 may be due to rotation, while the origin of velocity gradient around IRAS 04365+2535 is not clear. L1551-IRS 5 shows compact CS emission, possibly arising from a disk, together with weak extended features that may be attributed to a denser part of the outflow. The distribution of CS emission around IRAS 04368+2557 (L1527) is anticorrelated with its molecular outflow, suggesting that the CS gas may be a dense shell swept up by the outflow. The 3 mm continuum detectability toward the protostar candidates is significantly smaller than what we would expect from the statistics of T Tauri disks, which we consider may be due to an evolutionary effect; namely, during the transitional phase from embedded protostars to revealed T Tauri stars, either the disk mass has rapidly increased, or dust particles in the disks have grown significantly, or both. For the embedded protostar candidates, the CS intensity is correlated with bolometric luminosity. This may mean that the final stellar mass is correlated with the mass of dense cores. C1 NOBEYAMA RADIO OBSERV, MINAMISA KU, MINAMI KAWACHI, TOCHIGI 38413, JAPAN. NATL ASTRON OBSERV, SUBARU PROJECT OFF, MITAKA, TOKYO 181, JAPAN. RP Ohashi, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 86 TC 56 Z9 56 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1996 VL 466 IS 1 BP 317 EP 337 DI 10.1086/177512 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UW721 UT WOS:A1996UW72100025 ER PT J AU Donahue, RA Saar, SH Baliunas, SL AF Donahue, RA Saar, SH Baliunas, SL TI A relationship between mean rotation period in lower main-sequence stars and its observed range SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, activity; stars, chromospheres; stars, late-type; stars, rotation ID STELLAR DIFFERENTIAL ROTATION; EMISSION-LINE FLUXES; K-EMISSION; TIME VARIATIONS; SERIES AB Chromospheric Ca II H and K fluxes have been measured in a sample of similar to 100 stars on or neat the lower main sequence at Mount Wilson Observatory. Observations were made several times a week and span more than 10 years. Within an observing season, many stars show periodic variations due to rotation. Thirty-six of the stars have highly significant periods in at least five seasons. We compute the range in the observed period, Delta P, and suggest that it is a measure of, and a lower limit to, the surface differential rotation. Several physical and selection effects can affect the measured Delta P value. An analysis of the cumulative variance distribution at various timescales, however, demonstrates that Ca II variations due to active region growth and decay are generally of longer period and smaller amplitude than those due to rotation. We argue that other effects (e.g., multiple active regions, latitude bands) either are small or primarily act to reduce the measured Delta P relative to its true value. Including results for the Sun, we find that Delta P depends on the mean seasonal rotation period [P] such that Delta P proportional to [P](1.3+0.1), independent of mass. We briefly discuss this result in the context of dynamo models, and other observations of surface differential rotation and active region structure. C1 TENNESSEE STATE UNIV, CTR EXCELLENCE INFORMAT SYST, NASHVILLE, TN 37203 USA. RP Donahue, RA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 52 TC 207 Z9 208 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1996 VL 466 IS 1 BP 384 EP 391 DI 10.1086/177517 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UW721 UT WOS:A1996UW72100030 ER PT J AU Mazeh, T Latham, DW Stefanik, RP AF Mazeh, T Latham, DW Stefanik, RP TI Spectroscopic orbits for three binaries with low-mass companions and the distribution of secondary masses near the substellar limit SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries, spectroscopic; stars, individual (HD 29587, HD 114762, HD 140913); stars, low-mass, brown dwarfs ID SOLAR-TYPE STARS; PRECISION RADIAL-VELOCITIES; GLOBULAR-CLUSTERS; SEARCH; MULTIPLICITY; NEIGHBORHOOD; HD-114762; FREQUENCY; DWARFS; GIANTS AB We present orbital solutions for three low-amplitude spectroscopic binaries discovered in a sample of 20 solar-type IAU radial velocity standard stars observed with the Digital Speedometers at the Harvard-Smithsonian Center for Astrophysics. We update the orbital solutions for HD 114762 and HD 140913, and present a preliminary new solution for HD 29587. For all three orbits, the minimum mass for the secondary is less than 0.08 M., the borderline between stellar and substellar masses. We consider the probability that all three binaries have small enough inclination angles so that their companions are above the substellar limit. To do so, we treat the 20 IAU standards as a sample drawn from a population of binaries with a mass-ratio distribution that does not allow any substellar companions. We calculate the probability that such a sample could still have three binaries, with the low-amplitude orbits actually found within the IAU sample. We show that this probability is small, depending on the specific mass-ratio distribution. For example, a flat mass-ratio distribution that assumes there are no substellar companions can be excluded at a high confidence level, 99.7%. We further show that our three detections may imply that the secondary-mass distribution rises near the substellar limit. However, the observations do not yet allow us to distinguish whether the unseen companions of HD 114762, HD 140913, and HD 29587 have stellar or substellar masses. In particular, recent attempts to estimate the mass of the companion of HD 114762 based on assumptions about the intrinsic rotation of the primary are inconclusive, and the companion could easily have a mass as low as 0.02 M.. We compare our three detections with the null results of four very precise radial velocity searches for substellar companions. The difference is indeed puzzling but can be accounted for if just a small fraction of the solar-type stars, of the order of a few percent, have companions with masses near the substellar limit. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. RP Mazeh, T (reprint author), TEL AVIV UNIV,RAYMOND & BEVERLY SACKLER FAC EXACT SCI,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. NR 64 TC 55 Z9 56 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1996 VL 466 IS 1 BP 415 EP 426 DI 10.1086/177521 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UW721 UT WOS:A1996UW72100034 ER PT J AU McNamara, BR Wise, M Sarazin, CL Jannuzi, BT Elston, R AF McNamara, BR Wise, M Sarazin, CL Jannuzi, BT Elston, R TI Optical structure in the Abell 1795 cluster central galaxy: Evidence for stripping and deflection of radio jets SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; galaxies, clusters, general; galaxies, cooling flows; radio continuum, galaxies ID RAY LUMINOUS CLUSTERS; COOLING FLOWS; SURFACE PHOTOMETRY; DOMINANT GALAXIES; COLOR GRADIENTS; SAMPLE; CORES AB We have obtained a deep U-band image of the central similar to 100 kpc of the Abell 1795 cluster central galaxy. This image shows several faint (mu(U) similar to 23-24 mag arcsec (-2)), thin structures, of unknown origin, that extend between 20 and 70 kpc into the galaxy's halo. Some are located along filaments of nebular line emission. Two structures, detected in the ground-based U-band image and in V and R images obtained with the WFPC2 on the Hubble Space Telescope (HST), extend toward faint, disturbed galaxies. The structures may be stripped stellar and gaseous debris from several sub-L* galaxies that are interacting with the central dominant galaxy, The lobes of blue optical continuum found earlier along the galaxy's radio lobes are resolved into bright knots on the HST images. The knots are probably composed of young stars. A dust lane lies along the edges of the radio jets and along the edge of the northern radio lobe. The dust and associated cold, dense gas may have deflected the radio jets and may have become entrained along the radio jets and lobes. The images strengthen recent arguments for radio-triggered star formation in A1795, and they raise the possibility that some of the accreted gas may have been stripped from neighboring galaxies. C1 MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. UNIV VIRGINIA,DEPT ASTRON,CHARLOTTESVILLE,VA 22903. NATL OPT ASTRON OBSERV,TUCSON,AZ 85726. CERRO TOLOLO INTERAMER OBSERV,LA SERENA,CHILE. RP McNamara, BR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 28 TC 40 Z9 40 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1996 VL 466 IS 1 BP L9 EP & DI 10.1086/310162 PN 2 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UW722 UT WOS:A1996UW72200003 ER PT J AU Press, WH AF Press, WH TI Blind watchers of the sky: The people and ideas that shaped our view of the universe - Kolb,R SO NATURE LA English DT Book Review RP Press, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 18 PY 1996 VL 382 IS 6588 BP 220 EP 220 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UX790 UT WOS:A1996UX79000037 ER PT J AU Press, WH AF Press, WH TI Our evolving universe - Longair,MS SO NATURE LA English DT Book Review RP Press, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 18 PY 1996 VL 382 IS 6588 BP 220 EP 220 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UX790 UT WOS:A1996UX79000038 ER PT J AU Patnaik, AR Schneider, P Narayan, R AF Patnaik, AR Schneider, P Narayan, R TI A deep radio observation of the gravitational lens candidate QSO 2345+007 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Letter DE cosmology, observations; dark matter; gravitational lensing ID BRIGHT QUASAR SURVEY; DARK-MATTER; DISCOVERY; CLUSTER AB The double QSO 2345 + 007 comprises two optical components separated by 7.1 arcsec, and is the most prominent 'dark matter' gravitational lens candidate. Despite being known for more than a decade, optical spectroscopy and imaging have been unable to determine whether this double QSO is a binary QSO or a gravitational lens system. In this note we report a deep VLA observation of this system, yielding a map with a noise level of 8.5 mu Jy beam(-1). We have a 4 sigma detection of a radio source within 0.4 arcsec of the optical position of the brighter A-component of the QSO, but no significant detection of any radio counterpart of the B-component. Given that the flux ratio in the optical waveband is similar to 3-4, the gravitational lens hypothesis for this system would predict a radio flux of image B of less than or similar to 10 mu Jy. The non-detection of the B-component is thus consistent with, but does not prove, the lens interpretation. C1 MAX PLANCK INST ASTROPHYS,D-85740 GARCHING,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Patnaik, AR (reprint author), MAX PLANCK INST ASTROPHYS,AUF HUGEL 69,D-53121 BONN,GERMANY. NR 22 TC 1 Z9 1 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 15 PY 1996 VL 281 IS 2 BP L17 EP L20 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UZ125 UT WOS:A1996UZ12500001 ER PT J AU Jungman, G Kamionkowski, M Kosowsky, A Spergel, DN AF Jungman, G Kamionkowski, M Kosowsky, A Spergel, DN TI Cosmological-parameter determination with microwave background maps SO PHYSICAL REVIEW D LA English DT Article ID COLD DARK-MATTER; LARGE-SCALE STRUCTURE; GRAVITATIONAL-WAVES; RADIATION; COBE; ANISOTROPIES; FLUCTUATIONS; SPECTRUM; UNIVERSE; SKY AB The angular power spectrum of the cosmic microwave background (CMB) contains information on virtually all cosmological parameters of interest, including the geometry of the Universe (Omega), the baryon density, the Hubble constant (h), the cosmological constant (Lambda), the number of light neutrinos, the ionization history, and the amplitudes and spectral indices of the primordial scalar and tensor perturbation spectra. We review the imprint of each parameter on the CMB. Assuming only that the primordial perturbations were adiabatic, we use a covariance-matrix approach to estimate the precision with which these parameters can be determined by a CMB temperature map as a function of the fraction of sky mapped, the level of pixel noise, and the angular resolution. For example, with no prior information about any of the cosmological parameters, a full-sky CMB map with 0.5 degrees angular resolution and a noise level of 15 mu K per pixel can determine Omega, h, and Lambda with standard errors of +/-0.1 or better, and provide determinations of other parameters which are inaccessible with traditional observations. Smaller beam sizes or prior information on some of the other parameters from other observations improves the sensitivity. The dependence on the underlying cosmological model is discussed. C1 COLUMBIA UNIV, DEPT PHYS, NEW YORK, NY 10027 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. HARVARD UNIV, LYMAN LAB PHYS, DEPT PHYS, CAMBRIDGE, MA 02138 USA. PRINCETON UNIV, DEPT ASTROPHYS SCI, PRINCETON, NJ 08544 USA. UNIV MARYLAND, DEPT ASTRON, COLLEGE PK, MD 20742 USA. RP SYRACUSE UNIV, DEPT PHYS, SYRACUSE, NY 13244 USA. RI Spergel, David/A-4410-2011 NR 71 TC 390 Z9 390 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUL 15 PY 1996 VL 54 IS 2 BP 1332 EP 1344 DI 10.1103/PhysRevD.54.1332 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA UY733 UT WOS:A1996UY73300012 ER PT J AU Wiseman, JJ Ho, PTP AF Wiseman, JJ Ho, PTP TI Heated gaseous streamers and star formation in the Orion molecular cloud SO NATURE LA English DT Article ID LARGE-SCALE INTERACTION; QUIESCENT GAS; FRAGMENTATION; REGION; NH3; ROTATION; NEBULA; OMC-1; CORES AB THE Orion molecular cloud, which is obscured by the dust and ionized gas of the Orion nebula, is the nearest example of a giant molecular cloud, Massive stars are actively forming deep in the core of this cloud as a result of large-scale cloud instabilities, fragmentation and gravitational collapse, These young stars will inject a considerable amount of energy back into the surrounding environment through stellar winds and radiation(1), and they are thus expected to exert a major influence on the evolution of the cloud, Here we present a mosaic of ten high-resolution radio maps of the region of the cloud known as OMC-1; the maps were constructed from observations of two ammonia emission lines, which trace the densest regions of the gas while mitigating the obscuring effects of the dust, We find dense filaments of molecular gas with complex motions fanning out more than 0.5 parsec from the central core of the cloud, These filaments appear as long, bead-like chains, consisting of dense clumps of gas that may be the sites of future star formation, The outer sheaths of clumps and the edges of filaments may be heated as a direct result of radiation and outflows from young stars embedded in the central core. C1 NATL RADIO ASTRON OBSERV,CHARLOTTESVILLE,VA 22903. RP Wiseman, JJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 27 TC 35 Z9 35 U1 0 U2 2 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD JUL 11 PY 1996 VL 382 IS 6587 BP 139 EP 141 DI 10.1038/382139a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UW672 UT WOS:A1996UW67200040 ER PT J AU Pyne, T Gwinn, CR Birkinshaw, M Eubanks, TM Matsakis, DN AF Pyne, T Gwinn, CR Birkinshaw, M Eubanks, TM Matsakis, DN TI Gravitational radiation and very long baseline interferometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; cosmology, theory; gravitation; techniques, interferometric; waves ID MICROWAVE BACKGROUND ANISOTROPY; GRAND UNIFICATION; WAVES AB Gravitational waves affect the observed direction of light from distant sources. At telescopes, this change in direction appears as periodic variations in the apparent positions of these sources on the sky; that is, as proper motion. A wave of a given phase, traveling in a given direction, produces a characteristic pattern of proper motions over the sky. Comparison of observed proper motions with this pattern serves to test for the presence of gravitational waves. A stochastic background of waves induces apparent proper motions with specific statistical properties, and so may also be sought. In this paper we consider the effects of a cosmological background of gravitational radiation on astrometric observations. We derive an equation for the time delay measured by two antennae observing the same source in an Einstein-de Sitter spacetime containing gravitational radiation. We also show how to obtain similar expressions for curved Friedmann-Robertson-Walker spacetimes. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106. USN OBSERV,WASHINGTON,DC 20392. OI Eubanks, Thomas Marshall/0000-0001-9543-0414 NR 28 TC 37 Z9 40 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP 566 EP 577 DI 10.1086/177443 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV063 UT WOS:A1996UV06300008 ER PT J AU Thoul, AA Weinberg, DH AF Thoul, AA Weinberg, DH TI Hydrodynamic simulations of galaxy formation .2. Photoionization and the formation of low-mass galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, formation; galaxies, kinematics and dynamics; hydrodynamics; radiative transfer ID COLD DARK-MATTER; COLUMN DENSITY DISTRIBUTION; INTERGALACTIC MEDIUM; EVOLUTION; QUASARS; FIELDS; CLOUDS; ORIGIN; GAS AB Photoionization by the high-redshift ultraviolet radiation background heats low- density gas before it falls into dark matter potential wells, and it eliminates the neutral hydrogen and singly ionized helium that dominate cooling of primordial gas at temperatures of 10(4)-10(5) K. We investigate the influence of photoionization on galaxy formation using high-resolution simulations with a one-dimensional, spherically symmetric, Lagrangian hydrodynamics/gravity code. We find that the presence of a photoionizing background suppresses the formation of galaxies with circular velocities v(circ) less than or similar to 30 km s(-1) and substantially reduces the mass of cooled baryons in systems with circular velocities up to v(circ) similar to 50 km s(-1). Above v(circ) similar to 75 km s(-1), photoionization has no significant effect. Photoionization exerts its influence primarily by heating gas before collapse; the elimination of line cooling processes is less important. We discuss the implications of these results for hierarchical theories of galaxy formation. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OHIO STATE UNIV,DEPT ASTRON,COLUMBUS,OH 43210. RP Thoul, AA (reprint author), INST ADV STUDY,PRINCETON,NJ 08540, USA. NR 36 TC 373 Z9 373 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP 608 EP 616 DI 10.1086/177446 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV063 UT WOS:A1996UV06300011 ER PT J AU Henriksen, M Jones, C AF Henriksen, M Jones, C TI An X-ray and optical study of clusters in formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies, clusters, individual (A3395, A3528); intergalactic medium; X-rays, galaxies ID GALAXY CLUSTERS; COOLING FLOWS; EVOLUTION; SIMULATION; DYNAMICS; EINSTEIN; GAS AB We present an analysis of observations by the ROSAT Position Sensitive Proportional Counter (PSPC) of subclusters in bimodal systems A3395 (SC 0627-54) and A3528 (SC 1252-28). The best-fit temperatures range from 2 to 4 keV and are the first temperature measurements for this class of objects. The gas is detected out to 300 kpc (A3395) and 650 kpc (A3528) from the center of the subclusters, but this is likely not the full extent of the gas. Therefore, we have determined masses for the subclusters, assuming the gas is isothermal, of similar to 1.0 x 10(14) h(75)(-1) M(.) within 0.5 Mpc and similar to 2.1 x 10(14) h(75)(-1) M(.) within 1.0 Mpc. The average baryon fraction in gas is similar to 0.09 h(75)(-3/2) within 0.5 Mpc and similar to 0.14 h(75)(-3/2) within 1.0 Mpc. The average baryon fraction in gas is consistent with the central regions of rich, evolved clusters and suggests that the merger process does not appreciably increase the gas baryon fraction. The velocity dispersion of each subcluster is comparable to that found for rich clusters. The masses we have calculated from the optical data using three different estimators are larger than those from the X-ray data because of the larger velocity dispersion of the subclusters. Since the velocity dispersions are comparable to the difference in the mean velocities because of the Hubble flow, we have imposed a radial cutoff; this reduces, but does not remove, the conflict between the optically and X-ray-derived masses, suggesting that the galaxy velocity dispersions are contaminated by the component of radial infall along the line of sight. A dynamical analysis of the A3395 cluster using the X-ray-determined masses indicates that the subclusters will fully merge in 0.3-1.2 Gyr; this is consistent with an early stage of merger which is implied by the elongation of the X-ray emission perpendicular to the merger axis resulting from the collision of the hot atmospheres. If the merger product has a mass similar to the sum of the individual subclusters, then the merger product will be a low-mass rich cluster, which is strong support for rich clusters forming from the ''bottom up.'' Extending the dynamical analysis to include the cluster SC 0625-53 (A3391), which is similar to 2.8 h(75)(-1) Mpc away in projection, suggests that this cluster and the A3395 cluster form a bound, infalling system if they have again as much mass beyond 1 Mpc as within that radius. The improved spectral and spatial resolution of the ROSAT PSPC allows a determination of the cooling time in the central region of the subclusters. The subcluster cooling times are slightly longer than 10 Gyr, the nominal age of the cluster atmosphere, suggesting that cooling flows with mass accretion rates similar to nearby clusters are not present during this premerger stage or that they have been disrupted. Small cooling flows on the order of a few solar masses are not ruled out. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02115. RP Henriksen, M (reprint author), UNIV N DAKOTA,DEPT PHYS,GRAND FORKS,ND 58202, USA. NR 35 TC 16 Z9 16 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP 666 EP 679 DI 10.1086/177452 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV063 UT WOS:A1996UV06300017 ER PT J AU Magnani, L Caillault, JP Hearty, T Stauffer, J Schmitt, JHMM Neuhauser, R Verter, F Dwek, E AF Magnani, L Caillault, JP Hearty, T Stauffer, J Schmitt, JHMM Neuhauser, R Verter, F Dwek, E TI A search for star formation in the translucent cloud MBM 40 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, clouds; ISM, individual (MBM 40); ISM, molecules; radio lines, ISM; stars, formation; stars, pre-main-sequence; X-rays, stars ID LATITUDE MOLECULAR CLOUDS; T-TAURI STARS; MEDIUM SENSITIVITY SURVEY; HIGH GALACTIC LATITUDES; X-RAY SURVEY; CIRRUS CLOUDS; DARK CLOUDS; NH3 OBSERVATIONS; INFRARED CIRRUS; HIGH-VELOCITY AB The star formation status of the translucent high-latitude molecular cloud, MBM 40, is explored through analysis of radio, infrared, optical, and X-ray data. With a peak visual extinction of 1 to 2 mag, MBM 40 is an example of a high-latitude cloud near the diffuse/translucent demarcation. However, unlike most translucent clouds, MBM 40 exhibits a compact morphology and a kinetic energy-to-gravitational potential energy ratio near unity. Our radio data, encompassing the CO (J = 1-0), CS (J = 2-1), and H2CO 1(11)-1(10) spectral line transitions, reveal that the cloud contains a ridge of molecular gas with n greater than or equal to 10(3) cm(-3). In addition, the molecular data, together with IRAS data, indicate that the mass of MBM 40 is similar to 40 M.. In light of the ever-increasing number of recently formed stars far from any dense molecular clouds or cores, we searched the environs of MBM 40 for any trace of recent star formation. We used the ROSAT All-Sky Survey X-ray data and a ROSAT PSPC pointed observation toward MBM 40 to identify 33 stellar candidates with properties consistent with pre-main-sequence (PMS) stars. Follow-up optical spectroscopy of the candidates with V < 15.5 was conducted with the 1.5 m Fred Lawrence Whipple Observatory telescope in order to identify signatures of T Tauri or pre-main-sequence stars (such as the Li 6708 Angstrom resonance line). Since none of our optically observed candidates display standard PMS signatures, we conclude that MBM 40 displays no evidence of recent or ongoing star formation. The absence of high-density molecular cores in the cloud and the relatively low column density compared to star-forming interstellar clouds may be the principal reasons that MBM 40 is devoid of star formation. More detailed comparison between this cloud and other, higher extinction translucent and dark clouds may elucidate the necessary initial conditions for the onset of low-mass star formation. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP Magnani, L (reprint author), UNIV GEORGIA,DEPT PHYS & ASTRON,ATHENS,GA 30602, USA. NR 85 TC 13 Z9 13 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP 825 EP 839 DI 10.1086/177466 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV063 UT WOS:A1996UV06300031 ER PT J AU Slane, P Vancura, O Hughes, JP AF Slane, P Vancura, O Hughes, JP TI A study of the evolutionary state of the supernova remnant G299.2-2.9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual (G299.2-2.9); supernova remnants; X-rays, ISM ID CLOUDS AB Using archival data from the Einstein Slew Survey (ESS) and the Infrared Astronomical Satellite (IRAS), as well as results from the ROSAT All-Sky Survey (Busser et al.), we present an investigation of the newly discovered supernova remnant (SNR) G299.2 - 2.9. The object appears morphologically similar in the IR and X-ray bands, with a partially complete shell that is brightest in the northeast. The radio morphology is also similar, although a bright region in the western portion of the remnant is also evident. Results reported from the ROSAT Position Sensitive Proportional Counter (PSPC) observation include a low value for the line-of-sight interstellar column density, suggestive of a nearby remnant (distance similar to 0.5 kpc), leading Busser et al. to conclude G299.2-2.9 is a young remnant that has not yet entered the adiabatic stage of evolution. We investigate the properties expected from such a scenario and find that the results imply an extremely underluminous SNR. As an alternative, we consider an interpretation whereby the SNR is at a larger distance and in the Sedov phase of evolution. Using a model for a nonradiative shock propagating through a dusty interstellar medium, we show that a self-consistent model can reproduce the X-ray and IR fluxes. We discuss the plausibility of each of these models and propose observational tests to differentiate between the two scenarios. RP Slane, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 16 TC 6 Z9 6 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP 840 EP 844 DI 10.1086/177467 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV063 UT WOS:A1996UV06300032 ER PT J AU Vrtilek, SD Cheng, FH AF Vrtilek, SD Cheng, FH TI The ultraviolet/optical continuum of Hercules X-1 HZ Herculis SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, individual (Her X-1 = HZ Her); ultraviolet, stars ID X-RAY SOURCES; MULTIWAVELENGTH CAMPAIGN; LOW STATE; IUE; ACCRETION; UHURU AB We present observations of the binary X-ray pulsar system Hercules X-1/HZ Herculis taken with the International Ultraviolet Explorer (IUE) and several ground-based observatories as part of a multiwavelength campaign conducted in 1993 August. The 1993 campaign found the source in an unusual state, with substantially reduced X-ray flux, and also revealed a significant reduction in ultraviolet flux observed around eclipse ingress and egress, which implies an absence of the normally observed excess attributed to X-ray heating of the disk. Comprehensive modeling of the ultraviolet and optical continuum flux suggests that the ultraviolet and optical light curves can be reproduced by assuming variations in M alone; however, changes in accretion rate are insufficient to account for the observed drop in X-ray flux. Shifts in disk inclination angle and changes in mass accretion rate can consistently explain the observed changes in X-ray, ultraviolet, and optical fluxes. Changes in mass accretion rate and disk inclination angle may be related to shifts in the 35 day precession period, with the average mass accretion rate corresponding to the average 35 day period. The rapid fluctuations in soft X-ray flux, observed several times during the campaign, may be caused by rapid variation of the mass accretion rate. C1 VILLANOVA UNIV,DEPT ASTRON,VILLANOVA,PA 19085. SHANGHAI JIAO TONG UNIV,INST SPACE SCI,SHANGHAI 200030,PEOPLES R CHINA. RP Vrtilek, SD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 32 TC 25 Z9 25 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP 915 EP 925 DI 10.1086/177475 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV063 UT WOS:A1996UV06300040 ER PT J AU Gray, DF Baliunas, SL Lockwood, GW Skiff, BA AF Gray, DF Baliunas, SL Lockwood, GW Skiff, BA TI Magnetic, photometric, temperature, and granulation variations of xi Bootis A 1984-1993 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, individual (xi Bootis); stars, late-type; stars, magnetic fields ID SPECTRAL-LINE ASYMMETRIES; K-DWARFS; STELLAR GRANULATION; COOL STARS; FIELDS; ROTATION; EMISSION; SEARCH AB The magnetically active G8 dwarf star, xi Boo A = HR 5544 = HD 131156 is studied for magnetic-cycle type variations over the 1984-1993 interval. We present measurements of Ca II H and K emission as an indirect indicator of magnetic activity, blue and visual magnitudes as an indication of the power output and temperature, line-depth ratios of V I lambda 6251.83 to Fe I lambda 6252.57 as a measure of temperature, and line bisectors as a measure of the star's granulation. The season means of all these parameters show the same pattern of variation with several irregular rises and falls, rather different from the relatively smooth variations seen for the Sun. As found for several other stars in previous studies, the magnetic signal leads the others in time. Time lags relative to the H and K index variation are 1.4 +/- 0.4 yr for the photometric brightness, 1.5 +/- 0.5 yr for the b - y color index, 1.8 +/- 0.3 yr for the line-depth ratio, and 2.1 +/- 0.4 yr for the line bisectors. The approximate to 1.7 year temperature lag for xi Boo A is close to the linear relation between lag and effective temperature found for the other stars that have been measured. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. LOWELL OBSERV, FLAGSTAFF, AZ 86001 USA. RP Gray, DF (reprint author), UNIV WESTERN ONTARIO, DEPT ASTRON, LONDON, ON N6A 3K7, CANADA. NR 44 TC 41 Z9 41 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP 945 EP 950 DI 10.1086/177478 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV063 UT WOS:A1996UV06300043 ER PT J AU Vrtilek, SD Silber, A Primini, F Raymond, JC AF Vrtilek, SD Silber, A Primini, F Raymond, JC TI ROSAT PSPC observations of the intermediate polar TV Columbae SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae; cataclysmic variables; stars, individual (TV Columbae); ultraviolet, stars; X-rays, stars ID MAGNETIC CATACLYSMIC VARIABLES; RECOMBINATION-LINE-INTENSITIES; X-RAY SOURCES; ACCRETION DISKS; HYDROGENIC IONS; IUE; ULTRAVIOLET; RADIATION AB The intermediate polar TV Columbae was observed for 8640s with the ROSAT PSPC. The best-fitting model to the 0.1-2.0 keV spectrum combines a power law with photon index alpha = 0.82 and a 54 eV blackbody, both observed through a column density of 4.6 x 10(20) cm(-2). No evidence is seen for line emission from the Fe L-shell complex. We observe an X-ray/optical flux ratio of 0.2: our measured X-ray photon flux is not sufficient to produce the He II lambda 1640 recombination line flux found by IUE. Some of the missing X-ray flux can be attributed to absorption in an accretion curtain. An additional very soft EUV component (e.g., a 20 eV blackbody) could provide sufficient photons in the 55-100 eV band to account for most of the He II luminosity while remaining hidden to the PSPC and IUE. A second possibility is that the X-ray flux is indeed small and collisional excitation accounts for 80% of the He II lambda 1640 flux. Because of instrumental difficulties, we are unable to confirm the 32 minute period observed with EXOSAT and attributed to rotation of the white dwarf. C1 UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195. RP Vrtilek, SD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Primini, Francis/0000-0002-6077-0643 NR 41 TC 6 Z9 6 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP 951 EP 955 DI 10.1086/177479 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV063 UT WOS:A1996UV06300044 ER PT J AU Kohl, JL Strachan, L Gardner, LD AF Kohl, JL Strachan, L Gardner, LD TI Measurement of hydrogen velocity distributions in the extended solar corona SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; sun, corona; sun, UV radiation AB H I Ly alpha spectral line profiles have been measured in polar regions of the solar corona at projected heliocentric heights of 1.8-3.5 R(.). Observations were made with the Ultraviolet Coronal. Spectrometer on the Spartan 201 satellite from 16:52 to 04:04 UT on 1993 April 11-12 (south pole) and from 12:28 to 22:09 UT on 1993 April 12 (north pole). In general, the coronal profiles cannot be accurately curve-fitted with a single-Gaussian function. The fits with two Gaussians yield most probable velocities of 158 and 322 km s(-1) (south) and 98 and 266 km s(-1) (north). These parameters vary by less than 10% (1 sigma) over the observed heights. The observations are consistent with a line-of-sight model that attributes the narrow component to background streamers and to sites within polar coronal holes or a surrounding diffuse corona, and the broad component to the polar coronal holes and/or plumes. This interpretation suggests that there are regions within the observed coronal holes that have hydrogen and proton kinetic temperatures of (4-6) x 10(6) K, which is 4-10 times higher than the expected electron temperatures at the same heights. However, other models with, for example, local non-Maxwellian velocity distributions are also consistent with the observations. RP Kohl, JL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 15 TC 56 Z9 56 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP L141 EP L144 DI 10.1086/310145 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV064 UT WOS:A1996UV06400015 ER PT J AU Menten, KM Reid, MJ AF Menten, KM Reid, MJ TI Formaldehyde absorption at z=0.685 toward the ''Einstein ring'' B0218+357 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars, absorption lines; radio lines, galaxies ID MOLECULAR CLOUDS; DARK CLOUDS AB We report VLA observations of absorption in the 2(11) --> 2(12) transition of formaldehyde (H2CO) at a redshift of 0.68466 toward the Einstein ring gravitational lens system B0218+357. We observe the H2CO line at 8.6 GHz only toward the stronger of the two compact images of this system. The column densities of H2CO and other molecules previously observed at millimeter wavelengths, as well as their relative abundances, are comparable to the values one finds for molecular clouds within the Milky Way. We argue that the material seen in absorption has a molecular hydrogen column density between 5 x 10(21) and 5 x 10(22) cm(-2). RP Menten, KM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 TC 48 Z9 48 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP L99 EP L102 DI 10.1086/310147 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV064 UT WOS:A1996UV06400005 ER PT J AU Myers, PC Mardones, D Tafalla, M Williams, JP Wilner, DJ AF Myers, PC Mardones, D Tafalla, M Williams, JP Wilner, DJ TI A simple model of spectral-line profiles from contracting clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, molecules; line, profiles; stars, formation ID COLLAPSE AB A simple analytic model of radiative transfer in two parts of a contracting cloud matches a wide range of line profiles in candidate infall regions and provides a sensitive estimate of V-in, the characteristic inward speed of the gas forming the line. The model assumes two uniform regions of equal temperature and velocity dispersion sigma, whose density and velocity are attenuation-weighted means over the front and rear halves of a centrally condensed, contracting cloud. The model predicts two-peak profiles for ''slow'' infall, V-in much less than sigma and red-shoulder profiles for ''fast'' infall, V-in similar to sigma A simple formula expresses V-in solely in terms of sigma and of observable parameters of a two-peak line. We apply the model to fit profiles of high and low optical depth lines observed in a dense core with no star (L1544, V-in = 0.006 km s(-1)), with an isolated protostar (L1527, 0.025 km s(-1)), and with a small group of stars (L1251B, 0.35 km s(-1)). The mass infall rate obtained from V-in and the map size varies from (2-40) x 10(-6) M(.) yr(-1) and agrees within a factor similar to 2 in each core with the independently determined rate similar to sigma(3) G(-1) for a gravitationally collapsing isothermal sphere. This agreement suggests that the inward motions derived from the line profiles are gravitational in origin. RP Myers, PC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Williams, Jonathan/B-1643-2009; Mardones, Diego/I-5719-2016; OI Williams, Jonathan/0000-0001-5058-695X NR 22 TC 114 Z9 114 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1996 VL 465 IS 2 BP L133 EP L136 DI 10.1086/310146 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV064 UT WOS:A1996UV06400013 ER PT J AU Colinvaux, P AF Colinvaux, P TI Biogeography - Low-down on a land bridge SO NATURE LA English DT Editorial Material RP Colinvaux, P (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 3 TC 21 Z9 22 U1 1 U2 3 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD JUL 4 PY 1996 VL 382 IS 6586 BP 21 EP & DI 10.1038/382021a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UV473 UT WOS:A1996UV47300029 ER PT J AU Steponaitis, VP Blackman, MJ Neff, H AF Steponaitis, VP Blackman, MJ Neff, H TI Large-scale patterns in the chemical composition of Mississippian pottery SO AMERICAN ANTIQUITY LA English DT Article ID CERAMICS AB Neutron activation analysis of Mississippian sheds from 21 regions across the Southeast has revealed the existence of distinctive chemical groups that are associated with four large geographical areas. One such group is associated with sites along the Mississippi River and its western tributaries, a second is associated with sites on the Appalachian Rim in Tennessee, a third is associated with sites on the Piedmont and associated drainages, and a fourth is associated with sites in Alabama. This pattern reflects the existence of several large, clay-mineral provinces in the Southeast that now can be recognized as sources in future studies of long-distance exchange. C1 SMITHSONIAN INST, CONSERVAT ANALYT LAB, WASHINGTON, DC 20560 USA. UNIV MISSOURI, RES REACTOR CTR, COLUMBIA, MO 65211 USA. RP Steponaitis, VP (reprint author), UNIV N CAROLINA, RES LABS ANTHROPOL, CHAPEL HILL, NC 27599 USA. NR 63 TC 35 Z9 35 U1 0 U2 1 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 0002-7316 J9 AM ANTIQUITY JI Am. Antiq. PD JUL PY 1996 VL 61 IS 3 BP 555 EP 572 DI 10.2307/281840 PG 18 WC Anthropology; Archaeology SC Anthropology; Archaeology GA VM077 UT WOS:A1996VM07700009 ER PT J AU Prado, J Lellinger, DB AF Prado, J Lellinger, DB TI Observations on the nomenclature and taxonomy of Gleichenia nigropaleacea SO AMERICAN FERN JOURNAL LA English DT Article AB Nomenclature of the Brazilian endemic, Gleichenia nigropaleacea, is summarized, and it is transferred to the genus Sticherus. The distinctness of the species is discussed, and it is contrasted with the related Sticherus brevipubis of Mexico and Central America and S. remotus of the Guianas and Brazil. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560. RP Prado, J (reprint author), INST BOT,SECAO BRIOL & PTERIDOL,CAIXA POSTAL 4005,BR-01061 SAO PAULO,BRAZIL. RI Prado, Jefferson/C-4766-2012 OI Prado, Jefferson/0000-0003-4783-3125 NR 4 TC 2 Z9 3 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD JUL-SEP PY 1996 VL 86 IS 3 BP 98 EP 101 DI 10.2307/1547643 PG 4 WC Plant Sciences SC Plant Sciences GA VT078 UT WOS:A1996VT07800004 ER PT J AU Wagner, RH Schug, MD Morton, ES AF Wagner, RH Schug, MD Morton, ES TI Confidence of paternity, actual paternity and parental effort by purple martins SO ANIMAL BEHAVIOUR LA English DT Article ID EXTRAPAIR FERTILIZATIONS; POLYANDROUS DUNNOCKS; AGELAIUS-PHOENICEUS; PRUNELLA-MODULARIS; MATING SYSTEM; CARE; BEHAVIOR; EVOLUTION; CERTAINTY; COPULATIONS AB Parental effort by socially monogamous purple martins was measured to test the hypothesis that males reduce care in response to their risk of losing paternity through extra-pair copulations. Male martins occur in two age classes, with one-year-old males cuckolded in very high frequencies and older males achieving nearly complete paternity. This outcome is because females paired to young males pursue a mixed mating strategy of seeking extra-pair copulations, and females paired to old males avoid extra-pair copulations. Using multi-locus DNA fingerprinting to determine paternity, nb evidence was found that males reduced effort according to actual paternity or presumed confidence of paternity. Young and old males provisioned nestlings at similar rates in relative and absolute terms. There was also no relationship within the young age class, with young males provisioning similarly regardless of whether they were cuckolded. Young males achieving zero paternity provisioned similarly to young males achieving partial and complete paternity, suggesting that no threshold effect exists. Although several conditions have been proposed under which no relationship between paternity and male care is expected, these conditions did not exist for purple martins. Another condition under which males should not reduce care to unrelated offspring is proposed, namely, that performing poorly in the presence of potential future mates or extra-pair copulation partners can lower social status and thereby fitness. The 'status hypothesis' provides a perspective for viewing parental performance as a behavioural character on which sexual selection operates. (C) 1996 The Association for the Study of Animal Behaviour. C1 OHIO STATE UNIV,DEPT ZOOL,COLUMBUS,OH 43210. SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RP Wagner, RH (reprint author), YORK UNIV,DEPT BIOL,N YORK,ON M2M 1P3,CANADA. NR 51 TC 63 Z9 63 U1 1 U2 12 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUL PY 1996 VL 52 BP 123 EP 132 DI 10.1006/anbe.1996.0158 PN 1 PG 10 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA VA497 UT WOS:A1996VA49700012 ER PT J AU Allen, LA Geller, MJ AF Allen, LA Geller, MJ TI The rotation velocity-density relation SO ASTRONOMICAL JOURNAL LA English DT Article ID COLD DARK-MATTER; PISCES-PERSEUS SUPERCLUSTER; 21 CM SURVEY; NEUTRAL HYDROGEN; ISOLATED GALAXIES; SPIRAL GALAXIES; DISTANCE SCALE; WIDTH RELATION; RICH CLUSTERS; UNIVERSE AB We have assembled 21-cm linewidths for 376 of the 732 galaxies in a magnitude-limited redshift survey of the Perseus-Pisces region. We analyze a distance limited subset of 271 galaxies (131 widths) to examine the relationship between linewidth and local density. The sample indicates that galaxies with linewidths greater than or similar to 480 km/s are absent from regions where the galaxy density is less than or similar to 0.03 galaxies Mpc(-3) (M(B(0)) < -18.3). This effect is in the direction predicted by standard CDM models. Galaxies with linewidths less than or similar to 480 km/s appear throughout the sample. The observational constraints could be substantially improved with a larger sample, IR photometry, and more uniform 21-cm data. (C) 1996 American Astronomical Society. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 43 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUL PY 1996 VL 112 IS 1 BP 1 EP 8 DI 10.1086/117984 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UU510 UT WOS:A1996UU51000001 ER PT J AU McNamara, BR OConnell, RW Sarazin, CL AF McNamara, BR OConnell, RW Sarazin, CL TI Optical, radio, and X-ray structure in NGC 1275 SO ASTRONOMICAL JOURNAL LA English DT Article ID CENTRAL CLUSTER GALAXIES; HIGH-VELOCITY SYSTEM; YOUNG STAR CLUSTER; COOLING FLOWS; DOMINANT GALAXIES; PERSEUS CLUSTER; LINE EMISSION; NGC-1275; FILAMENTS; REDSHIFT AB We have compiled U, I, H alpha, radio, and x-ray maps of NGC 1275 in order to study the galaxy's structure and color distribution. There are strong indications that the radio source is interacting with the gaseous medium in NGC 1275. A similar or equal to 2 mag spread in U-I color is found across the face of the galaxy. The brightest and bluest structure in the U-band image is located along the northern radio lobes and cavity walls in the x-ray emission. Correspondingly bright features are absent along the southern radio lobe. The low velocity H alpha emission avoids the cavities in the x-ray emission occupied by the radio lobes. The global distribution of excess blue light, Ha emission, and brightest x-ray emission occur over similar spatial scales (similar to 30-40 kpc). However, the x-ray and optical structures are not correlated in detail. We have detected a faint blue continuum from the outer, ''crab-like'' low velocity filaments, which may signal ongoing star formation there. In addition, we have detected blue continuum toward the high velocity emission regions, perhaps from stars associated with the high velocity gas. Dark features, probably associated with dust, surround the nucleus and extend in filaments to the north-west. We suggest the dust surrounding the nucleus is associated with NGC 1275 itself, whereas the dust to the north-west may be associated with the high velocity system. The color distribution is consistent with population ages ranging from similar to 10 Myr to 1 Gyr superposed on an older, elliptical background population. The formation of the youngest (brightest, bluest) population along the radio lobes may have been induced by shock compression of cold gas along the northern radio lobe. This interpretation is complicated, however, by the superposition of light toward both high and low velocity gas to the north-west of the nucleus and the pole-on aspect of the radio source. The cooling rate of the x-ray-emitting gas in the central 20 kpc or so is comparable to the estimated star formation rates over the past several hundred Myr. However, the x-ray structure is more complicated than simple cooling flow models would predict, and there an indications that the dense x-ray structures are falling into the galaxy and have not had time to cool. A merger with a gas-enriched galaxy [Holtzman et al. AJ, 103, 691 (1992)] may have contributed to the structure. (C) 1996 American Astronomical Society. C1 UNIV VIRGINIA, DEPT ASTRON, CHARLOTTESVILLE, VA 22903 USA. RP McNamara, BR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 70 TC 41 Z9 41 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1996 VL 112 IS 1 BP 91 EP + DI 10.1086/117991 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UU510 UT WOS:A1996UU51000008 ER PT J AU Evans, NR Holberg, JB Polidan, RS AF Evans, NR Holberg, JB Polidan, RS TI Voyager observations of the companion of the classical cepheid S muscae SO ASTRONOMICAL JOURNAL LA English DT Article ID FAR-ULTRAVIOLET SPECTROPHOTOMETRY; STARS; MASS AB We have observed the companion of the Cepheid S Mus with the Voyager ultraviolet spectrometer, including a spectrum of the background. We have derived the energy distribution from 912 to 3200 Angstrom using the reddening obtained from Cepheid colors corrected for the effect of the companion. This has been compared with three Morgan-Keenan ''dagger'' spectral standards of appropriate spectral types. The addition of the Voyager flux to the energy distribution provides a clear discriminant between B3 and B5, and shows that S Mus B is a good match to both of the B3 V spectral standards. Although there is some uncertainty in the H-2 absorption correction, even the S Mus B spectrum uncorrected for H-2 absorption has more flux at 1000 Angstrom than the B5 star. (C) 1996 American Astronomical Society. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. UNIV ARIZONA,LUNAR & PLANETARY LAB,TUCSON,AZ 85721. NASA,GODDARD SPACE FLIGHT CTR,LAB ASTRON & SPACE PHYS,GREENBELT,MD 20771. RP Evans, NR (reprint author), YORK UNIV,DEPT PHYS & ASTRON,4700 KEELE ST,N YORK,ON M3J 1P3,CANADA. NR 24 TC 4 Z9 4 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1996 VL 112 IS 1 BP 264 EP 268 DI 10.1086/118009 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UU510 UT WOS:A1996UU51000026 ER PT J AU Barret, D Grindlay, JE AF Barret, D Grindlay, JE TI ROSAT-HRI observations of SIGMA hard X-ray sources of the Galactic Center region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galactic Center; X-rays, stars; stars, individual, GRS1734-292, GRS1747-341, and GRS1743-290; black hole physics ID STARS AB We report on the ROSAT HRI observations of three Galactic Center hard X-ray sources discovered by the ARTP/SIGMA experiments aboard the GRANAT satellite, namely GRS1734-292, GRS1747-341, and GRS 1743-290. We found a possible counterpart for GRS 1734-292 located at a position alpha = 17(h) 37(mn) 28.2(s) and delta = -29 degrees 08' 03.1 '' (equinox 2000) with an associated error radius of 3 arcsec (90% confidence level). The HRI X-ray flux is consistent with previous measurements by ART-P. This variable source was also clearly detected during two PSPC pointed observations of the Galactic Center region. Although the significance of our detection is low (similar to 3 sigma), we may have also an X-ray counterpart for the persistent SIGMA source GRS 1747-341; its position would be alpha = 17(h) 50(mn) 55.0(s) and delta = -34 degrees 11' 37.0 '' (equinox 2000) with an associated error radius of 5.5 arcsec (90% confidence level). On the other hand, we failed to detect GRS1743-290; another sourer which displays persistent emission in the SIGMA hard X-ray band. This result is consistent with the source being highly absorbed as suggested by previous observations. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Barret, D (reprint author), CTR ETUD SPATIALE RAYONNEMENTS, CNRS, UPS, 9 AVE COLONEL ROCHE, BP 4346, F-31029 TOULOUSE, FRANCE. NR 19 TC 4 Z9 4 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 1996 VL 311 IS 1 BP 239 EP 244 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UV894 UT WOS:A1996UV89400024 ER PT J AU Wallington, S Kochanek, CS Narayan, R AF Wallington, S Kochanek, CS Narayan, R TI LensMEM: A gravitational lens inversion algorithm using the maximum entropy method SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; methods, numerical ID DARK MATTER AB We present a new algorithm for inverting poorly resolved gravitational lens systems using the maximum entropy method. We test the method with simulations and then apply it to an 8 CHz VLA map of the radio ring lens MG 1654+134. We model the lens as a singular isothermal sphere embedded in an external shear held and find that the critical radius of the lens is b = 0 ''.9820, the dimensionless shear is gamma = 0.0771, and the position angle of the shear is theta = 100 degrees.8. These results are consistent with the results obtained by Kochanek using a complementary inversion algorithm based on Clean. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 25 TC 42 Z9 42 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1996 VL 465 IS 1 BP 64 EP 72 DI 10.1086/177401 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UR889 UT WOS:A1996UR88900006 ER PT J AU Esin, AA Narayan, R Ostriker, E Yi, I AF Esin, AA Narayan, R Ostriker, E Yi, I TI Hot one-temperature accretion flows around black holes SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; radiation mechanisms, thermal ID PAIR EQUILIBRIUM; BINARY-SYSTEMS; SOFT PHOTONS; CYGNUS X-1; DISKS; COMPTONIZATION; PLASMAS; ORIGIN; MODEL AB We describe hot, optically thin solutions for one-temperature accretion disks around black holes. We include cooling by synchrotron, bremsstrahlung, and Comptonization. Our solutions are thermally and viscously stable, with gas temperatures on the order of T similar to 10(9) - 10(10.7) K. The thermal stability is a direct result of the inclusion of synchrotron cooling. The new solution branch is related to the advection-dominated solution for a two-temperature gas, described by Narayan & Yi (1995b). It is present only for mass accretion rates less than some critical M(crit), which depends on the radius R and viscosity parameter alpha. The solutions are advection dominated for extremely low values of M. However, for a range of intermediate accretion rates, the new solutions are both hot (T similar to 10(10) K and cooling dominated. Because of this new feature, one-temperature solutions are significantly more luminous than the corresponding two-temperature solutions at the same M. The radial profile of the new solutions is unusual. The inner parts of the flow are cooling-dominated and have a disklike geometry, while the outer parts are fully advection-dominated and nearly quasi-spherical. C1 INST ADV STUDY, PRINCETON, NJ 08540 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 47 TC 56 Z9 56 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1996 VL 465 IS 1 BP 312 EP 326 DI 10.1086/177421 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UR889 UT WOS:A1996UR88900026 ER PT J AU Mahadevan, R Narayan, R Yi, I AF Mahadevan, R Narayan, R Yi, I TI Harmony in electrons: Cyclotron and synchrotron emission by thermal electrons in a magnetic field SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; plasmas; radiation mechanisms, thermal AB We present a complete solution to the cyclotron-synchrotron radiation that results from an isotropic distribution of electrons moving in a magnetic field. We make no approximations in the calculations other than artificially broadening the harmonics by a small amount in order to facilitate the numerics. In contrast to previous calculations, we sum over all relevant harmonics and integrate over all particle and observer angles relative to the magnetic field. We present emission spectra for electron temperatures T = 5 x 10(8) K, 10(9) K, 2 x 10(9) K to 3.2 x 10(10) K, and provide simple fitting formulae that give a fairly accurate representation of the detailed results. For T greater than or equal to 3.2 x 10(10) K, the spectrum is represented well by the asymptotic synchrotron formula, which is obtained by assuming that the radiating electrons have Lorentz factors large compared to unity. We give an improved fitting formula for this asymptotic case as well. RP Mahadevan, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 19 TC 70 Z9 71 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1996 VL 465 IS 1 BP 327 EP 337 DI 10.1086/177422 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UR889 UT WOS:A1996UR88900027 ER PT J AU Rengarajan, TN Ho, PTP AF Rengarajan, TN Ho, PTP TI Search for optically thick H II regions and ionized stellar wind from luminous embedded infrared sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; infrared, stars; radio continuum, stars; stars, pre-main-sequence ID BIPOLAR NEBULA; MOLECULAR CLOUDS; RADIO-CONTINUUM; EMISSION; NGC-6334; STARS; POLARIMETRY; RADIATION; OUTFLOWS; OBJECTS AB High-resolution radio continuum observations of 14 protostellar candidates have been obtained using the VLA at 2 cm. The sources were chosen from a compilation of Wynn-Williams. Positive detections were made for W33A, OMC-2 IRS 4, S255 IRS 1, S255N, and NGC 6334V IRS 4, while 3 sigma upper limits of 0.15-0.5 mJy were obtained for 11 other sources. Additional 3.6 cm and 2 cm data were also obtained for W33A and OMC-2. In OMC-2 IRS 4, the radio source coincides with the northern source IRS 4N seen in the near-IR. The 3.6 cm emission of this source shows a faint extension in the same direction as the outflow inferred from infrared polarization measurements. The total spectral energy distribution of W33A at radio wavelengths is nearly flat and is consistent with a confined stellar wind model. In NGC 6334V IRS 4, a compact source slightly displaced from the central 20 mu m source and extended emission corresponding to the eastern lobe of the bipolar flow observed in the near-IR are seen. The bolometric luminosity inferred from the radio continuum emission assuming optically thin conditions is substantially less than the far-IR luminosity for most of the sources. For deeply embedded high-luminosity young stars, this suggests that either the radio continuum emission is optically thick or the stellar source is still in the pre-main-sequence stage with low ionizing radiation. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Rengarajan, TN (reprint author), TATA INST FUNDAMENTAL RES,HOMI BHABHA RD,BOMBAY 400005,MAHARASHTRA,INDIA. NR 43 TC 24 Z9 24 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1996 VL 465 IS 1 BP 363 EP 370 DI 10.1086/177425 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UR889 UT WOS:A1996UR88900030 ER PT J AU Peterson, RC Carney, BW Latham, DW AF Peterson, RC Carney, BW Latham, DW TI The rotation of RR Lyrae stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, evolution; stars, horizontal-branch; stars, Population II; stars, variables (RR Lyrae); stars, rotation; stars, variables, other ID BAADE-WESSELINK METHOD; HORIZONTAL-BRANCH STARS; GLOBULAR-CLUSTER M5; METAL ABUNDANCES; VY SERPENTIS; FIELD STARS; OXYGEN ABUNDANCES; BV PHOTOMETRY; HALO GIANTS; DISTANCES AB We report upper limits to rotation from the measurement of line breadths via cross-correlation analysis for 27 RR Lyrae variables. The eight best-observed stars of type RRab show the same variation of breadth with phase: the breadth peaks sharply during the rise to maximum light, drops gradually, and reaches a broad minimum during the phase of maximum radius. During this phase the breadth is always narrow, consistent with instrumental resolution and turbulence alone. For the three well-observed RRc variables, the breadth is this narrow at all phases except for a slight increase during the rise to maximum light. The remaining stars also conform to these patterns, albeit with sparse phase coverage and lower signal-to-noise ratio. We interpret these results as indicating that lines are broadened in RRab stars by shock-induced plumes or turbulence during the rise to maximum light, and perhaps by other causes as well, but not by rotation in RR Lyrae stars of either type. We estimate an upper limit of nu sin i < 10 km s(-1) in all cases. This is in stark contrast to the rotation seen in field blue horizontal branch stars, where nu sin i > 10 km s(-1) in three out of six well-studied field stars, and to the more rapid rotation, often exceeding 100 km s(-1), of the Population I delta Scuti variables which occupy adjacent regions of the instability strip. C1 UNIV N CAROLINA,DEPT PHYS & ASTRON,CHAPEL HILL,NC 27599. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Peterson, RC (reprint author), UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064, USA. NR 52 TC 26 Z9 26 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1996 VL 465 IS 1 BP L47 EP L50 DI 10.1086/310134 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UR891 UT WOS:A1996UR89100012 ER PT J AU Travers, MJ McCarthy, MC Gottlieb, CA Thaddeus, P AF Travers, MJ McCarthy, MC Gottlieb, CA Thaddeus, P TI Laboratory detection of the C7H radical SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, molecules; line, identification; molecular data; molecular processes; radio lines, ISM ID PARAMETERS; MOLECULES; SPECTRUM AB The linear carbon chain radical C7H has been detected in the same acetylene-argon discharge in which C8H was recently observed. Fifty rotational transitions, 23 in the ground (II1/2)-I-2 state and 27 in the (II3/2)-I-2 state (37 K higher in energy), were measured. Precise values for the rotational, fine structure, and lambda-doubling constants have been derived which allow calculation of the entire microwave and millimeter-wave spectrum to an accuracy of 0.2 km s(-1) or better. With the recent discovery of C8H in space, C7H is an excellent candidate for astronomical detection. To aid future observations, the transition frequencies for the most interesting astronomical lines are tabulated. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Travers, MJ (reprint author), HARVARD UNIV,DIV APPL SCI,29 OXFORD ST,CAMBRIDGE,MA 02138, USA. NR 21 TC 25 Z9 25 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1996 VL 465 IS 1 BP L77 EP L80 DI 10.1086/310135 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UR891 UT WOS:A1996UR89100020 ER PT J AU Wurdack, JJ AF Wurdack, JJ TI Memories of the 1950s at the New York Botanical Garden SO BRITTONIA LA English DT Article AB Memories of The New York Botanical Garden during the 1950s are given. RP Wurdack, JJ (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 SN 0007-196X J9 BRITTONIA JI Brittonia PD JUL-SEP PY 1996 VL 48 IS 3 BP 359 EP 361 DI 10.1007/BF02805301 PG 3 WC Plant Sciences SC Plant Sciences GA VN225 UT WOS:A1996VN22500010 ER PT J AU Lemaitre, R McLaughlin, PA AF Lemaitre, R McLaughlin, PA TI Revision of Pylopagurus and Tomopagurus (Crustacea: Decapoda: Paguridae), with the descriptions of new genera and species .5. Anisopagurus McLaughlin, Manucomplanus McLaughlin, and Protoniopagurus new genus SO BULLETIN OF MARINE SCIENCE LA English DT Article ID WESTERN ATLANTIC; HERMIT CRABS AB In this fifth part of a six part series, the genera Anisopagurus McLaughlin and Manucomplanus McLaughlin, together with their respective species, are diagnosed in detail and illustrated. Protoniopagurus bioperculatus n. gen., n. sp., and three new species of Anisopagurus, A. actinophorus, A. vossi and A. hopkinsi, are described. Morphological variations in some of the most common or abundant species are discussed. The assignment of Pylopagurus ungulatus (Studer, 1883) to Manucomplanus is confirmed; it has proved to be the senior synonym of Manucomplanus corallinus (Benedict, 1892). Keys to species of Anisopagurus and Manucomplanus are presented. C1 WESTERN WASHINGTON UNIV, SHANNON POINT MARINE CTR, ANACORTES, WA 98221 USA. RP Lemaitre, R (reprint author), SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT INVERTEBRATE ZOOL, MRC 163, WASHINGTON, DC 20560 USA. NR 59 TC 12 Z9 14 U1 0 U2 0 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 1996 VL 59 IS 1 BP 89 EP 141 PG 53 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA VB343 UT WOS:A1996VB34300006 ER PT J AU Kensley, B AF Kensley, B TI New species of Calocarididae from the Caribbean Sea and Gulf of Mexico (Crustacea: Decapoda: Thalassinidea) SO BULLETIN OF MARINE SCIENCE LA English DT Article ID AXIIDAE; GENUS AB Three new species of deepwater calocaridid shrimps are recorded from the Gulf of Mexico: Calastacus colpos, Calastacus mexicanus, and Calocaris caribbaeus. The latter species is also recorded from several sites in the Caribbean Sea. Calastacus colpos is characterised by flattened contiguous eyes, a single spine on the dorsal margin of the merus of pereopod 1, and 3-4 spines on the uropodal suture. Calastacus mexicanus is characterised by rounded non-contiguous eyes, strongly spinose merus and carpus of pereopod 1, and 8-9 spines on the uropodal suture. Calocaris caribbaeus is similar to the north-east Atlantic C. templemani Squires, but differs in having weaker spination of the uropod and telson. RP Kensley, B (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 14 TC 10 Z9 13 U1 0 U2 0 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 1996 VL 59 IS 1 BP 158 EP 168 PG 11 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA VB343 UT WOS:A1996VB34300009 ER PT J AU Wright, TL Helz, RT AF Wright, TL Helz, RT TI Differentiation and magma mixing on Kilauea's east rift zone: A further look at the eruptions of 1955 and 1960 .2. The 1960 lavas SO BULLETIN OF VOLCANOLOGY LA English DT Article DE Kilauea; magma mixing; magmatic temperatures; glass composition; basalt composition; magmatic plumbing/storage/transport ID PUU-OO ERUPTION; SUBMARINE LAVAS; VOLCANO; HAWAII; ORIGIN; PHENOCRYSTS; CONSTRAINTS; PETROLOGY; RIDGE AB New and detailed petrographic observations, mineral compositional data, and whole-rock vs glass compositional trends document magma mixing in lavas erupted from Kilauea's lower east rift zone in 1960. Evidence includes the occurrence of heterogeneous phenocryst assemblages, including resorbed and reversely zoned minerals in the lavas inferred to be hybrids. Calculations suggest that this mixing, which is shown to have taken place within magma reservoirs recharged at the end of the 1955 eruption, involved introduction of four different magmas. These magmas originated beneath Kilauea's summit and moved into the rift reservoirs beginning 10 days after the eruption began. We used microprobe analyses of glass to calculate temperatures of liquids erupted in 1955 and 1960. We then used the calculated proportions of stored and recharge components to estimate the temperature of the recharge components, and found those temperatures to be consistent with the temperature of the same magmas as they appeared at Kilauea's summit. Our studies reinforce conclusions reached in previous studies of Kilauea's magmatic plumbing. We infer that magma enters shallow storage beneath Kilauea's summit and also moves laterally into the fluid core of the East rift zone. During this process, if magmas of distinctive chemistry are present, they retain their chemical identity and the amount of cooling is comparable for magma transported either upward or laterally to eruption sites. Intrusions within a few kilometers of the surface cool and crystallize to produce fractionated magma. Magma mixing occurs both within bodies of previously fractionated magma and when new magma intersects a preexisting reservoir. Magma is otherwise prevented from mixing, either by wall-rock septa or by differing thermal and density characteristics of the successive magma batches. C1 US GEOL SURVEY,RESTON,VA 22092. RP Wright, TL (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,NHB-119,WASHINGTON,DC 20560, USA. RI Asavin, Alex/F-5800-2012 OI Asavin, Alex/0000-0002-0202-2970 NR 40 TC 21 Z9 21 U1 0 U2 5 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0258-8900 J9 B VOLCANOL JI Bull. Volcanol. PD JUL PY 1996 VL 57 IS 8 BP 602 EP 630 DI 10.1007/s004450050115 PG 29 WC Geosciences, Multidisciplinary SC Geology GA VA404 UT WOS:A1996VA40400002 ER PT J AU Sanchez, G Perry, HM Trigg, CB Vecchione, M Roper, C Biesiot, PM AF Sanchez, G Perry, HM Trigg, CB Vecchione, M Roper, C Biesiot, PM TI Morphometry of juvenile and subadult Loligo pealei and L-plei from the northern Gulf of Mexico SO FISHERY BULLETIN LA English DT Article ID SQUID AB Two species of Loligo are abundant in northern Gulf waters: the long-finned squid, Loligo pealei, and the arrow squid, Loligo plei. Variability within species and similarities between the species often hamper accurate identification. The two species more closely resemble each other in areas of sympatry, and there is overlap in almost all of the diagnostic characters. Small specimens of Loligo are not easily identified, and there are few studies detailing their morphometry. Because of the taxonomic uncertainties associated with the identification of juveniles and subadults of L. pealei and L. plei, the species were differentiated by isoelectric focusing, and morphometric characters and indices of potential use in species separation were evaluated. Emphasis was placed on those taxonomic characters suitable for use in the field. Best discrimination between the two species was achieved with combinations of measurements of characters and calculated indices associated with cartilaginous structures (funnel cartilage length, gladius width [GW], nuchal cartilage length, and rachis width [RW]) and the shape of the gladius. An arbitrary cutoff in GW/RW ratio of 2.7 (ratio of the greatest width of the gladius to the width of the free rachis at the junction of the vane) correctly classified 100% of the L. plei and 91% of the L. pealei. The overall shape of the gladius (broader and more rounded in L. pealei), presence or absence of marginal ribs in the vane of the gladius, and the nature of the junction of the vane and free rachis (junction gradual and not distinct in L. pealei) were also useful in distinguishing the two species. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,NOAA,NMFS SYSTEMAT LAB,WASHINGTON,DC 20560. SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. UNIV SO MISSISSIPPI,DEPT BIOL SCI,HATTIESBURG,MS 39406. RP Sanchez, G (reprint author), GULF COAST RES LAB,POB 7000,OCEAN SPRINGS,MS 39566, USA. NR 12 TC 6 Z9 6 U1 1 U2 3 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD JUL PY 1996 VL 94 IS 3 BP 535 EP 550 PG 16 WC Fisheries SC Fisheries GA UU710 UT WOS:A1996UU71000012 ER PT J AU Johnson, DG Orphal, J Toon, GC Chance, KV Traub, WA Jucks, KW Guelachvili, G MorillonChapey, M AF Johnson, DG Orphal, J Toon, GC Chance, KV Traub, WA Jucks, KW Guelachvili, G MorillonChapey, M TI Measurement of chlorine nitrate in the stratosphere using the nu(4) and nu(5) bands SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ABSORPTION; CLONO2; SPECTRA; HNO3; O3 AB We present laboratory measurements of the absorption cross sections of the vg band (540-580 cm(-1)) of chlorine nitrate made under stratospheric conditions of temperature and pressure. We use the measured cross sections and observed mid-infrared stratospheric emission spectra to retrieve mid-latitude vertical mixing ratio profiles for both day and night in the altitude range 20-34 km, and compare the results with a sunset profile obtained simultaneously from solar absorption measurements of the v(4) Q branch at 780 cm(-1). The profiles obtained using these two methods are shown to be in excellent agreement, validating retrievals using the v(4) band. We also find good agreement in this altitude range between the observed day/night ratio and the results of a 1-D photochemical model. C1 UNIV BREMEN,INST ENVIRONM PHYS,D-28334 BREMEN,GERMANY. CALTECH,JET PROP LAB,PASADENA,CA 91109. UNIV PARIS 06,CNRS UPR 136,LAB PHYS MOL & APPLICAT,CTR ORSAY,F-91405 ORSAY,FRANCE. UNIV PARIS 11,CNRS UPR 136,LAB PHYS MOL & APPLICAT,CTR ORSAY,F-91405 ORSAY,FRANCE. RP Johnson, DG (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Orphal, Johannes/A-8667-2012; Johnson, David/F-2376-2015 OI Orphal, Johannes/0000-0002-1943-4496; Johnson, David/0000-0003-4399-5653 NR 17 TC 20 Z9 20 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 1 PY 1996 VL 23 IS 14 BP 1745 EP 1748 DI 10.1029/96GL01675 PG 4 WC Geosciences, Multidisciplinary SC Geology GA UV847 UT WOS:A1996UV84700011 ER PT J AU Pukazhenthi, BS Wildt, DE Ottinger, MA Howard, J AF Pukazhenthi, BS Wildt, DE Ottinger, MA Howard, J TI Compromised sperm protein phosphorylation after capacitation, swim-up, and zona pellucida exposure in teratospermic domestic cats SO JOURNAL OF ANDROLOGY LA English DT Article DE cat; sperm; teratospermia; tyrosine phosphorylation; zona pellucida; hexokinase ID PHOSPHOTYROSINE-CONTAINING PROTEIN; ACROSOME REACTION; MOUSE SPERM; TYROSINE KINASE; EXTRACELLULAR-MATRIX; HUMAN SPERMATOZOA; BINDING; IDENTIFICATION; EXOCYTOSIS; ACTIVATION AB Tyrosine phosphorylated proteins recently have been found in mouse and human spermatozoa. Our objectives were to (1) determine if domestic cat spermatozoa also express tyrosine phosphorylated proteins, and (2) examine the changes in protein phosphorylation between normospermic and teratospermic domestic cats following sperm capacitation, swim-up separation and exposure to zona pellucida (ZP). Membranes from cat spermatozoa contained two phosphorylated proteins of molecular weights 160 kDa and 95 kDa (designated as p160 and p95) that immunoreacted with monoclonal antibodies to tyrosine phosphate. The p95 protein was distinct from sperm-specific hexokinase. Following capacitation, the extent of phosphorylation of p95 was increased (P <0.05) 3-fold in normospermic cats compared to only 1.75-fold in teratospermic cats. Similarly, phosphorylation of p160 also increased (P <0.05) 2.4-fold in normospermic compared to 1.84-fold in teratospermic cats. Although swim-up separation increased the percentage of normal spermatozoa in teratospermic ejaculates, phosphorylation of p95 in swim-up aliquots was increased (P <0.05) only 1.95-fold in teratospermic cats compared to 2.9-fold in normospermic counterparts. Likewise, phosphorylation of p160 was lower (P <0.05) in teratospermic (1.5-fold) compared to normospermic cats (2.0-fold) cats. Phosphorylation also was influenced by exposure to cat ZP proteins (P <0.05). Solubilized cat ZP bound to the sperm proteins of apparent molecular mass 120, 95, 50, 42, 30, 27, 23 and 20 kDa, suggesting a direct binding interaction between p95 and the ZP. Overall, these findings (1) indicate the presence of tyrosine phosphorylated proteins in the domestic cat spermatozoon that directly interact with homologous ZP glycoproteins; (2) demonstrate that cat sperm hexokinase is not phosphorylated on tyrosine residues; and (3) suggest that the diminished phosphorylation efficiency of sperm from teratospermic cats may result in a compromise in capacitation and the acrosome reaction. C1 SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA. UNIV MARYLAND,DEPT ANIM SCI,COLLEGE PK,MD 20742. UNIV MARYLAND,DEPT POULTRY SCI,COLLEGE PK,MD 20742. FU NCRR NIH HHS [RR 00045]; NICHD NIH HHS [HD 23853] NR 33 TC 31 Z9 32 U1 0 U2 2 PU AMER SOC ANDROLOGY, INC PI LAWRENCE PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 SN 0196-3635 J9 J ANDROL JI J. Androl. PD JUL-AUG PY 1996 VL 17 IS 4 BP 409 EP 419 PG 11 WC Andrology SC Endocrinology & Metabolism GA VK243 UT WOS:A1996VK24300015 PM 8889704 ER PT J AU Gacia, E Ballesteros, E AF Gacia, E Ballesteros, E TI The effect of increased water level on Isoetes lacustris L in Lake Baciver, Spain SO JOURNAL OF AQUATIC PLANT MANAGEMENT LA English DT Article DE pyrenees; oxygen; light; leaf primary production; water level fluctuations; anoxia ID PYRENEAN LAKE; MACROPHYTES AB Ten months after flooding lake Baciver, water levels were 5.5 m higher than the previous normal and the area formally occupied by the Isoetes population was reduced. All Isoetes originally present below 0.6 m died, and only plants standing between 5.8 and 6.1 m (new depth) survived. As irradiance decreased, remaining individuals produced fewer leaves, but their biomass production was higher, as leaf length increased in response to the diminished available irradiance. Because leaf mortality was excessive, regeneration capacity, population performance and dynamics were adversely affected. In 1992, no new production occurred in Isoetes lacustris individuals surviving after the winter. We suggest that low surface oxygen levels at the water column under the ice, and total anoxia below 6 m depth, caused the demise of the I. lacustris population in Lake Baciver. C1 CSIC,BLANESBLA 17300,GIRONA,SPAIN. UNIV BARCELONA,INST HIGH MT RES,VIELHA 25530,LLEIDA,SPAIN. RP Gacia, E (reprint author), SMITHSONIAN MARINE STN LINK PORT,5612 OLD DIXIE HIGHWAY,FT PIERCE,FL 34946, USA. RI Gacia, Esperanca/J-9238-2012; Ballesteros, Enric/K-6497-2012 OI Gacia, Esperanca/0000-0002-7687-7437; NR 12 TC 9 Z9 10 U1 0 U2 2 PU AQUATIC PLANT MANAGEMENT SOC, INC PI CLERMONT PA PO BOX 121086, CLERMONT, FL 34712-1086 SN 0146-6623 J9 J AQUAT PLANT MANAGE JI J. Aquat. Plant Manage. PD JUL PY 1996 VL 34 BP 57 EP 59 PG 3 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA VL343 UT WOS:A1996VL34300005 ER PT J AU West, SA Herre, EA Windsor, DM Green, PRS AF West, SA Herre, EA Windsor, DM Green, PRS TI The ecology and evolution of the New World non-pollinating fig wasp communities SO JOURNAL OF BIOGEOGRAPHY LA English DT Article; Proceedings Paper CT 5th International Symposium on Fig Biology CY MAY, 1994 CL BERGEN, NORWAY DE Ficus; parasitoid; parasites; coevolution; density dependence; spatial heterogeneity; community structure ID HOST-PARASITOID ASSOCIATIONS; PATCHY ENVIRONMENTS; DENSITY DEPENDENCE; SPECIES RICHNESS; FRUIT PRODUCTION; FICUS FRUIT; SEX-RATIOS; HETEROGENEITY; MUTUALISM; DYNAMICS AB We present data on several previously undescribed species from six genera of New World nonpollinating fig wasps. We show that many of these species have a negative effect on the reproductive success of both the pollinator wasps and the host figs. Our results suggest that the two most abundant genera of non-pollinating wasps, the Idarnes and the Critogaster, compete for the same pool of female flowers as the pollinating wasps in the Urostigma and Pharmacosycea figs, respectively. Wasps from the genus Aepocerus induce and develop within large galls, in the Urostigma figs. By draining resources from the fruit these wasps may have a detrimental effect on the production of pollinator wasps and viable seeds. Some of the species investigated are parasitoids of other non-pollinating species. We examine the importance of the various forms of spatial heterogeneity in the parasitism rate that can act to stabilise the host-parasitoid interaction. Finally, we discuss the factors underlying the large variation in the abundance and diversity of the non-pollinating wasps both among and within fruit crops. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP West, SA (reprint author), UNIV LONDON IMPERIAL COLL SCI TECHNOL & MED,DEPT BIOL,SILWOOD PK,ASCOT SL5 7PY,BERKS,ENGLAND. RI West, Stuart/M-3608-2014 OI West, Stuart/0000-0003-2152-3153 NR 71 TC 110 Z9 131 U1 3 U2 33 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD JUL PY 1996 VL 23 IS 4 BP 447 EP 458 DI 10.1111/j.1365-2699.1996.tb00006.x PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA VZ750 UT WOS:A1996VZ75000006 ER PT J AU Nason, JD Herre, EA Hamrick, JL AF Nason, JD Herre, EA Hamrick, JL TI Paternity analysis of the breeding structure of strangler fig populations: Evidence for substantial long-distance wasp dispersal SO JOURNAL OF BIOGEOGRAPHY LA English DT Article; Proceedings Paper CT 5th International Symposium on Fig Biology CY MAY, 1994 CL BERGEN, NORWAY DE Ficus; gene flow; paternity analysis; pollen dispersal; tropical forest ID GENE FLOW; MATING SYSTEM; NATURAL-POPULATION; NEOTROPICAL TREE; POLLEN DISPERSAL; TROPICAL PLANTS; WILD RADISH; RAIN-FOREST; FICUS; CONSEQUENCES AB The mutualistic interaction of figs with their species-specific wasp pollinators and the role of figs as 'keystone' plant resources in tropical communities has received substantial attention from both plant and animal ecologists. Despite this focus on the reproductive biology of figs, the minute size of the wasps has effectively precluded our ability to monitor patterns of wasp dispersal and fig mating relationships in natural forest habitats. In this paper we use genetic markers and genealogy reconstruction techniques to examine the breeding structure of populations of four strangler fig species occurring in central Panama. The natural history of figs facilitates the genetic analysis of full-sib progeny arrays from which the genotypes of successful pollen donors can be reconstructed precisely. Paternity reconstruction in the four study species reveals that individual flowering trees may routinely receive pollen from numerous donors despite characteristically low densities of co-flowering individuals. These data indicate not only that breeding populations of these figs are larger than the minimum critical sizes predicted to be necessary to support populations of their species-specific pollinators, but are more extensive in size and area than has been described for any plant species yet examined. Further, the fig wasps are shown to be efficient agents of long-distance dispersal, routinely moving up to 10 km between flowering trees. In accord with the potential for substantial long-distance gene flow and large effective population sizes, ten of eleven species of Panamanian figs assayed were found to maintain exceptionally high levels of genetic variation within their populations. Combined with other reports of occasional long-distance dispersal, the results of this study suggest that fig wasps may be more effective at colonizing isolated fig populations than previously thought. C1 SMITHSONIAN TROP RES INST,BALBOA,ANCON,PANAMA. RP Nason, JD (reprint author), UNIV GEORGIA,DEPT BOT,ATHENS,GA 30602, USA. NR 84 TC 89 Z9 94 U1 1 U2 16 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD JUL PY 1996 VL 23 IS 4 BP 501 EP 512 DI 10.1111/j.1365-2699.1996.tb00012.x PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA VZ750 UT WOS:A1996VZ75000012 ER PT J AU Herre, EA Machado, CA Bermingham, E Nason, JD Windsor, DM McCafferty, SS VanHouten, W Bachmann, K AF Herre, EA Machado, CA Bermingham, E Nason, JD Windsor, DM McCafferty, SS VanHouten, W Bachmann, K TI Molecular phylogenies of figs and their pollinator wasps SO JOURNAL OF BIOGEOGRAPHY LA English DT Article; Proceedings Paper CT 5th International Symposium on Fig Biology CY MAY, 1994 CL BERGEN, NORWAY DE Moraceae; Ficus; chloroplast DNA; coevolution; mitochondrial DNA; mutualism ID MITOCHONDRIAL-DNA EVOLUTION; HYMENOPTERA CHALCIDOIDEA; POPULATION BIOLOGY; CHLOROPLAST DNA; FICUS MORACEAE; AMPLIFICATION; SYSTEMATICS; HOST; SPECIFICITY; GENETICS AB We collected and analysed nucleotide sequence and protein electrophoretic data in order to estimate phylogenies of figs and fig-pollinating wasps at several taxonomic scales. The relatively conserved chloroplast gene coding rbCl allowed the estimation of the taxonomic position of Ficus relative to other genera within the Moraceae. Further, in conjunction with chloroplast tRNA spacer genes, rbcL sequences allowed the partial resolution of the phylogenetic associations of fig species from different parts of the world with representatives from all the recognized subgenera of Fiats. The phylogeny of the corresponding wasp species that pollinate most of those taxa was estimated using mitochondrial COI-COII and 12S ribosomal genes. At a fine scale, the phylogenies of species within two subgenera of figs growing in Panama (Urostigma, and Pharmacosycea) were estimated by using protein electrophoretic data. The phylogeny of the corresponding pollinator wasp species was estimated using COII sequence data. Although we need to extend the taxa sampled and augment the molecular database, the host and pollinator phylogenies show a high degree of congruence and the results support the predominance of strict-sense coevolution between figs and their pollinator wasps at both global and fine scales. C1 STRI,UNIT 0948,APO,AA 34002. UNIV CALIF IRVINE,DEPT ECOL & EVOLUTIONARY BIOL,IRVINE,CA 92717. UNIV GEORGIA,DEPT BOT,ATHENS,GA 30602. PURDUE UNIV,DEPT AGRON,W LAFAYETTE,IN 47906. UNIV AMSTERDAM,HUGO DE VRIES LAB,NL-1098 SM AMSTERDAM,NETHERLANDS. RP Herre, EA (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. RI Machado, Carlos/B-8855-2009 OI Machado, Carlos/0000-0003-1546-7415 NR 65 TC 104 Z9 121 U1 5 U2 30 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD JUL PY 1996 VL 23 IS 4 BP 521 EP 530 DI 10.1111/j.1365-2699.1996.tb00014.x PG 10 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA VZ750 UT WOS:A1996VZ75000014 ER PT J AU Kalko, EKV Herre, EA Handley, CO AF Kalko, EKV Herre, EA Handley, CO TI Relation of fig fruit characteristics to fruit-eating bats in the New and Old World tropics SO JOURNAL OF BIOGEOGRAPHY LA English DT Article; Proceedings Paper CT 5th International Symposium on Fig Biology CY MAY, 1994 CL BERGEN, NORWAY DE bats; birds; Ficus fruit characteristics; echolocation; foraging ID BARRO-COLORADO-ISLAND; CAROLLIA-PERSPICILLATA; ARTIBEUS-JAMAICENSIS; TEMPORAL VARIATION; FRUGIVOROUS BATS; SEED DISPERSAL; RAIN-FOREST; CHIROPTERA; PLANTS; BIRDS AB Long-term studies of a Panamanian fig community have revealed that the figs separate into two major groups based on distinct patterns in fruit characteristics including fruit size, colour, scent and synchrony of ripening. Furthermore, these differences can be linked to sensory, morphological and behavioural capabilities of the figs' primary dispersers. One group of figs attracts primarily bats; the other group is visited mainly by birds. Whereas fruits of 'bat' figs span a wide range of size classes, ripen synchronously and remain green(ish) when ripe, all fruits of 'bird' figs have small fruit which ripen asynchronously and turn red when ripe. Among 'bat' figs, fruit size is correlated with body size of the bats that prefer them. Based on the consistent differences between 'bat' and 'bird' fig fruits in Panama we expect similar patterns in Old World figs. Furthermore, since fig-eating bats of the Old World differ in morphology, behaviour and sensory capabilities from fig-eating bats of the New World we speculate that these differences should be reflected in differences in fruit characteristics of Old and New World 'bat' figs. Personal observations and literature reports of Old World bats and figs are consistent with our predictions. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. NATL MUSEUM NAT HIST, DIV MAMMALS, MRC, NHB 108, WASHINGTON, DC 20560 USA. RP Kalko, EKV (reprint author), UNIV TUBINGEN, MORGENSTELLE 28, D-72076 TUBINGEN, GERMANY. NR 110 TC 133 Z9 142 U1 4 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD JUL PY 1996 VL 23 IS 4 BP 565 EP 576 DI 10.1111/j.1365-2699.1996.tb00018.x PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA VZ750 UT WOS:A1996VZ75000018 ER PT J AU Herre, EA AF Herre, EA TI An overview of studies on a community of Panamanian figs SO JOURNAL OF BIOGEOGRAPHY LA English DT Article; Proceedings Paper CT 5th International Symposium on Fig Biology CY MAY, 1994 CL BERGEN, NORWAY DE monoecious fig species; pollinators; phylogenetic reconstructions; Panama; mutualism ID FICUS-CARICA L; POLLINATOR MUTUALISM; SPECIES RICHNESS; FRUIT PRODUCTION; SEX-RATIOS; COMMON FIG; NEW-WORLD; WASPS; EVOLUTION; CONSEQUENCES AB Findings from long-term studies of eighteen monoecious fig species and their associated pollinators, parasites, and seed dispersers from a lowland tropical forest community in Panama are summarized. Studies of evolutionary genetics confirm the suggestion from earlier morphological studies that pollinator and non-pollinator wasps, as well as parasitic nematodes, are generally species-specific. Further, phylogenetic reconstructions suggest that these systems are predominated by strict-sense co-evolution among several trophic levels of fig-associated organisms. Studies of population genetics show that fig wasps routinely disperse pollen over surprisingly great distances. Moreover, both the number of individual fig trees constituting a breeding population and the area that they occupy (>100 km(2)) are among the largest for any plant species known. Studies of factors influencing reproductive success of both the figs and their pollinators indicate that, for any given species, many factors (e.g. number and size of pollinators, resource availability, parasite loads) interact in complex but systematic ways to affect the production of seeds and pollinator wasps. Across species, there are repeated patterns of associations among characters such as average number of pollinators per fruit, pollinator sex ratios, nematode virulence, fruit size, fruit colour, physiological properties of the fruit, taxa of associated seed dispersers and degree of synchrony of fruit ripening that imply causal, adaptive linkages and trade-offs among these characters. Collectively, these studies suggest the critical role for comparative work of many species, preferably at many sites, in the understanding of this complex mutualism. RP Herre, EA (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO,AA 34002, USA. NR 71 TC 72 Z9 80 U1 4 U2 16 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0NE SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD JUL PY 1996 VL 23 IS 4 BP 593 EP 607 DI 10.1111/j.1365-2699.1996.tb00020.x PG 15 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA VZ750 UT WOS:A1996VZ75000020 ER PT J AU Waterhouse, JS Ke, J Pickett, JA Weldon, PJ AF Waterhouse, JS Ke, J Pickett, JA Weldon, PJ TI Volatile components in dorsal gland secretions of the collared peccary, Tayassu tajacu (Tayassuidae, mammalia) SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE dorsal gland; collared peccary; Tayassu tajacu; gerariylgeraniol; springene; squalene; straight-chain esters; branched-chain esters ID HYMENOPTERA AB Secretions of the dorsal gland of free-ranging adult male and female collared peccaries (Tayassu tajacu) were analyzed by gas chromatography-mass spectrometry. Both sexes contain (2E,6E, 10E)-geranylgeraniol; squalene (all E isomer); and the following isomers of springene, a diterpene homolog of beta-farnesene: (3E,6E, 10E)-alpha-springene, (3Z,6E, 10E)-alpha-springene, and (6E, 10E)-beta-springene. A diterpene alcohol and an additional isomer each of squalene and springene also were observed. Straight- and branched-chain esters abound in the secretions of females, but they were not detected in males. C1 IACR ROTHAMSTED,HARPENDEN AL5 2JQ,HERTS,ENGLAND. SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. RP Waterhouse, JS (reprint author), ANGLIA POLYTECH UNIV,ENVIRONM SCI RES CTR,EAST RD,CAMBRIDGE CB1 1PT,ENGLAND. NR 19 TC 17 Z9 17 U1 2 U2 5 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD JUL PY 1996 VL 22 IS 7 BP 1307 EP 1314 DI 10.1007/BF02266967 PG 8 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA VD011 UT WOS:A1996VD01100007 PM 24226086 ER PT J AU Petervary, N Gillette, DM Lewbart, GA Harshbarger, JC AF Petervary, N Gillette, DM Lewbart, GA Harshbarger, JC TI A spontaneous neoplasm of the renal collecting ducts in an oscar, Astronotus ocellatus (Cuvier), with comments on similar cases in this species SO JOURNAL OF FISH DISEASES LA English DT Article C1 N CAROLINA STATE UNIV,COLL VET MED,DEPT COMPAN ANIM & SPECIAL SPECIES MED,RALEIGH,NC 27606. ROHM & HAAS RES LABS,NORRISTOWN,PA. SMITHSONIAN INST,NATL MUSEUM NAT HIST,WASHINGTON,DC. NR 2 TC 6 Z9 6 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0140-7775 J9 J FISH DIS JI J. Fish Dis. PD JUL PY 1996 VL 19 IS 4 BP 279 EP 281 DI 10.1111/j.1365-2761.1996.tb00704.x PG 3 WC Fisheries; Marine & Freshwater Biology; Veterinary Sciences SC Fisheries; Marine & Freshwater Biology; Veterinary Sciences GA VA350 UT WOS:A1996VA35000003 ER PT J AU Miller, AAL Nomura, R Osterman, LE AF Miller, AAL Nomura, R Osterman, LE TI Islandiella algida (Cushman, 1944); Senior subjective synonym of Islandiella islandica (Norvang) SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID STRATIGRAPHY AB The modern species Cassidulina algida (Cushman), type locality Casco Bay, Maine has rarely been reported in the literature. Islandiella islandica (Norvang), type locality off the north coast of Iceland, has been widely reported as a constituent of Pliocene to Recent arctic, subarctic and boreal benthic foraminiferal faunas. Various studies by the authors of modern and fossil cassidulinid foraminifera along the eastern Canadian continental margin and Cenozoic marine deposits on and around the islands of Japan led to the examination of the holotype and paratypes of C. algida and topotypic material of I. islandica (identified by Norvang) deposited in the Cushman Collection at the National Museum of Natural History (Smithsonian Institution). The holotype and paratypes of Cassidulina algida Cushman show Islandiella algida (Cushman) to be conspecific with Islandiella islandica (Norvang), the type species of the genus Islandiella (Norvang). Thus, Islandiella algida is the senior subjective synonym of I. islandica (Norvang). C1 SHIMANE UNIV,DEPT MICROPALEONTOL,FAC EDUC,MATSUE,SHIMANE 690,JAPAN. SMITHSONIAN INST,DEPT PALEOBIOL,NHB121,WASHINGTON,DC 20560. GEORGE WASHINGTON UNIV,DEPT GEOL,WASHINGTON,DC 20052. RP Miller, AAL (reprint author), MARINE GEOS,3824 NOVALEA DR,HALIFAX,NS B3K 5K5,CANADA. NR 46 TC 3 Z9 3 U1 0 U2 1 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD JUL PY 1996 VL 26 IS 3 BP 209 EP 212 PG 4 WC Paleontology SC Paleontology GA UY961 UT WOS:A1996UY96100003 ER PT J AU Jett, JA AF Jett, JA TI Recent literature on foraminifera SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Bibliography RP Jett, JA (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,NMNH MRC 121,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD JUL PY 1996 VL 26 IS 3 BP 268 EP 272 PG 5 WC Paleontology SC Paleontology GA UY961 UT WOS:A1996UY96100008 ER PT J AU Wcislo, WT AF Wcislo, WT TI Parasitism rates in relation to nest site in bees and wasps (Hymenoptera: Apoidea) SO JOURNAL OF INSECT BEHAVIOR LA English DT Article DE Apoidea; bee; sphecid wasp; parasitism; search behavior; habitat ID CRABRO HYMENOPTERA; FRIESE HYMENOPTERA; SOLITARY BEE; COSTA-RICA; SEX-RATIO; SPHECIDAE; DIPTERA; MEGACHILIDAE; EVOLUTION; BEHAVIOR AB To account for differences in occurrence of social behavior in different lineages of bees, Michener (1985) hypothesized that ground nests are move easily located by parasites than are twig nests, In the former case parasites search in two dimensions, while in the fatter they search in three-dimensional space, One prediction derived from this hypothesis is that ground nests will have higher rates of parasitism than twig nests. A survey of published reports on rates of cell parasitism for 92 species of nesting bees and wasps (Apoidea) shows no significant differences in mean parasitism razes between these two classes of nests. The analyses were repeated at the generic level (N = 44), yielding the same pattern. These data may be biased due to phylogenetic effects. Paired comparisons (n = 11 pairs) of related taxa that differ in nest site show that ground-nesting taxa more often have higher rates of parasitism than twig-nesters. The use of artificial ''trap-nests'' to study twig-nesters significantly enhances the success rare of parasites. This bias, as well as several other limitations, suggests that experimental studies of the host-searching capabilities of parasites and predators may be more efficacious than such comparative tests. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. NR 78 TC 18 Z9 21 U1 3 U2 20 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0892-7553 J9 J INSECT BEHAV JI J. Insect Behav. PD JUL PY 1996 VL 9 IS 4 BP 643 EP 656 DI 10.1007/BF02213885 PG 14 WC Entomology SC Entomology GA VG495 UT WOS:A1996VG49500009 ER PT J AU Cheung, ASC Yoshino, K Esmond, JR Parkinson, WH AF Cheung, ASC Yoshino, K Esmond, JR Parkinson, WH TI The Schumann-Runge absorption bands of O-2 at 670 K and the spectroscopic constants of the ground state, X(3)Sigma(g)(-) SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID VIBRATIONALLY EXCITED O-2; HIGH-RESOLUTION; HERZBERG CONTINUUM; REGION; OXYGEN AB High-resolution absorption spectra of O-2 have been photographed at 670 K throughout the wavelength region 179 to 212 nm. Precise wavelength measurements and rotational analyses of the Schumann-Runge (upsilon', upsilon '') bands with upsilon' = 12-17 and upsilon '' = 1-4 have been completed. The term values for the B-3 Sigma(u)(-) and the X(3) Sigma(g)(-) states are presented. Spectroscopic constants of the X(3) Sigma(g)(-) State of O-2 for upsilon '' = 1-4 have been determined. Good agreement has been obtained between the determined molecular constants and those reported earlier. (C) 1996 Academic Press, Inc. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Cheung, ASC (reprint author), UNIV HONG KONG,DEPT CHEM,POKFULAM RD,HONG KONG,HONG KONG. RI Cheung, Allan/D-3059-2009 NR 21 TC 20 Z9 20 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD JUL PY 1996 VL 178 IS 1 BP 66 EP 77 DI 10.1006/jmsp.1996.0158 PG 12 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA UX808 UT WOS:A1996UX80800010 ER PT J AU Lucas, SG Emry, RJ AF Lucas, SG Emry, RJ TI Biochronological significance of Amynodontidae (Mammalia, Perissodactyla) from the Paleogene of Kazakhstan SO JOURNAL OF PALEONTOLOGY LA English DT Article AB Five taxa of amynodontid rhinoceroses have been named from Kazakhstan. We consider only two of these valid, and recognize three amynodontid taxa from Paleogene deposits in Kazakhstan: Cadurcodon ardynensis (=Cadurcodon zaisanensis; =Amynodon tuskabakensis) from the upper Eocene (Ergilian)-lower Oligocene (Shandgolian) of the Zaysan basin, Zaisanamynodon borisovi, from the Ergilian of the Zaysan basin and Cadurcodon kazakademius, from Shandgolian strata in the vicinity of the Chelkar-Teniz lake basin. Gigantamynodon akespensis, from the upper Oligocene north of the Aral Sea is a rhinocerotid, not an amynodontid. Close similarity of the amynodontids of Kazakhstan to those of Mongolia and China supports direct correlation of Ergilian and Shandgolian strata across Asia. C1 SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT PALEOBIOL, WASHINGTON, DC 20560 USA. RP Lucas, SG (reprint author), NEW MEXICO MUSEUM NAT HIST & SCI, 1801 MT RD NW, ALBUQUERQUE, NM 87104 USA. NR 30 TC 6 Z9 9 U1 0 U2 1 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 1996 VL 70 IS 4 BP 691 EP 696 PG 6 WC Paleontology SC Paleontology GA VA765 UT WOS:A1996VA76500013 ER PT J AU Huang, K Tommasini, P AF Huang, K Tommasini, P TI Methods for a nonuniform Bose gas SO JOURNAL OF RESEARCH OF THE NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY LA English DT Article DE Bogoliubov transformation; Bose-Einstein condensation; Bose gas; Gaussian wave function; hard-sphere interaction; negative scattering length; pseudopotential; self-consistent field; variational method ID EINSTEIN CONDENSATION; ATOMS AB We review mathematical methods for the treatment of a system of Bose particles with nonuniform density. The use of the pseudopotential is explained, especially with respect to negative scattering lengths. It is emphasized that the delta-function potential produces no scattering in three dimensions, and should not be used in the Bogoliubov self-consistent field method, which is variational in nature. A common misuse of the Bogoliubov method at finite temperatures is pointed out. A Gaussian variational method is proposed. C1 MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOL PHYS, CAMBRIDGE, MA 02138 USA. RP Huang, K (reprint author), MIT, CTR THEORET PHYS, NUCL SCI LAB, CAMBRIDGE, MA 02139 USA. NR 29 TC 17 Z9 17 U1 0 U2 1 PU US GOVERNMENT PRINTING OFFICE PI WASHINGTON PA SUPERINTENDENT DOCUMENTS,, WASHINGTON, DC 20402-9325 USA SN 1044-677X J9 J RES NATL INST STAN JI J. Res. Natl. Inst. Stand. Technol. PD JUL-AUG PY 1996 VL 101 IS 4 BP 435 EP 442 DI 10.6028/jres.101.046 PG 8 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA VX636 UT WOS:A1996VX63600003 PM 27805099 ER PT J AU You, L Lewenstein, M AF You, L Lewenstein, M TI Near-Resonant imaging of trapped cold atomic samples SO JOURNAL OF RESEARCH OF THE NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY LA English DT Article DE Bose-Einstein condensation; light scattering; optical imaging; quantum statistics ID BOSE-EINSTEIN CONDENSATION; NONLINEAR SCHRODINGER-EQUATION; NEUTRAL ATOMS; SCATTERING LENGTH; SODIUM ATOMS; GAS AB We study the formation of diffraction patterns in the near-resonant imaging of trapped cold atomic samples. We show that the spatial imaging can provide detailed information on the trapped atomic clouds. C1 CENS, CEA, SERV PHOTONS ATOMES & MOL, F-91191 GIF SUR YVETTE, FRANCE. RP You, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOL PHYS, 60 GARDEN ST, MS 14, CAMBRIDGE, MA 02138 USA. RI Lewenstein, Maciej/I-1337-2014 OI Lewenstein, Maciej/0000-0002-0210-7800 NR 32 TC 5 Z9 5 U1 0 U2 0 PU US GOVERNMENT PRINTING OFFICE PI WASHINGTON PA SUPERINTENDENT DOCUMENTS,, WASHINGTON, DC 20402-9325 USA SN 1044-677X J9 J RES NATL INST STAN JI J. Res. Natl. Inst. Stand. Technol. PD JUL-AUG PY 1996 VL 101 IS 4 BP 575 EP 582 DI 10.6028/jres.101.057 PG 8 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA VX636 UT WOS:A1996VX63600014 PM 27805110 ER PT J AU Riley, SM AF Riley, SM TI Crows over a wheatfield - Sharp,P SO LIBRARY JOURNAL LA English DT Book Review RP Riley, SM (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD JUL PY 1996 VL 121 IS 12 BP 163 EP 163 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA UX600 UT WOS:A1996UX60000342 ER PT J AU Kelley, SL Schottlaender, BEC AF Kelley, SL Schottlaender, BEC TI UCLA/OCLC core record pilot project: Preliminary report SO LIBRARY RESOURCES & TECHNICAL SERVICES LA English DT Article AB This report details the record-creation phase of the UCLA/OCLC Core Record Pilot Project. A total of 384 records were created, consisting of 234 core and 150 full (control) records. Approximately half of the core records were coded K level in OCLC, and half I level. NACO authority work was done for all controlled (name, series, subject) access points in both the core and control records. Core record creation was determined to be significantly faster than control record creation: between 8.5% and 17% faster, depending upon whether learning curves are factored in. The core records created included, on average, 1.52 subject headings and 1.01 name headings each; the control records averaged 2.05 subject headings and 1.59 name headings each. The importance of these differences for access is unclear. Of the 384 records created, 30 core and 15 control records-a total of 45-were subsequently used by 91 institutions within two months of their creation. Of the 45 used, only 7 were modified: 6 core and 1 control. Of the ten modifications made to these records, only two involved the addition of controlled access points. With OCLC support, UCLA will continue to gather use and modification data for a year. C1 UNIV CALIF LOS ANGELES,COLLECT & TECH SERV,LOS ANGELES,CA. RP Kelley, SL (reprint author), SMITHSONIAN INST LIB,CATALOGING SERV DEPT,WASHINGTON,DC 20560, USA. NR 3 TC 4 Z9 4 U1 0 U2 0 PU AMER LIBRARY ASSN PI CHICAGO PA 50 E HURON ST, CHICAGO, IL 60611 SN 0024-2527 J9 LIBR RESOUR TECH SER JI Libr. Res. Tech. Serv. PD JUL PY 1996 VL 40 IS 3 BP 251 EP 260 PG 10 WC Information Science & Library Science SC Information Science & Library Science GA VV704 UT WOS:A1996VV70400004 ER PT J AU Gallegos, CL Vant, WN AF Gallegos, CL Vant, WN TI An incubation procedure for estimating carbon-to-chlorophyll ratios and growth-irradiance relationships of estuarine phytoplankton SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE phytoplankton; carbon-to-chlorophyll ratio; growth rate; estuarine ID MANUKAU HARBOR; NEW-ZEALAND; A-RATIO; PHOTOSYNTHESIS; LIGHT; RATES; TEMPERATURE; ZOOPLANKTON; MICROALGAE; NITROGEN AB The carbon-to-chlorophyll ratio of phytoplankton, theta, is difficult to determine by direct chemical measurement because natural waters also contain particulate carbon due to heterotrophic organisms and detritus that cannot be separated from the phytoplankton. When growth is balanced phytoplankton produce new C and chlorophyll in proportion to theta, but growth will be unbalanced in the short-term when there is accumulation of C that has not had time to be proportionately allocated to chlorophyll, or when the phytoplankton are adjusting theta to a new light regime (i.e. photoadaptation). We conducted incubations in Manukau Harbour, New Zealand, to estimate theta from increments in C-14 and chlorophyll using highly diluted water (fraction of unfiltered seawater = 0.05 to 0.1) to greatly reduce grazing by microzooplankton. Estimated theta ranged from 21.5 to 46.6 mg C (mg chi a)(-1), typical of healthy, nutrient-sufficient diatoms. Maximal growth rates varied from about 1 to 2 d(-1), and C- and chlorophyll-based growth rates agreed well with one another. Growth rates predicted from separate, short-term measurements of photosynthesis-irradiance (P-I) curves agreed well with light-saturated rates measured in 24 h incubations, but were generally higher than the 24 h measurements at lower irradiances, possibly due to greater effect of respiration in the longer incubations. Dilution had contrasting effects on chlorophyll and C-14 increments because grazed chlorophyll was degraded, but grazed C appeared to be conserved in the particulate matter. Failure to use diluted water for the incubations would have resulted in large overestimates in theta. We constructed a model of C-14 tracer flux and chlorophyll production to explore the consequences of unbalanced growth, e.g. photoadaptation, on estimates of theta determined using incubations substantially free of grazing. Simulations indicated that accurate estimates of theta can be obtained by commencing 24 h incubations prior to sunrise before new C accumulates, and by avoiding major shifts in the range of light intensities to which the phytoplankton are adapted. The procedure should be applicable in other environments provided precautions about sunrise start and avoidance of light shifts and photoinhibiting irradiances are observed. C1 NATL INST WATER & ATMOSPHER RES, HAMILTON, NEW ZEALAND. RP Gallegos, CL (reprint author), SMITHSONIAN ENVIRONM RES CTR, POB 28, EDGEWATER, MD 21037 USA. OI Gallegos, Charles/0000-0001-5112-0166 NR 41 TC 26 Z9 28 U1 3 U2 19 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD JUL PY 1996 VL 138 IS 1-3 BP 275 EP 291 DI 10.3354/meps138275 PG 17 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA VC147 UT WOS:A1996VC14700027 ER PT J AU Stanley, DJ Wingerath, JG AF Stanley, DJ Wingerath, JG TI Nile sediment dispersal altered by the Aswan High Dam: The kaolinite trace SO MARINE GEOLOGY LA English DT Letter ID MEDITERRANEAN SEA; DELTA; EGYPT; MINERALS AB Proportions of kaolinite have increased substantially in lower River Nile clay mineral assemblages since emplacement in 1964 of the High Dam at Aswan, Egypt. Monitoring this recent increase can be used to help gauge sediment load changes induced by the High Dam in the lower River Nile, between the dam and Nile delta and, eventually, offshore in the Mediterranean's Levantine Basin. High kaolinite values (to 50%) are recorded north of the new Nile delta presently forming in Lake Nasser, and are even higher below the High Dam (to 70%). Kaolinite is introduced to Lake Nasser from adjacent desert terrains largely from wind transported material and wave erosion of lake margins. As the major clay component of the suspended sediment load in lake waters, this mineral is released through the dam. Additional kaolinite enters the Nile system just below the High Dam from late Pleistocene and older sections scoured by swift, turbulent Nile waters flowing northward of the dam. During the past 31 years, sediment containing higher concentrations of kaolinite (similar to 30%) has migrated northward at a rate of similar to 10 km/year, and presently extends to Qena similar to 350 km north of the dam; this stretch defines the River Nile sector most altered since closure of the High Dam. It is predicted that enhanced proportions of kaolinite will be recorded at Cairo and the southern Nile delta within 50 years, and at the Mediterranean coast by the end of the next century. RP Stanley, DJ (reprint author), SMITHSONIAN INST, DELTAS GLOBAL CHANGE PROGRAM, WASHINGTON, DC 20560 USA. NR 41 TC 19 Z9 19 U1 1 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0025-3227 J9 MAR GEOL JI Mar. Geol. PD JUL PY 1996 VL 133 IS 1-2 BP 1 EP 9 DI 10.1016/0025-3227(96)00019-9 PG 9 WC Geosciences, Multidisciplinary; Oceanography SC Geology; Oceanography GA UY014 UT WOS:A1996UY01400001 ER PT J AU Brown, P Hildebrand, AR Green, DWE Page, D Jacobs, C Revelle, D Tagliaferri, E Wacker, J Wetmiller, B AF Brown, P Hildebrand, AR Green, DWE Page, D Jacobs, C Revelle, D Tagliaferri, E Wacker, J Wetmiller, B TI The fall of the St-Robert meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INNISFREE METEORITE; FIREBALLS; METEOROIDS; RECORDS; ORBIT; FRAGMENTATION; NUCLIDES; NETWORK AB The St-Robert (Quebec, Canada) meteorite shower occurred on 1994 June 15 at 0h02m UT accompanied by detonations audible for >200 km from the fireball endpoint. The fireball was recorded by visual observers in Vermont, New York State, New Hampshire, Quebec and Ontario as well as by optical and infrared sensors in Earth-orbit. Penetration to an altitude of 36 km occurred similar to 60 km to the northeast of Montreal, where the bolide experienced several episodes of fragmentation. A total of 20 fragments of this H5 chondrite, comprising a total mass of 25.4 kg, were recovered in an ellipse measuring 8 x 3.5 km. One fragment of the shower partially penetrated the aluminum roof of a shed. Interpretation of the visual and satellite data suggests that the fireball traveled from south-southwest to north-northeast, with a slope from the horizontal of 55 degrees-61 degrees. A statistical evaluation of the likely heliocentric orbits for the body prior to collision with the Earth, coupled with theoretical modeling of the entry, suggests an entry velocity in the range of 12.7-13.3 km/s; the meteoroid had moved in a low-inclination orbit, with orbital perihelion located extremely close to the Earth's orbit. From satellite optical data, it is found that the photometric mass consumed during the largest detonation is similar to 1200 kg. Estimation of the amplitude of the acoustic signal detected by the most distant observer yields a source energy near 0.5 kt TNT equivalent energy, which corresponds to a mass of order 10 metric tonnes. This measure is uncertain to approximately one order of magnitude. Theoretical modeling of the entry of the object suggests a mass near 1600 kg. Cosmogenic radionuclide activities constrain the lower initial mass to be similar to 700 kg with an upper limit near 4000 kg. Seismic data possibly associated with the fireball suggest extremely poor coupling between the airwave and the ground. The total mass estimated to have reached the ground is similar to 100 kg (in material comprising >55 g fragments), while the preatmospheric mass is found to be most probably in the range of 1200-2000 kg. C1 GEOL SURVEY CANADA, NAT RESOURCES CANADA, COTINENTAL GEOSCI DIV, OTTAWA, ON K1A 0Y3, CANADA. SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. ROYAL ASTRON SOC CANADA, QUEBEC CTR, MONTREAL, PQ H2A 1K4, CANADA. SANDIA NATL LABS, ALBUQUERQUE, NM 87185 USA. LOS ALAMOS NATL LAB, LOS ALAMOS, NM 87545 USA. ET SPACE SYST, CAMARILLO, CA 93012 USA. PACIFIC NW LAB, RICHLAND, WA 99352 USA. GEOL SURVEY CANADA, NAT RESOURCES CANADA, PACIFIC DIV, OTTAWA, ON K1A 0Y3, CANADA. RP Brown, P (reprint author), UNIV WESTERN ONTARIO, DEPT PHYS, LONDON, ON N6A 3K7, CANADA. NR 72 TC 41 Z9 41 U1 0 U2 1 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 1996 VL 31 IS 4 BP 502 EP 517 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA UX180 UT WOS:A1996UX18000010 ER PT J AU Sansom, AE Dotani, T Okada, K Yamashita, A Fabbiano, G AF Sansom, AE Dotani, T Okada, K Yamashita, A Fabbiano, G TI ASCA observations of 'the Antennae' SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies, individual, NGC 4038/9; galaxies, interactions; X-rays, galaxies ID EARLY-TYPE GALAXIES AB We analyse X-ray data from the ASCA satellite for the galaxies NGC 4038/9 (also known as 'the Antennae'), and find emission from both galaxies, At least two spectral components are required to describe the overall emission from these galaxies: thermal emission from a plasma at 0.8 keV, and a component at higher energies. The hot gas contributes about half of the Bur in the 0.5- to 6-keV band. If the column density to the higher energy component is > 2 x 10(21) cm(-2) then the fitted abundance in the hot gas component is less than 0.2 times solar, This low abundance is not expected for the hot interstellar medium in NGC 4038/9 in which supernovae and star formation (expected to enrich and heat the gas) are ongoing. We do not detect any spatial variations in the spectrum. We relate these findings to data obtained by other X-ray satellites (Einstein, ROSAT) for this interacting galaxy pair. C1 INST SPACE & ASTRONAUT SCI,SAGAMIHARA,KANAGAWA 229,JAPAN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Sansom, AE (reprint author), UNIV CENT LANCASHIRE,CTR ASTROPHYS,PRESTON PR1 2HE,LANCS,ENGLAND. NR 37 TC 20 Z9 20 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 1996 VL 281 IS 1 BP 48 EP 58 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UW119 UT WOS:A1996UW11900007 ER PT J AU Zotz, G Tyree, MT AF Zotz, G Tyree, MT TI Water stress in the epiphytic orchid, Dimerandra emarginata (G. Meyer) Hoehne SO OECOLOGIA LA English DT Article DE epiphytes; orchids; water balance; crassulacean acid metabolism; photoinhibition ID CHLOROPHYLL FLUORESCENCE; PHOTOSYSTEM-II; COMPARATIVE ECOPHYSIOLOGY; GUZMANIA-MONOSTACHIA; C-3 BROMELIADS; LIGHT; CAM; PHOTOSYNTHESIS; PHOTOINHIBITION; EFFICIENCY AB The epiphytic orchid, Dimerandra emarginata, occurs in habitats characterized by high light intensities and very variable water supply. Long-term observations of the water status indicate that this species experienced at least moderate water stress over most of the year. Well-watered, it showed high rates of net CO2 uptake (A, 7 mu mol m(-2) s(-1)), high transpiration rates (E, 14 mmol m(-2) s(-1)), and little nocturnal acidification. Drought induced crassulacean acid metabolism activity and resulted in a strong decline of both A and E. The same conditions also led to chronic photoinhibition as indicated by a predawn ratio of variable to maximum fluorescence (F-v/F-m) of 0.6 after 9 days of drought. Diurnal changes in fluorescence characteristics were much more pronounced. Midday ratios of dark adapted F-v/F-m were as low as 0.35, but recovered in the afternoon and were probably mostly due to non-photochemical quenching of photosynthesis. Measured water losses of leaves and stems were compared to plant water content (PWC). In large plants, about 32% of PWC was transpired on a single day under well-watered conditions. Model calculations indicate that transpiration per unit leaf area should be strongly dependent upon plant size in this species. Comparisons of calculated daily water loss, PWC and the length of drought periods suggest that D. emarginata can only survive a dry season by drawing on the water reserves of older stems and by an efficient uptake of the occasional rain. C1 UNIV VERMONT,DEPT BOT,BURLINGTON,VT 05405. USDA ARS,BURLINGTON,VT 05405. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 37 TC 37 Z9 41 U1 2 U2 11 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUL PY 1996 VL 107 IS 2 BP 151 EP 159 DI 10.1007/BF00327898 PG 9 WC Ecology SC Environmental Sciences & Ecology GA VA148 UT WOS:A1996VA14800002 PM 28307300 ER PT J AU Wells, JC Schultz, DR Gavras, P Pindzola, MS AF Wells, JC Schultz, DR Gavras, P Pindzola, MS TI Numerical solution of the time-dependent Schrodinger equation for intermediate-energy collisions of antiprotons with hydrogen SO PHYSICAL REVIEW A LA English DT Article ID DOUBLE IONIZATION; ATOM COLLISIONS; PROTON IMPACT; HARTREE-FOCK; HELIUM; HE2++HE; SPECTRA; SINGLE AB We study the behavior of ionization intermediate-energy collisions of antiprotons with atomic hydrogen by direct solution of the time-dependent Schrodinger equation represented on a three-dimensional Cartesian lattice. Total cross sections for these processes are computed over the collision energy range of 0.2 to 500 keV from knowledge of the asymptotic state probabilities as a function of impact parameter. The computed ionization cross sections are in good agreement with results from recent experiments conducted at CERN [Phys. Rev. Lett. 74, 4627 (1995)]. In the energy range from 0.2 top 30 keV, for which measurements are not available, our calculations are in qualitative agreement with other results based on classical-trajectory and coupled-channel methods, confirming the predicted significant difference from the analog proton-impact ionization process. This contrast with proton-hydrogen collisions is also explored qualitatively by employing a model two-dimensional space in which lattice solutions are less computationally intensive. C1 OAK RIDGE NATL LAB,DIV PHYS,OAK RIDGE,TN 37831. AUBURN UNIV,DEPT PHYS,AUBURN,AL 36849. RP Wells, JC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138, USA. RI Wells, Jack/D-3675-2016 OI Wells, Jack/0000-0002-5083-3030 NR 38 TC 80 Z9 81 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL PY 1996 VL 54 IS 1 BP 593 EP 604 DI 10.1103/PhysRevA.54.593 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA UX034 UT WOS:A1996UX03400067 ER PT J AU Norden, BB Krombein, KV AF Norden, BB Krombein, KV TI Nest and prey of Solierella vierecki (Rohwer) (Hymenoptera: Sphecidae: Larrinae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article RP Norden, BB (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ENTOMOL,MRC-165,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 1996 VL 98 IS 3 BP 607 EP 607 PG 1 WC Entomology SC Entomology GA VC381 UT WOS:A1996VC38100023 ER PT J AU Erwin, DH AF Erwin, DH TI The mother of mass extinctions SO SCIENTIFIC AMERICAN LA English DT Article RP Erwin, DH (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. RI Erwin, Douglas/A-9668-2009 NR 4 TC 13 Z9 13 U1 0 U2 5 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 SN 0036-8733 J9 SCI AM JI Sci.Am. PD JUL PY 1996 VL 275 IS 1 BP 72 EP 78 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UR016 UT WOS:A1996UR01600030 ER PT J AU Soltis, PS Soltis, DE Weller, SG Sakai, AK Wagner, WL AF Soltis, PS Soltis, DE Weller, SG Sakai, AK Wagner, WL TI Molecular phylogenetic analysis of the Hawaiian endemics Schiedea and Alsinidendron (Caryophyllaceae) SO SYSTEMATIC BOTANY LA English DT Article ID CHLOROPLAST DNA; EVOLUTION; ALSINOIDEAE; ASTERACEAE; ISLANDS; LIMITS; DIOECY; RATES AB Schiedea and Alsinidendron (Caryophyllaceae), which represent the fifth or sixth largest endemic radiation of species in the angiosperm flora of the Hawaiian Islands, exhibit striking diversity in morphology, breeding system, and habitat. To gain a historical perspective on this diversity, we conducted a phylogenetic analysis using restriction site variation in chloroplast DNA and nuclear ribosomal DNA. In addition, we compared, and ultimately combined, the molecular data with a recently published morphological data set. Within the Schieden-Alsinidendron lineage, DNA variation is limited, and relationships are generally poorly resolved. These results raise the possibility that, following the initial colonization of the Hawaiian archipelago and the early diversification of the complex, much of the complex radiated rapidly and relatively recently. Phylogenetic analyses of DNA data revealed three clades within the complex (the S. membranacea, S. nuttallii, and S. adamantis clades), in agreement with results of a morphologically-based analysis. Molecular data do not, however, support the S. globosa clade, a weakly-supported clade based on morphology. A combined analysis of morphological and molecular data provided both greater resolution and stronger internal support than either data set did individually. The molecular and combined topologies suggest nearly identical patterns of the evolution of sexual dimorphism, habitat shifts, and biogeography within the complex. However, the greater resolution in trees derived from the combined analysis suggests simpler patterns of breeding-system evolution and habitat shifts. Sexual dimorphism may have evolved twice in the complex, with a single reversal to hermaphroditism in one species, or perhaps only once, with three reversals to hermaphroditism. Although the habitat occupied by the ancestor of the complex remains uncertain, it appears that a single shift to dry habitats more or less accompanied the evolution of dimorphic breeding systems, followed by a single shift back to a mesic environment in one species. Alternatively, two parallel shifts to dry habitats may have occurred. Molecular data are consistent with an origin on Kaua'i of the S. membranacea, S. adamantis, and S. nuttallii clades, as suggested by previous morphological analyses. However, both the molecular and combined trees suggest it is equally likely that the complex originated on O'ahu. C1 UNIV CALIF IRVINE,DEPT ECOL & EVOLUTIONARY BIOL,IRVINE,CA 92717. SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP Soltis, PS (reprint author), WASHINGTON STATE UNIV,DEPT BOT,PULLMAN,WA 99164, USA. RI Soltis, Pamela/L-5184-2015 NR 23 TC 41 Z9 41 U1 0 U2 8 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 1996 VL 21 IS 3 BP 365 EP 379 DI 10.2307/2419665 PG 15 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA WQ817 UT WOS:A1996WQ81700008 ER PT J AU Multhauf, RP AF Multhauf, RP TI Science and civilisation in China, vol 5, Chemistry and chemical technology .6. Military technology: Missiles and sieges - Needham,J, Yates,RDS SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 1996 VL 37 IS 3 BP 621 EP 622 DI 10.2307/3107175 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA WA431 UT WOS:A1996WA43100015 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI The illusion of miracle weapons: The role of jets and missiles in the arms policy of the Third Reich - German - Schabel,R SO TECHNOLOGY AND CULTURE LA English DT Book Review RP Neufeld, MJ (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 1996 VL 37 IS 3 BP 642 EP 644 DI 10.2307/3107187 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA WA431 UT WOS:A1996WA43100027 ER PT J AU Knowlton, N AF Knowlton, N TI Trench Warfare on the shore: Interclonal aggression in sea anemones SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Editorial Material ID ANTHOPLEURA-ELEGANTISSIMA; INTERSPECIFIC AGGRESSION; SCLERACTINIAN CORALS C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 9 TC 2 Z9 2 U1 1 U2 9 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD JUL PY 1996 VL 11 IS 7 BP 271 EP 272 DI 10.1016/0169-5347(96)30026-8 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA UR378 UT WOS:A1996UR37800001 PM 21237837 ER PT J AU Bayer, FM AF Bayer, FM TI Three new species of precious coral (Anthozoa: Gorgonacea, genus Corallium) from Pacific waters SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Two new species of Corallium from New Caledonia with the consolidated axial skeleton having smooth pits with beaded margins accommodating the autozooids are described, Corallium thrinax with double-club sclerites, C. nix without. A third new species, C. kishinouyei, lacking smooth, well-defined axial pits and lacking double-club sclerites, is described from Cross Sea Mount south of Hawaii. Preliminary observations of axis formation are reported. RP Bayer, FM (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 15 TC 12 Z9 12 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 25 PY 1996 VL 109 IS 2 BP 205 EP 228 PG 24 WC Biology SC Life Sciences & Biomedicine - Other Topics GA UV770 UT WOS:A1996UV77000001 ER PT J AU Ferrari, FD Markhaseva, EL AF Ferrari, FD Markhaseva, EL TI Parkius karenwishnerae, a new genus and species of calanoid copepod (Parkiidae, new family) from benthopelagic waters of the eastern tropical Pacific Ocean SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The last five copepodid stages of a new genus and species of calanoid copepod, Parkins karenwishnerae, are described. The basis of the maxilliped of P. karenwishnerae is elongate distal to its two medial setae and its medial row of denticles; endopodal segments 2-5 are attenuate, forming a hook-like structure distally, with denticles along the concave margin. These character states are expected to be found in adult females of other species of Parkius. Parkiidae, new family, are clausocalanoidean copepods whose adult female has two Bradford's setae on the fifth enditic lobe on the basis of maxilla 2, two medial setae on the basis of the maxilliped, and endopodal segments of the maxilliped with 4, 0, 1, 1, 1 setae. On leg 1 the anterior denticles of Von Vaupel Klein's organ are found proximal to the presumptive boundary of the second endopodal segment. C1 ACAD SCI,INST ZOOL,ST PETERSBURG 199034,RUSSIA. RP Ferrari, FD (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL MRC534,WASHINGTON,DC 20560, USA. NR 17 TC 17 Z9 21 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 25 PY 1996 VL 109 IS 2 BP 264 EP 285 PG 22 WC Biology SC Life Sciences & Biomedicine - Other Topics GA UV770 UT WOS:A1996UV77000006 ER PT J AU Manning, RB Felder, DL AF Manning, RB Felder, DL TI Nannotheres moorei, a new genus and species of minute pinnotherid crab from Belize, Caribbean Sea (Crustacea: Decapoda: Pinnotheridae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID BRACHYURA AB Nannotheres moorei is described from a small pteriid bivalve mollusk taken in the Caribbean Sea off Belize. This minute, ovigerous pinnotherid crab can be distinguished by its size and the 2-segmented palp on its third maxilliped. With a carapace width of about 1.5 mm in a sexually mature female, it may be the smallest known species of crab. C1 UNIV SW LOUISIANA,DEPT BIOL,LAFAYETTE,LA 70504. RP Manning, RB (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 22 TC 6 Z9 8 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 25 PY 1996 VL 109 IS 2 BP 311 EP 317 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA UV770 UT WOS:A1996UV77000010 ER PT J AU Mathis, WN AF Mathis, WN TI Australian beach flies (Diptera: Canacidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The Australian fauna of beach flies (8 genera and 14 species), excluding Zaleinae, is reviewed, including description of seven new species as follows (type locality indicated in parentheses): Nocticanace australina (NSW: Lord Howe Island, Roach Island Beach), Procanace mcalpinei (NSW: Karuah), Chaetocanace flavipes (WA: West Kimberley, 4 km SSW of Cape Bertholet), Chaetocanace koongarra (WA: Koongarra, 15 km E of Mt. Cahill), Chaetocanace longicauda (NT: 35 km W Jabiru, South Alligator River area), Dynomiella australica (TAS: Squeaking Point near Port Sorell), and Xanthocanace collessi (WA: West Kimberley, 5 km SSW of Cape Bertholet). Procanace Hendel and Dynomiella Giordani Soika are reported for the first time from Australia. An undescribed genus and species, represented by a single female, is also reported. RP Mathis, WN (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ENTOMOL,MRC 169,WASHINGTON,DC 20560, USA. NR 33 TC 2 Z9 3 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 25 PY 1996 VL 109 IS 2 BP 326 EP 348 PG 23 WC Biology SC Life Sciences & Biomedicine - Other Topics GA UV770 UT WOS:A1996UV77000012 ER PT J AU Graves, GR AF Graves, GR TI Hybrid wood warblers, Dendroica striata x Dendroica castanea (Aves: Fringillidae: tribe Parulini) and the diagnostic predictability of avian hybrid phenotypes SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID HERITABILITY; POPULATION AB The plumage pattern and color and external morphology of hybrid wood warblers (Dendroica striata X Dendroica castanea) are described. This hybrid combination constitutes the only known case of hybridization between two broadly sympatric species of the genus Dendroica (Fringillidae; Tribe Parulini), that is represented by both male and female specimens in definitive alternate plumage. The plumage of the hybrids exhibited a mosaic of character states that varied in the degree of intermediacy between those of the parental species. External measurements of the hybrids fell within the cumulative ranges of characters of the postulated parental species. I hypothesize that the diagnostic predictability of hybrid phenotypes decreases as an inverse function of genetic relatedness of the hybridizing species. RP Graves, GR (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 32 TC 16 Z9 16 U1 0 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 25 PY 1996 VL 109 IS 2 BP 373 EP 390 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA UV770 UT WOS:A1996UV77000016 ER PT J AU Lucas, SG Emry, RJ AF Lucas, SG Emry, RJ TI Early record of indricothere (Mammalia: Perissodactyla: Hyracodontidae) from the Aral sea region of western Kazakhstan SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Upper molar fragments of the indricothere rhinoceros Paraceratherium sp. are described from the Chilikta Formation at Altyn Chokysu, north of the Aral Sea in western Kazakhstan. Marine bivalves indicate the Chilikta Formation is of early Oligocene (Late Rupelian) age, and thus provide the first direct cross-correlation of an occurrence of Paraceratherium with the marine timescale. This find extends the temporal range of Paraceratherium in the Aral Sea region back from the late Oligocene to the early Oligocene, making it consistent with the temporal range noted for the genus in China. Paraceratherium thus had a geologically synchronous first appearance across Eurasia during the late early Oligocene. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALAEONTOL,WASHINGTON,DC 20560. RP Lucas, SG (reprint author), NEW MEXICO MUSEUM NAT HIST & SCI,1801 MT RD NW,ALBUQUERQUE,NM 87104, USA. NR 13 TC 2 Z9 3 U1 0 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 25 PY 1996 VL 109 IS 2 BP 391 EP 396 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA UV770 UT WOS:A1996UV77000017 ER PT J AU Lucas, SG Emry, RJ AF Lucas, SG Emry, RJ TI Late Eocene entelodonts (Mammalia: Artiodactyla) from inner Mongolia, China SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Previously undescribed specimens of Entelodon from the late Eocene (Ergilian) of Nei Monggol, China represent two species, small and large. We identify the small species as Entelodon gobiensis (Trofimov, 1952), because this is the oldest valid name available for a relatively small species of Asian Entelodon. E. diconodon (Trofimov, 1952) is a nomen dubium, and it is probable that E. ordosius (Young & Chow, 1956), E. major Biryukov, 1961 and E. orientalis Dashzeveg, 1965 are junior subjective synonyms of E. gobiensis (Trofimov, 1952). The large species is Entelodon dirus Matthew & Granger, 1923, a species previously known only from its holotype M3, but to which we now refer a lower jaw with p2-m3. In Asia, Entelodon is more common in strata of Ergilian (late Eocene) age; its Shandgolian (early Oligocene) occurrences are few. Entelodonts originated in Asia during the middle Eocene, immigrated to North America (late Eocene) and Europe (early Oligocene) and persisted until late Oligocene in Eurasia and North America. The last entelodonts, from the early Miocene of North America, apparently arose from a separate, latest Oligocene emigration from Asia. C1 SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT PALEOBIOL, WASHINGTON, DC 20560 USA. RP Lucas, SG (reprint author), NEW MEXICO MUSEUM NAT HIST & SCI, 1801 MT RD NW, ALBUQUERQUE, NM 87104 USA. NR 22 TC 4 Z9 5 U1 1 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 25 PY 1996 VL 109 IS 2 BP 397 EP 405 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA UV770 UT WOS:A1996UV77000018 ER PT J AU Ellithorpe, JD Kochanek, CS Hewitt, JN AF Ellithorpe, JD Kochanek, CS Hewitt, JN TI Visibility LensClean and the reliability of deconvolved radio images SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; radio continuum, galaxies; techniques, image processing; techniques, interferometric ID GRAVITATIONAL LENS 0957+561; TIME-DELAY; SELF-CALIBRATION; ALGORITHM; ASTRONOMY AB Multiple imaging by a gravitational lens strongly correlates widely separated regions of the image, allowing reconstruction of both the lens potential and the unlensed source structure. Thus, lens inversion is analogous to self-calibration because both techniques construct a model of the distorting medium constrained by consistency requirements in the data. The lens inversion algorithm, LensClean, has assumed that the image reconstruction techniques used in radio astronomy do not introduce errors that affect the lens modeling, We extend LensClean to work directly from visibility data, with the option of adding self-calibration steps, and investigate the level of systematic errors present in reconstructions of a point source system, MG 0414+0534, and an extended emission system, MG 1654+1346. We find that CLEAN-reconstructed radio maps contain significant deconvolution errors that degrade both the accuracy of reconstructed lens images and broaden the uncertainty in physical parameters of the lens models. Lens model reconstructions, even with a less than perfect lens model, are generally a better fit to the visibility data than a standard CLEAN map. Rigorous analyses of radio observations should be performed directly on the visibility data. C1 MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. MIT, ELECTR RES LAB, CAMBRIDGE, MA 02139 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NR 36 TC 20 Z9 20 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1996 VL 464 IS 2 BP 556 EP 567 DI 10.1086/177346 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UQ194 UT WOS:A1996UQ19400004 ER PT J AU Ferrarese, L Freedman, WL Hill, RJ Saha, A Madore, BF Kennicutt, RC Stetson, PB Ford, HC Graham, JA Hoessel, JG Han, MS Huchra, J Hughes, SM Illingworth, GD Kelson, D Mould, JR Phelps, R Silbermann, NA Sakai, S Turner, A Harding, P Bresolin, F AF Ferrarese, L Freedman, WL Hill, RJ Saha, A Madore, BF Kennicutt, RC Stetson, PB Ford, HC Graham, JA Hoessel, JG Han, MS Huchra, J Hughes, SM Illingworth, GD Kelson, D Mould, JR Phelps, R Silbermann, NA Sakai, S Turner, A Harding, P Bresolin, F TI The extragalactic distance scale key project .4. The discovery of Cepheids and a new distance to M100 using the Hubble space telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; galaxies, distances and redshifts; galaxies, individual (M100) ID VIRGO CLUSTER; CCD PHOTOMETRY; GALAXIES; CLOUD; STARS AB We report on observations of Cepheids in the Virgo spiral galaxy M100, based on data obtained with the Wide Field and Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope (HST). The observations are part of the HST Key Project on the Extragalactic Distance Scale, which aims to provide a measurement of the Hubble constant H-0 with 10% accuracy. A total of 12 epochs were obtained using the F555W filter (transformed to Johnson V), and 4 epochs using the F814W filter (transformed to Cousins I). Photometry on the data was performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME; a total of 52 Cepheids, with periods ranging from about 10 to 70 days, were identified based on both sets of photometry. We have fitted V and I period-luminosity relations and derived apparent V and I distance moduli assuming a Large Magellanic Cloud distance modulus and mean color excess of mu(LMC) = 18.50 +/- 0.10 mag and E(B - V) = 0.10 mag, respectively. Using the extinction law given by Cardelli, Clayton, & Mathis, and adopting our most recent WFPC2 (''long-exposure'') zero-point calibration, we obtain a true distance modulus for M100 of mu(0) = 30.04 +/- 0.17 mag, corresponding to a distance d = 16.1 +/- 1.3 Mpc, and a total (Galactic plus internal) mean color excess E(B - V) = 0.10 +/- 0.06 mag. When compared with the preliminary distance of 17.1 +/- 1.8 Mpc derived by Freedman et al. from the same set of data, the results presented here benefit from a larger sample size, refinements in the zero-point calibration, and improvements in the software packages used for the photometry. The two results agree to within their quoted errors. C1 SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. CALTECH,PASADENA,CA 91125. NASA,IPAC EXTRAGALACT DATABASE,PASADENA,CA 91125. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. UNIV WISCONSIN,MADISON,WI 53706. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0HA,ENGLAND. UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,INST ADV STUDIES,WESTON,ACT 2611,AUSTRALIA. RP Ferrarese, L (reprint author), JOHNS HOPKINS UNIV,BALTIMORE,MD 21218, USA. NR 53 TC 177 Z9 177 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1996 VL 464 IS 2 BP 568 EP & DI 10.1086/177347 PN 1 PG 49 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UQ194 UT WOS:A1996UQ19400005 ER PT J AU Bartelmann, M Narayan, R Seitz, S Schneider, P AF Bartelmann, M Narayan, R Seitz, S Schneider, P TI Maximum likelihood cluster reconstruction SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, clusters, general; gravitational lensing; methods, numerical ID DARK MATTER AB We present a novel method to reconstruct the mass distribution of galaxy clusters from their gravitational lens effect on background galaxies. The method is based on a least-chi(2) fit of the two-dimensional gravitational cluster potential. The method combines information from shear and magnification by the duster lens and is designed to easily incorporate possible additional information. We describe the technique and demonstrate its feasibility with simulated data. Both the cluster morphology and the total cluster mass are well reproduced. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Bartelmann, M (reprint author), MAX PLANCK INST ASTROPHYS,KARL SCHWARZSCHILD STR 1,D-85748 GARCHING,GERMANY. RI Bartelmann, Matthias/A-5336-2014; OI Bartelmann, Matthias/0000-0001-6951-3582; Narayan, Ramesh/0000-0002-1919-2730 NR 32 TC 65 Z9 65 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1996 VL 464 IS 2 BP L115 EP L118 DI 10.1086/310114 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UQ195 UT WOS:A1996UQ19500005 ER PT J AU Harrus, IM Hughes, JP Helfand, DJ AF Harrus, IM Hughes, JP Helfand, DJ TI Discovery of an X-ray synchrotron nebula associated with the radio pulsar PSR B1853+01 in the supernova remnant W44 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, individual (W44); pulsars, individual (PSR B1853+01); radiation mechanisms, nonthermal; supernova remnants; X-rays, ISM ID EMISSION AB We report the detection, using data from the Advanced Satellite for Cosmology and Astrophysics (ASCA), of a hard X-ray source in the vicinity of the radio pulsar PSR B1853+01, which is located within the supernova remnant (SNR) W44. PSR B1853+01, a 267 ms pulsar, has to date been detected only in the radio band. Previous observations at soft X-ray energies (e.g., with ROSAT HRI) have failed to detect any significant X-ray emission (pulsed or unpulsed) from the pulsar. In addition, no high-energy emission (greater than or similar to 4 keV) has been detected previously from W44. Over the 0.5-4.0 keV band, the ASCA data show soft thermal emission from W44, with a morphology very similar to that observed earlier by Einstein and ROSAT. In the high-energy band (4.0-9.5 keV), the SNR is, for the most part, invisible, although a source coincident with the position of PSR B1853+01 is evident. The observed ASCA spectra are consistent with a power-law origin (photon index similar to 2.3) for the X-ray emission from this source at a flux level (flux density similar to 0.5 mu Jy at 1 keV) consistent with previous upper limits. The maximum allowed size for the source is determined directly from the ASCA data (<5'), while the minimum size is derived from the nondetection of a point source in the ROSAT HRI data (greater than or similar to 30''). Timing analysis of the hard X-ray source failed to detect pulsations at the pulsar's period. Based on these lines of evidence, we conclude that the new hard source in W44 represents an X-ray synchrotron nebula associated with PSR B1853+01, rather than the beamed output of the pulsar itself. This discovery adds W44 to the small group of previously known plerionic SNRs. This nebula lies at the low end of, but is consistent with, the correlation between X-ray luminosity and pulsar spin-down energy loss found for such objects, lending further support to our interpretation. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. COLUMBIA UNIV,DEPT ASTRON,NEW YORK,NY 10027. NR 17 TC 35 Z9 35 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1996 VL 464 IS 2 BP L161 EP & DI 10.1086/310106 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UQ195 UT WOS:A1996UQ19500016 ER PT J AU Jaldehag, RTK Johansson, JM Davis, JL Elosegui, P AF Jaldehag, RTK Johansson, JM Davis, JL Elosegui, P TI Geodesy using the Swedish permanent GPS network: Effects of snow accumulation on estimates of site positions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB We have observed variations at the several centimeter level in estimates of the vertical coordinate of site position. The estimates are obtained from our analysis of data acquired from the Swedish permanent Global Positioning System (GPS) network. The observed variations are strongly correlated with changes in the indirectly inferred accumulation of snow, which we assume collects on the radomes and pillars; the GPS sites could not be observed directly due to their remoteness. Numerical simulations which assume a simple geometry for the snow cover are used to study the effects of snow accumulation on GPS phase observables and hence on estimates of the vertical coordinate of site position obtained from these observables. Our results indicate that the variations in the vertical coordinate of site position can be fully explained by reasonable accumulations of snow which retard the GPS signals and enhance signal scattering effects. C1 CHALMERS UNIV TECHNOL,ONSALA SPACE OBSERV,DEPT RADIO & SPACE SCI,S-43992 ONSALA,SWEDEN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 9 TC 22 Z9 22 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 15 PY 1996 VL 23 IS 13 BP 1601 EP 1604 DI 10.1029/96GL00970 PG 4 WC Geosciences, Multidisciplinary SC Geology GA UT009 UT WOS:A1996UT00900014 ER PT J AU Kochanek, CS Rybicki, GB AF Kochanek, CS Rybicki, GB TI Deprojection of axially symmetric objects SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies, fundamental parameters; galaxies, kinematics and dynamics; galaxies, photometry AB The deprojection of axisymmetric density distributions is generally indeterminate to within the addition of certain axisymmetric distributions (konus densities) that are invisible in projection. The known class of konus densities is expanded considerably here through the introduction of semikonus functions. These functions are closed with respect to multiplication in ordinary space, and the real part of an arbitrary polynomial of semikonus functions is a konus function. This property facilitates the construction of semikonus (and konus) functions with tailored properties, such as asymptotic forms. We also develop a simple technique for constructing several classes of konus distributions with arbitrary density profiles in the equatorial plane. RP Kochanek, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 7 TC 15 Z9 15 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 15 PY 1996 VL 280 IS 4 BP 1257 EP 1263 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UT637 UT WOS:A1996UT63700030 ER PT J AU Lin, H Kirshner, RP Shectman, SA Landy, SD Oemler, A Tucker, DL Schechter, PL AF Lin, H Kirshner, RP Shectman, SA Landy, SD Oemler, A Tucker, DL Schechter, PL TI The luminosity function of galaxies in the Las Campanas Redshift Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, observations; galaxies, distances and redshifts; galaxies, luminosity function, mass function; surveys ID FIELD GALAXIES; NEARBY GALAXIES; EVOLUTION; DENSITY; UNIVERSE; VELOCITY; COUNTS; BLUE AB We present the r-band luminosity function for a sample of 18,678 galaxies, with average redshift z = 0.1, from the Las Campanas Redshift Survey (LCRS). The luminosity function may be fitted by a Schechter function with M* = -20.29 +/- 0.02 + 5 log h, alpha = -0.70 +/- 0.05, and phi* = 0.019 +/- 0.001 h(3) Mpc(-3), for absolute magnitudes -23.0 less than or equal to M - 5 log h less than or equal to -17.5 and h = H-0/(100 km s(-1) Mpc(-1)). Over the same absolute magnitude range, the mean galaxy density is 0.029 +/- 0.002 h(3) Mpc(-3) for a volume extending to cz = 60,000 km s(-1). We compare our luminosity function to that from other redshift surveys; in particular, our luminosity function normalization is consistent with that of the Stromlo-APM survey and is therefore a factor of 2 below the normalization implied by the b(J) approximate to 20 bright galaxy counts. Our normalization thus indicates that much more evolution is needed to match the faint galaxy count data, compared to minimal evolution models that normalize at b(J) approximate to 20. Also, we show that our faint-end slope alpha = -0.7, though ''shallower'' than typical previous values alpha = -1, results primarily from fitting the detailed shape of the LCRS luminosity function, rather than from any absence of intrinsically faint galaxies from our survey. Finally, we find that the faint end of the luminosity function is dominated by galaxies with emission lines. Using [O II] lambda 3727 equivalent width W-lambda = 5 Angstrom as the dividing line, we find significant differences in the luminosity functions of emission and nonemission galaxies, particularly in their alpha values; emission galaxies have Schechter parameters M* = -20.03 +/- 0.03 + 5 log h and alpha = -0.9 +/- 0.1, while nonemission galaxies are described by M* = -20.22 +/- 0.02 + 5 log h and alpha = -0.3 + 0.1. The average [O II] lambda 23727 equivalent widths do not change significantly with redshift, consistent with a star formation rate that stays constant over the depths sampled by the LCRS. This result holds for galaxies of different luminosities and over the respective redshift ranges that these galaxies may be observed, in particular up to about z = 0.2 for galaxies brighter than M*. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. CARNEGIE INST WASHINGTON OBSERV, PASADENA, CA 91101 USA. YALE UNIV, DEPT ASTRON, NEW HAVEN, CT 06520 USA. ASTROPHYS INST POTSDAM, D-14482 POTSDAM, GERMANY. MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. NR 57 TC 279 Z9 279 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1996 VL 464 IS 1 BP 60 EP 78 DI 10.1086/177300 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UN840 UT WOS:A1996UN84000007 ER PT J AU Grogin, NA Narayan, R AF Grogin, NA Narayan, R TI A new model of the gravitational lens 0957+561 and a limit on the Hubble constant SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; gravitational lensing; quasars, individual (0957+561) ID ELLIPTICAL POTENTIAL WELLS; TIME-DELAY; QUASAR 0957+561; QSO 0957+561; SYSTEM 0957+561; DARK MATTER; IMAGES; DISTRIBUTIONS; Q0957+561; PARAMETER AB We present a simple mass model for the lensing galaxy in the gravitationally lensed quasar 0957+561. We represent the galaxy as a softened power-law sphere (SPLS), a generalization of the singular isothermal sphere with three parameters-rho(0), the central density; theta(c), the angular core radius; and eta, l, the radial index, which is defined such that mass increases as r(eta) at large radius. As in previous studies, we approximate the galaxy cluster surrounding the lensing galaxy by means of a quadratic potential described by its convergence kappa and shear gamma. A feature of the model is that it does not require a large central compact mass. We fit the model to a recent high-resolution VLBI map of the two images of 0957+561. The data provide a number of independent constraints, and the model fit has 6 degrees of freedom, which is a significant improvement over previous models. Although the reduced chi(2) of the best-fit model is only 4.3, nevertheless we obtain a tight constraint on the radial index, 1.07 < eta < 1.18, at the 95% confidence level. Thus, the galaxy has mass increasing slightly more rapidly than isothermal (eta = 1) out to at least 15 h(-1) kpc. Since the light from the galaxy follows a de Vaucouleurs profile, we deduce that the mass-to-light ratio of the galaxy increases rapidly with increasing radius. We also obtain an upper limit on the core radius, namely theta(c) < 0''.11 or linear core radius <330 h(-1) pc. We use the model to calculate the Hubble constant H-0 as a function of the time delay Delta tau(BA) between the two images. We obtain H-0 = (60.5(-2.2)(+5.3))(1 - kappa)(Delta tau(BA)/1.5 yr)(-1) km s(-1) Mpc(-1), or = (82.5(-3.0)(+7.2))(1 - kappa)(Delta tau(BA)/1.1 yr)(-1) km s(-1) Mpc(-1). Once Delta tau(BA) is measured, this will provide an upper bound on H-0 since kappa cannot be negative. In addition, the model degeneracy due to kappa can be eliminated if the one-dimensional velocity dispersion sigma of the lensing galaxy is measured. In this case, we find that H-0 = (60.5(-4.1)(+6.4))(sigma/322 km s(-1))(2)(Delta tau(BA)/1.5 yr)(-1) km s(-1) Mpc(-1), or = (82.5(-5.6)(+8.7))(sigma/322 km s(-1))(2)(deltBA/1.1 yr)(-1) km s(-1) Mpc(-1). We find that these results are virtually unchanged if we include the ellipticity of the lensing galaxy or dumpiness of the lensing cluster. RP Grogin, NA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 64 TC 89 Z9 90 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1996 VL 464 IS 1 BP 92 EP 113 DI 10.1086/177302 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UN840 UT WOS:A1996UN84000009 ER PT J AU Hartmann, DH Narayan, R AF Hartmann, DH Narayan, R TI Are gamma-ray bursts due to rotation-powered high-velocity pulsars in the halo? SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy, halo; gamma rays, bursts; pulsars, general ID NEUTRON-STARS; MAGNETIC-FIELDS; RADIO PULSARS; ORIGIN; ACCRETION; BINARIES; MODELS; MATTER; DECAY AB The BATSE experiment has now observed more than 1100 gamma-ray bursts. The observed angular distribution is isotropic, while the brightness distribution of bursts shows a reduced number of faint events. These observations favor a cosmological burst origin. Alternatively, very extended Galactic halo (EGH) models have been considered. In the latter scenario, the currently favored source of gamma-ray bursts involves high-velocity pulsars ejected from the Galactic disk. To be compatible with the observed isotropy, most models invoke a sampling distance of D similar to 300 kpc, a turn-on delay t(turn-on) similar to 3 x 10(7) yr, and a source life time t(max) similar to 10(9) yr. We consider the global energy requirements of,such models and show that the largest known resource, rotational kinetic energy, is insufficient by orders of magnitude to provide the observed burst rate. More exotic energy sources or differently tuned pulsar models may be able to get around the global energy constraint bur at the cost of becoming contrived. Thus, while extended halo models are not ruled out, our argument places a severe obstacle for such models and we encourage proponents of EGH models to clearly address the issue of energetics. C1 CLEMSON UNIV,DEPT ASTRON,CLEMSON,SC 29634. UNIV CALIF SANTA BARBARA,INST THEORET PHYS,SANTA BARBARA,CA 93106. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Hartmann, DH (reprint author), CLEMSON UNIV,DEPT PHYS,CLEMSON,SC 29634, USA. NR 60 TC 9 Z9 9 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1996 VL 464 IS 1 BP 226 EP 232 DI 10.1086/177314 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UN840 UT WOS:A1996UN84000021 ER PT J AU Hartmann, L Calvet, N Boss, A AF Hartmann, L Calvet, N Boss, A TI Sheet models of protostellar collapse SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars, formation; stars, pre-main-sequence ID YOUNG STELLAR OBJECTS; MOLECULAR CLOUD CORES; T-TAURI STARS; HL-TAURI; DARK CLOUDS; SCATTERING ENVELOPES; ROTATING PROTOSTARS; CIRCUMSTELLAR DISKS; INFRARED-SPECTRA; ACCRETION DISKS AB Recognizing that protostellar clouds are unlikely to be completely spherical, we explore some effects of initial cloud geometry by considering collapse from a sheet initially in hydrostatic equilibrium. A qualitatively different feature of sheet collapse compared with spherical contraction is the development of relatively evacuated cavities in the infalling dusty cloud, which arise because material falls in first along the shortest dimension to the central gravitating mass. Using analytic models of collapse, which reproduce the main features of our previous numerical time-dependent simulations, we perform detailed radiative transfer calculations, which suggest that these collapse cavities can naturally explain the morphological appearance of many reflection nebulae around young stars on small distance scales without requiring initially diverging outflows. Sheet collapse models can simultaneously explain small-scale reflection nebula morphologies and dust envelope emission properties of many young stellar objects more easily than the standard spherical collapse models. The sheet collapse picture suggests that protostars, i.e., young stellar objects still accreting a large fraction of their mass from infalling envelopes, may be optically visible over a substantial range of system inclinations to the line of sight. These results may be especially relevant to cases where fragmentation and collapse has been triggered by an external impulse, such as a shock wave. We show how many properties of the flat-spectrum T Tauri star HL Tau can be interpreted in terms of flattened protostellar cloud collapse and draw some distinctions between the flattened toroids resulting in our calculations and the ''pseudodisk'' of Galli & Shu. C1 UNIV MASSACHUSETTS,FIVE COLL RADIO ASTRON OBSERV,AMHERST,MA 01003. CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,WASHINGTON,DC 20015. RP Hartmann, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 64 TC 62 Z9 62 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1996 VL 464 IS 1 BP 387 EP 403 DI 10.1086/177330 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UN840 UT WOS:A1996UN84000037 ER PT J AU Neale, L Miller, S Tennyson, J AF Neale, L Miller, S Tennyson, J TI Spectroscopic properties of the H-3(+) molecule: A new calculated line list SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared, general; line, identification; molecular data; planets and satellites, general; stars, atmospheres ID H-3+; JUPITER; EMISSION; SPECTRUM; STATES; H2D+ AB A new list of H-3(+) infrared transition frequencies and intensities is presented. This list greatly extends the range of transitions considered to both higher energy and higher rotational states. The 3 x 10(6) transitions are found to significantly affect both the absorption coefficient of H-3(+) and its cooling properties at temperatures above 1000 K. It is hoped these new data will be used for models of cool stars of low metallicity, the giant planets, and other warm bodies composed largely of H-2. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, CAMBRIDGE, MA 02138 USA. RP Neale, L (reprint author), UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, GOWER ST, LONDON WC1E 6BT, ENGLAND. RI Tennyson, Jonathan/I-2222-2012 OI Tennyson, Jonathan/0000-0002-4994-5238 NR 31 TC 136 Z9 136 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1996 VL 464 IS 1 BP 516 EP 520 DI 10.1086/177341 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UN840 UT WOS:A1996UN84000048 ER PT J AU Strelnitski, V Haas, MR Smith, HA Erickson, EF Colgan, SWJ Hollenbach, DJ AF Strelnitski, V Haas, MR Smith, HA Erickson, EF Colgan, SWJ Hollenbach, DJ TI Far-infrared hydrogen lasers in the peculiar star MWC 349A SO SCIENCE LA English DT Article ID RECOMBINATION LINE MASER; MWC-349 AB Far-infrared hydrogen recombination lines H15 alpha (169.4 micrometers), H12 alpha (88.8 micrometers), and H10 alpha (52.5 micrometers) were detected in the peculiar luminous star MWC 349A from the Kuiper Airborne Observatory. Here it is shown that at least H15 alpha is strongly amplified, with the probable amplification factor being greater than or about equal to 10(3) and a brightness temperature that is greater than or about equal to 10(7) kelvin. The other two lines also show signs of amplification, although to a lesser degree. Beyond H10 alpha the amplification apparently vanishes. The newly detected amplified lines fall into the laser wavelength domain. These lasers, as well as the previously detected hydrogen masers, may originate in the photoionized circumstellar disk of MWC 349A and constrain the disk's physics and structure. C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. SEARCH EXTRATERR INTELLIGENCE INST,MT VIEW,CA 94043. RP Strelnitski, V (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560, USA. RI Colgan, Sean/M-4742-2014 NR 41 TC 37 Z9 37 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JUN 7 PY 1996 VL 272 IS 5267 BP 1459 EP 1461 DI 10.1126/science.272.5267.1459 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UP899 UT WOS:A1996UP89900040 PM 8633236 ER PT J AU Cooper, A Rhymer, J James, HF Olson, SL McIntosh, CE Sorenson, MD Fleischer, RC AF Cooper, A Rhymer, J James, HF Olson, SL McIntosh, CE Sorenson, MD Fleischer, RC TI Ancient DNA and island endemics SO NATURE LA English DT Letter C1 CLEMSON UNIV,DEPT BIOL SCI,CLEMSON,SC 29634. SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560. RP Cooper, A (reprint author), SMITHSONIAN INST,NATL ZOOL PK,MOLEC GENET LAB,WASHINGTON,DC 20008, USA. RI Sorenson, Michael/D-8065-2011; Cooper, Alan/E-8171-2012 OI Sorenson, Michael/0000-0001-5375-2917; Cooper, Alan/0000-0002-7738-7851 NR 14 TC 61 Z9 66 U1 1 U2 8 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD JUN 6 PY 1996 VL 381 IS 6582 BP 484 EP 484 DI 10.1038/381484a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UP435 UT WOS:A1996UP43500042 PM 8632821 ER PT J AU RAVENHILL, PL AF RAVENHILL, PL TI 7 STORIES ABOUT MODERN ART IN AFRICA - DELISS,C SO AFRICAN ARTS LA English DT Book Review RP RAVENHILL, PL (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SUM PY 1996 VL 29 IS 3 BP 15 EP & DI 10.2307/3337334 PG 0 WC Art SC Art GA VE118 UT WOS:A1996VE11800003 ER PT J AU THOMPSON, RF SIEBER, R WALKER, RA DRISKELL, DC JANTJES, G AF THOMPSON, RF SIEBER, R WALKER, RA DRISKELL, DC JANTJES, G TI IN MEMORIAM + ADMINISTRATOR AT NATIONAL-MUSEUM-OF-AFRICAN-ART - WILLIAMS,SYLVIA,H. SO AFRICAN ARTS LA English DT Article C1 SMITHSONIAN INST,NATL MUSEUM AFRICAN ART,WASHINGTON,DC 20560. RP THOMPSON, RF (reprint author), YALE UNIV,NEW HAVEN,CT 06520, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SUM PY 1996 VL 29 IS 3 BP 20 EP & PG 0 WC Art SC Art GA VE118 UT WOS:A1996VE11800014 ER PT J AU SIEBER, R AF SIEBER, R TI AFRICA, THE ART OF A CONTINENT SO AFRICAN ARTS LA English DT Art Exhibit Review RP SIEBER, R (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 7 TC 1 Z9 1 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SUM PY 1996 VL 29 IS 3 BP 68 EP & DI 10.2307/3337345 PG 0 WC Art SC Art GA VE118 UT WOS:A1996VE11800020 ER PT J AU RAVENHILL, PL AF RAVENHILL, PL TI NATIONAL-MUSEUM-OF-AFRICAN-ART - NEW ACQUISITIONS SO AFRICAN ARTS LA English DT Article RP RAVENHILL, PL (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SUM PY 1996 VL 29 IS 3 BP 80 EP 84 PG 5 WC Art SC Art GA VE118 UT WOS:A1996VE11800025 ER PT J AU Dobrowolski, JA Traub, WA AF Dobrowolski, JA Traub, WA TI New designs for far-infrared beam splitters SO APPLIED OPTICS LA English DT Article ID OPTICAL-CONSTANTS; SPECTRUM; PARYLENE; FILM AB We explore theoretically the design of multilayer beam splitters for the far-infrared that are based on coated pellicles as well as on solid substrates. The specific design criterion considered is as high a value as possible of the efficiency E = 4RT throughout the 10-140-mu m spectral region. Here R and T are the reflectance and the transmittance of the beam splitter, respectively. In the numerical study the refractive indices of the substrates and coating materials varied between 1.50 and 4.00. To survey the range of designs, we make a number of simplifying assumptions, the significance of which is later investigated. Various potential manufacturing problems are considered. It is shown that the performance of the beam splitters is not sensitive to the accuracy with which the layer thicknesses can be controlled. However, it does depend strongly on the lowest available refractive index of the coating materials. The performance is particularly sensitive to the extinction coefficients of solid substrate materials. Multilayer designs presented should be useful for use in Fourier-transform spectrometers, as well as in other applications that do not require as high a spectral resolution. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Dobrowolski, JA (reprint author), NATL RES COUNCIL CANADA,INST MICROSTRUCT SCI,MONTREAL RD,OTTAWA,ON K1A 0R6,CANADA. NR 40 TC 12 Z9 12 U1 1 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0003-6935 J9 APPL OPTICS JI Appl. Optics PD JUN 1 PY 1996 VL 35 IS 16 BP 2934 EP 2946 DI 10.1364/AO.35.002934 PG 13 WC Optics SC Optics GA UQ482 UT WOS:A1996UQ48200027 PM 21085445 ER PT J AU Johnson, DG Traub, WA Jucks, KW AF Johnson, DG Traub, WA Jucks, KW TI Phase determination from mostly one-sided interferograms SO APPLIED OPTICS LA English DT Article DE Fourier transform spectroscopy; interferometer; phase ID SINGLE-AXIS PLATFORM AB We show how to detect and correct for nonlinear phase shifts in a mainly one-sided interferogram of an emission-line source. We simultaneously detect and correct for an out-of-phase emission background from the spectrometer. The method requires two auxiliary spectra, one of a strong continuum source, and one of an emission-line source with little or no continuum. RP Johnson, DG (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Johnson, David/F-2376-2015 OI Johnson, David/0000-0003-4399-5653 NR 6 TC 5 Z9 5 U1 0 U2 0 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0003-6935 J9 APPL OPTICS JI Appl. Optics PD JUN 1 PY 1996 VL 35 IS 16 BP 2955 EP 2959 DI 10.1364/AO.35.002955 PG 5 WC Optics SC Optics GA UQ482 UT WOS:A1996UQ48200029 PM 21085447 ER PT J AU Loinard, L Allen, RJ Lequeux, J AF Loinard, L Allen, RJ Lequeux, J TI CO emission associated with dust clouds in the inner disk of M 31 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies, individual (M 31); galaxies, ISM; ISM, molecules; radio lines, galaxies ID M31; ULTRAVIOLET; GALAXY AB Allen & Lequeux (1993) have reported the detection of faint CO emission from two dust clouds (D268 and D478, Hodge 1980a) in the inner disk of M 31. During the same observing run, several other positions in the inner disk of M 31 were observed, and we report here the results of these observations. Two dust clouds located less than a few arcminutes from the center were observed; one of them was reported earlier by Sofue & Yoshida (1993) to be a CO(1-0) source. We failed to detect emission in either cloud, although our sensitivity was much better than that of the previous authors. The lack of detection for these clouds indicates that the physical state of the gas associated with the dust very close to the center of M 31 is different from that of the other dust clouds in the inner disk of this galaxy. This difference may be related to the intense UV field present in the nucleus of M 31. Farther from the center, at R less than or equal to 4 kpc (but still inside the bright ring at R similar to 10 kpc), 4 other isolated positions associated with dust clouds were observed. Faint CO(1-0) and CO(2-1) emission was detected for all of them. As a check on the relative calibration of the CO(1-0) line, we observed as a reference position the brightest CO feature in the small region mapped by Casoli, Combes & Stark (1987) in the star-forming ring; here, we find a more common value of 0.63 +/- 0.23 for the line ratio. Finally, several positions on another dust cloud (D192) were observed. This cloud is located in the star-forming ring, but in a region of locally diminished radio-continuum radiation. The CO emission is again quite faint and well associated with the dust itself. The ratio of the integrated CO(2-1) to CO(1-0) line intensities for D192 is 0.50 +/- 0.15, intermediate between the value found for D478 or D268 and those found for our reference position. C1 UNIV GRENOBLE 1, ASTROPHYS LAB, OBSERV GRENOBLE, F-38041 GRENOBLE, FRANCE. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. OBSERV PARIS, DEMIRM, F-75014 PARIS, FRANCE. ECOLE NORMALE SUPER, F-75231 PARIS 05, FRANCE. RP Loinard, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 23 TC 9 Z9 9 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 1996 VL 310 IS 1 BP 93 EP 96 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UP694 UT WOS:A1996UP69400011 ER PT J AU Fiebig, D Duschl, WJ Menten, KM Tscharnuter, WM AF Fiebig, D Duschl, WJ Menten, KM Tscharnuter, WM TI The masing environment of star forming object IRAS 00338+6312: Disk, outflow, or both? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion disks; masers; stars, pre-main sequence; ISM, jets and outflows; radio lines, ISM; stars, individual, IRAS 00338+6312 ID H2O MASER SOURCES; PROPER MOTIONS; MOLECULAR OUTFLOWS; DISTANCES; KINEMATICS; LINE; CO AB We present results of a multi-epoch 0.'' 1 angular resolution study of the 22 GHz H2O maser emission towards the young stellar outflow source IRAS 00338+6312. The overall maser emission consists of about a dozen individual spectral features that form a systematic position-velocity structure indicative of a pattern expected from a protostellar disk. Since it is a priori not clear whether the H2O maser emission originates in a disk or the associated outflow, we consider both possibilities. C1 MAX PLANCK INST RADIOASTRON, D-53121 BONN, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP Fiebig, D (reprint author), UNIV HEIDELBERG, INST THEORET ASTROPHYS, TIERGARTENSTR 15, D-69121 HEIDELBERG, GERMANY. NR 32 TC 34 Z9 34 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 1996 VL 310 IS 1 BP 199 EP 210 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UP694 UT WOS:A1996UP69400022 ER PT J AU Navascues, DBY Stauffer, JR AF Navascues, DBY Stauffer, JR TI Lithium abundance in binaries of the Hyades open cluster SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars, abundances; stars, binaries, close; stars, late type; open clusters, Hyades ID MAIN-SEQUENCE; SPECTROSCOPIC ORBITS; F-STARS; MODEL ATMOSPHERES; DWARFS; AGE; METALLICITY; EVOLUTION; PLEIADES; DISTANCE AB We have derived accurate and homogeneous lithium abundances in 49 Main Sequence binary systems belonging to the Hyades open cluster by using a deconvolution method to determine individual magnitudes and colors for the primary and secondary components of the binary. The input parameters of the model are the observed Li equivalent width, the actual distance to the binary, the integrated apparent magnitude and the integrated colors of the binaries -BV(RI)(K). We show that the general behavior is the same in binaries and in single stars (Li is depleted faster in K stars than in G stars and there is a deep dip for mid-F stars). However, there is a larger scatter in the abundances of binary systems than in single stars. Moreover, in general, binary systems have an overabundance, which is more conspicuous in close binaries. In fact, there is a cut-off period, which can be estimated as P(orb)similar to 9 d. This value is in excellent agreement with the theoretical predition of Zahn (1994). C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. REIAL COLEGIO COMPLUTENSE, CAMBRIDGE, MA 02138 USA. RP Navascues, DBY (reprint author), UNIV COMPLUTENSE MADRID, FAC CIENCIAS FIS, DEPT ASTROFIS, E-28040 MADRID, SPAIN. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 77 TC 43 Z9 43 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 1996 VL 310 IS 3 BP 879 EP 892 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UU581 UT WOS:A1996UU58100021 ER PT J AU Rovero, AC Buckley, JH Fleury, P Jiang, Y Pare, E Sarazin, X Urban, M Weekes, TC AF Rovero, AC Buckley, JH Fleury, P Jiang, Y Pare, E Sarazin, X Urban, M Weekes, TC TI Calibration of the Whipple atmospheric Cerenkov telescope SO ASTROPARTICLE PHYSICS LA English DT Article ID TEV AB Cerenkov ring images from single muons have been used to calibrate the Whipple Observatory 10 m imaging telescope. This approach tests the total throughput of the telescope and uses a known atmospheric Cerenkov light signal that closely matches the spectrum of the atmospheric Cerenkov signal from an air-shower, The absolute calibration is derived by matching the observed ring images with those predicted by a simple geometrical and physical model; a value of 1.25 +/- 0.13 photoelectrons equivalent to 1 digital count was found. Using this value simulations indicate that the telescope had an energy threshold of 300 GeV when this calibration was made. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,AMADO,AZ 85645. ECOLE POLYTECH,LPNHE,F-91128 PALAISEAU,FRANCE. INST HIGH ENERGY PHYS,BEIJING 100039,PEOPLES R CHINA. RP Rovero, AC (reprint author), INST ASTRON & FIS ESPACIO,CC 67,SUC 28,RA-1428 BUENOS AIRES,DF,ARGENTINA. NR 19 TC 7 Z9 7 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD JUN PY 1996 VL 5 IS 1 BP 27 EP 34 DI 10.1016/0927-6505(95)00054-2 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA UR397 UT WOS:A1996UR39700002 ER PT J AU Wu, XP Mao, SD AF Wu, XP Mao, SD TI The cosmological constant and statistical lensing of giant arcs SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology, theory; galaxies, clusters, general; gravitational lensing ID MAGNIFIED GRAVITATIONAL IMAGES; GALAXY REDSHIFT SURVEY; VELOCITY DISPERSION; CLUSTERS; LUMINOSITY; EVOLUTION; LENSES; LIMITS AB Using a singular isothermal sphere model for the matter distribution of foreground clusters of galaxies, we study the statistics of giant arcs in flat cosmologies with and without a cosmological constant. We find that the relative number of arcs predicted within z = 1 in a universe with Omega(0) = 0.3 and lambda(0), Lambda/(3H(0)(2)) = 0.7 is a factor of similar to 2 greater than that predicted in the Einstein-de Sitter universe (Omega(0) = 1, lambda(0) = 0). For a luminosity-dependent evolution model of the number density of background galaxies that accounts for the overdensity of faint blue galaxies at z(s) approximate to 0.4, the Einstein-de Sitter cosmological model predicts that similar to 5% of clusters of galaxies with X-ray luminosity L(X) > 2 x 10(44) ergs s(-1) should have giant arcs, with length-to-width ratio greater than 10. This is a factor of similar to 4 4 lower than the observed fraction in the gravitational-lensing survey of distant X-ray-selected Einstein Extended Medium-Sensitivity Survey clusters of galaxies, indicating a significant deviation of the matter distribution of clusters of galaxies from simple isothermal spheres and/or the presence of a significant cosmological constant. It will be profitable to further study the constraints on the cosmological constant from giant arcs with more realistic cluster models. C1 CHINESE ACAD SCI,BEIJING ASTRON OBSERV,BEIJING 100080,PEOPLES R CHINA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 44 TC 31 Z9 32 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1996 VL 463 IS 2 BP 404 EP 408 DI 10.1086/177256 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UM945 UT WOS:A1996UM94500002 ER PT J AU Urry, CM Sambruna, RM Worrall, DM Kollgaard, RI Feigelson, ED Perlman, ES Stocke, JT AF Urry, CM Sambruna, RM Worrall, DM Kollgaard, RI Feigelson, ED Perlman, ES Stocke, JT TI Soft X-ray properties of a complete sample of radio-selected BL Lacertae objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects, general; radio continuum, galaxies; X-rays, galaxies ID SPECTRAL VARIABILITY; ABSORPTION FEATURE; LAC OBJECTS; 5 GHZ; BLAZARS; EXOSAT; ROSAT; AGN AB We report the soft X-ray properties of the complete 1 Jy sample of 34 radio-selected BL Lacertae objects (RBLs) as measured with the ROSAT Position Sensitive Proportional Counter. The 0.1-2.0 keV spectra of RBLs are generally well described by a single power-law model modified at low energies by absorption in our Galaxy. In a few brighter cases, either a convex or concave spectrum was detected. The distribution of the X-ray photon indices for the RBL sample is quite broad, 1 < Gamma < 3, with a measurable intrinsic dispersion. Comparing the ROSAT spectral index distributions of RBLs and other blazars, we find that RBLs have soft X-ray spectra similar to the X-ray-selected BL Lacertae objects (XBLs) of the EMSS complete sample, and both are steeper than more luminous (and more distant) strong emission-line blazars. Sorting the sources according to the ratio of their radio to X-ray fluxes into low-frequency peaked BL Lacertae objects (LBLs, which are mostly RBLs) and high-frequency peaked BL Lacertae objects (HBLs, which are mostly XBLs), the soft X-ray spectral index distributions for the two classes. are statistically different, with LBLs being flatter than HBLs. The ROSAT spectra of RBLs are steeper than those obtained previously with the Einstein Observatory IPC at slightly higher energies, suggesting that for these objects a flatter (Compton) component emerges at or above similar to 1 keV. The ROSAT data confirm that RBLs are variable X-ray sources, on timescales as short as weeks or even hours. Spectral variability was detected for three of the six sources having more than two pointed observations. Two of these are flatter in the fainter state, in contrast to the trend seen in previous X-ray studies of BL Lac objects (mostly XBLs). C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. PENN STATE UNIV,DEPT ASTRON & ASTROPHYS,UNIVERSITY PK,PA 16802. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,BOULDER,CO 80309. RP Urry, CM (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. RI Urry, Claudia/G-7381-2011; OI Urry, Claudia/0000-0002-0745-9792; Perlman, Eric/0000-0002-3099-1664 NR 79 TC 88 Z9 91 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1996 VL 463 IS 2 BP 424 EP 443 DI 10.1086/177259 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UM945 UT WOS:A1996UM94500005 ER PT J AU Giampapa, MS Rosner, R Kashyap, V Fleming, TA Schmitt, JHMM Bookbinder, JA AF Giampapa, MS Rosner, R Kashyap, V Fleming, TA Schmitt, JHMM Bookbinder, JA TI The coronae of low-mass dwarf stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, coronae; stars, low-mass, brown dwarfs; X-rays, stars ID X-RAY-EMISSION; RS CANUM-VENATICORUM; SOLAR ACTIVE REGIONS; INFRARED PHOTOMETRY; OUTER ATMOSPHERES; MAGNETIC-FIELDS; FLARE STARS; COOL STARS; DM STARS; EINSTEIN AB We report the results of our analysis of pointed X-ray observations of nearby dMe and dM stars using the position sensitive proportional counter (PSPC) on board the ROSAT satellite (Roentgensatellit). In the cases of those M dwarf stars where PSPC pulse-height distributions of sufficient quality for spectral fitting were obtained, we derive key coronal plasma parameters in order to investigate stellar coronal structure in more detail. In particular, we utilize temperatures and emission measures inferred for one or more distinct components as constraints for the development of semiempirical magnetic loop models as representations of the coronae of low-mass stars. The consistency of these static models as adequate descriptions of the coronae of M dwarfs is then examined. We find that the coronae of low-mass dwarfs consist of two distinct thermal components: a ''soft'' component with T similar to 2-4 x 10(6) K and a ''hard'' component with T similar to 10(7) K. We find that the pulse-height spectra are systematically fitted better with ''depleted'' abundances compared to solar; the high-temperature emission component on dMe stars appears to contribute a systematically larger fraction of the total flux than the corresponding component in dM stars; and the high-temperature emission component on dMe stars is responsible for most of the observed variation in the count rate. We have modeled the observed temperature components with hydrostatic coronal loop models, and find that: the low-temperature components can be modeled with loops of small size (l much less than R*) and high pressure (p(0) greater than or similar to p(0.)); and the high-temperature components require solutions with either small filling factors (similar to 0.1), large loops (1 greater than or similar to R*), and high base pressure (p(0) greater than or similar to p(0.)), or very small filling factors (much less than 0.1), small loops (l less than or similar to R*), and very high pressure (p(0) much greater than p(0.)). Based on these observational and model results, we conclude that coronal emission in dMe stars can be interpreted as arising from quiescent active regions (a quiescent, low-temperature component) and compact flaring structures (variable, high-temperature component). Our conclusion that the coronal geometry for low-mass dwarf stars is dominated by a combination of relatively compact, quiescent loop configurations and an unstable flaring component has implications for both stellar dynamo theory and for our understanding of stellar angular momentum evolution. With regard to rotation in late-type stars, which has a direct bearing on dynamo action, we know from observations that the lowest mass stars spin down (via magnetic braking) more slowly than the more nearly solar-type stars. The compact loops we find for the low-temperature component suggests a natural explanation for the observed mass dependence of angular momentum evolution in late-type, main-sequence stars. C1 UNIV CHICAGO, DEPT ASTRON & ASTROPHYS, CHICAGO, IL 60637 USA. UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. MAX PLANCK INST EXTRATERR PHYS, D-37075 GARCHING, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP NATL OPT ASTRON OBSERV, NATL SOLAR OBSERV, POB 26732, TUCSON, AZ 85726 USA. NR 92 TC 95 Z9 95 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1996 VL 463 IS 2 BP 707 EP 725 DI 10.1086/177284 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UM945 UT WOS:A1996UM94500030 ER PT J AU Schachter, JF Remillard, R Saar, SH Favata, F Sciortino, S Barbera, M AF Schachter, JF Remillard, R Saar, SH Favata, F Sciortino, S Barbera, M TI Optical and x-ray characteristics of stars detected in the Einstein Slew Survey SO ASTROPHYSICAL JOURNAL LA English DT Review DE stars, activity; stars, flare; surveys; X-rays, stars ID RS-CANUM-VENATICORUM; LOWER MAIN-SEQUENCE; ACTIVE BINARY-SYSTEMS; ALL-SKY SURVEY; LOW-MASS STARS; CA-II-H; CHROMOSPHERIC ACTIVITY; RADIO-CONTINUUM; K-DWARFS; FK-COMAE AB We detect X-rays for the first time from 63 cool (types A-M) stars. These stars are part of the 229 total stellar X-ray sources identified to date in the Einstein Slew Survey (hereafter Slew). We also list new X-ray data on one A star that may have a corona, five OB stars, and report discoveries of two new T Tauri stars and two new cataclysmic variables. The stellar content of the Slew high-latitude subset (currently 93% identified for \b(II)\ > 20 degrees) is 26%. This agrees well with the Einstein Extended Medium Sensitivity Survey (EMSS) stellar sample, which only considered high latitudes. Because of the large solid angle covered by the Slew, and its shallow limiting flux, the sample will better probe the bright end of the stellar X-ray luminosity function (L(X) > 10(30) ergs s(-1)). Presently (based on the 221 Slew stars with known spectral types), the sample is dominated by late-type systems (cooler than F; 68%). These include dMe's, BY Dra, RS CVn, and FK Comae systems. Based on the limiting magnitudes of catalogs searched to date, the Slew is assessed to be complete for spectral types earlier than K. Hence, K and M systems will be prominent in the similar to 50 as yet unidentified stars. We have embarked on an extensive program to (1) confirm the X-ray identifications with the optical counterparts; (2) search for Ca II H and K and Balmer line emission as activity signatures; and (3) search for supporting evidence of magnetic activity by measuring rotational velocities and relating them to X-ray luminosity level. Of 64 proposed coronal systems observed to date, we have confirmed 44 active stars, while in the remaining 20 we have been unable to find definitive activity. We have confirmed an additional 19 active stars from stellar database searches, and reclassified nine systems as having nonstellar optical counterparts from optical follow-up identification work and extragalactic database searches. We discuss notable new discoveries. From the sample of single active F7-M5 Slew stars with measured upsilon sin i-values, we find a strong (99.9% confidence level) linear correlation of X-ray luminosity with upsilon sin i and with stellar radius (R). However, L(X) is uncorrelated with angular rotation speed at the 99% level, For the combined Slew and EMSS single star F7-M5 sample, we find the same 99.9% upsilon sin i-L(X) and R-L(X) correlations. The L(X)-upsilon sin i relation for the combined sample appears to flatten with respect to the quadratic behavior seen for optically selected stellar samples at rotational velocities in excess of similar to 16 km s(-1). For the s unevolved subset of the Slew single star sample, we also find a correlation between L(X) and Rossby number (R(0); more than 99% confidence). A least-squares fit gives L(X) similar to R(0)(-0.4), which is similarly flatter o than the quadratic dependence seen in optical samples. Using the stellar surface X-ray flux F-X versus B-V diagram, we interpret these results as saturation of the stellar surface by active regions at F-X/F-bol approximate to 10(-3). C1 MIT, SPACE RES CTR, CAMBRIDGE, MA 02139 USA. EUROPEAN SPACE AGCY, DIV ASTROPHYS, 2200 AG NOORDWIJK, NETHERLANDS. IST & OSSERVATORIO ASTRON PALERMO, PALERMO, ITALY. RP Schachter, JF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, HIGH ENERGY ASTROPHYS DIV, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. OI Barbera, Marco/0000-0002-3188-7420 NR 130 TC 28 Z9 28 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1996 VL 463 IS 2 BP 747 EP 765 DI 10.1086/177287 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UM945 UT WOS:A1996UM94500033 ER PT J AU ONeal, D Saar, SH Neff, JE AF ONeal, D Saar, SH Neff, JE TI Measurements of starspot area and temperature on five active, evolved stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, activity; stars, atmospheres; stars, late-type; stars, magnetic fields; techniques, spectroscopic ID BINARY SIGMA-GEMINORUM; II-PEGASI; HD 26337; RS; PHOTOMETRY; SPOT; HD-26337; CYCLE AB We present results from a study of starspot areas and temperatures on active stars using the 7055 and 8860 Angstrom bands of the titanium oxide molecule. Because the two bands have different temperature sensitivities, the ratio of their strengths provides a measure of the spot temperature, while their absolute strengths are a function of total starspot area. We have analyzed the TiO bands of four active, evolved, single-lined spectroscopic binaries (EI Eridani, sigma Geminorum, V1762 Cygni, and II Pegasi) and of the FK Comae star V1794 Cygni. Where possible, we compare our results with contemporaneous photometry, which is used to refine our estimate of the nonspotted photospheric temperature. We find that, over multiple epochs of observation, the spot filling factor ranges from below our detection threshold (approximate to 8%) to just under 60%. In some cases, we find that significant starspot coverage was likely present at historical light maxima. Our results suggest a possible correlation between increasing surface gravity and the temperature difference between the spotted and nonspotted photosphere. This might result from smaller starspot magnetic field strengths on active stars of lower gravity and the corresponding decrease in the pressure and temperature contrast between the photosphere and the umbra. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP ONeal, D (reprint author), PENN STATE UNIV, DEPT ASTRON & ASTROPHYS, 525 DAVEY LAB, UNIVERSITY PK, PA 16802 USA. NR 44 TC 76 Z9 76 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1996 VL 463 IS 2 BP 766 EP 775 DI 10.1086/177288 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UM945 UT WOS:A1996UM94500034 ER PT J AU MoriartySchieven, GH Xie, T Patel, NA AF MoriartySchieven, GH Xie, T Patel, NA TI H I ''tails'' from cometary globules in IC 1396 SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II Regions; ISM, globules; ISM, individual (IC 1396) ID DISSOCIATION; CLOUDS AB IC 1396 is a relatively nearby (750 pc), large (>2 degrees), H II region ionized by a single 06.5 V star and containing bright-rimmed cometary globules. We have made the first arcminute resolution images of atomic hydrogen toward IC 1396, and have found remarkable ''tail''-like structures associated with some of the globules and extending up to 6.5 pc radially away from the central ionizing star. These H I ''tails'' may be material which has been ablated from the globule through ionization and/or photodissociation and then accelerated away from the globule by the stellar wind, but which has since drifted into the ''shadow'' of the globules. This report presents the first results of the Galactic Plane Survey Project recently begun by the Dominion Radio Astrophysical Observatory. C1 UNIV MARYLAND,DEPT ASTRON,LAB MILLIMETERWAVE ASTRON,COLLEGE PK,MD 20742. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MoriartySchieven, GH (reprint author), NATL RES COUNCIL CANADA,DOMINION RADIO ASTROPHYS OBSERV,PENTICTON,BC V2A 6K3,CANADA. NR 20 TC 8 Z9 8 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1996 VL 463 IS 2 BP L105 EP & DI 10.1086/310064 PN 2 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UM946 UT WOS:A1996UM94600015 ER PT J AU Willmer, CNA Koo, DC Ellman, N Kurtz, MJ Szalay, AS AF Willmer, CNA Koo, DC Ellman, N Kurtz, MJ Szalay, AS TI A medium-deep survey of a minislice at the north Galactic Pole .2. The data SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology, observations; galaxies, distances and redshifts; galaxies, photometry; surveys ID CFA REDSHIFT SURVEY; GALAXY SURVEY; PHOTOMETRY; SKY AB We report 328 redshifts, b(J) magnitudes, and b(J) - r(F) colors of galaxies measured in a redshift survey of a 4 degrees x 0 degrees.67 slice close to the north Galactic pole. The faintest galaxies in this survey have a magnitude of b(J) similar to 20.5. The redshifts present external errors of the order of 70 km s(-1), and we estimate that the mean photometry errors are similar to 0.2 for magnitudes and similar to 0.3 for colors. The redshift completeness level of the sample is of the order of similar to 35% at b(J) = 20, and part of this rather low completeness is the result of the combination of limitations imposed by the multifiber system with the clustering of galaxies, and an insufficient number of configurations, At the nominal magnitude limit of the survey, we were able to measure redshifts for similar to 70% of the galaxies we observed. From the correlation between observed properties of the galaxies in this sample, we demonstrate that the mean surface brightness is a major limiting factor in our ability to measure redshifts of faint objects. C1 UNIV CALIF SANTA CRUZ,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. JOHNS HOPKINS UNIV,DEPT PHYS,BALTIMORE,MD 21218. OBSERV NACL,BR-20921030 RIO JANEIRO,BRAZIL. UNIV CALIF SANTA CRUZ,UCO LICK OBSERV,SANTA CRUZ,CA 95064. PRINCETON UNIV OBSERV,PRINCETON,NJ 08544. RP Willmer, CNA (reprint author), INST ASTROPHYS PARIS,CNRS,98 BIS BLVD ARAGO,F-75014 PARIS,FRANCE. RI KURTZ, Michael /B-3890-2009; OI Kurtz, Michael/0000-0002-6949-0090 NR 34 TC 11 Z9 11 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 1996 VL 104 IS 2 BP 199 EP 215 DI 10.1086/192298 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UM568 UT WOS:A1996UM56800003 ER PT J AU Perlman, ES Stocke, JT Schachter, JF Elvis, M Ellingson, E Urry, CM Potter, M Impey, CD Kolchinsky, P AF Perlman, ES Stocke, JT Schachter, JF Elvis, M Ellingson, E Urry, CM Potter, M Impey, CD Kolchinsky, P TI The Einstein slew survey sample of BL Lacertae objects SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE BL Lacertae objects, general; surveys; X-rays, galaxies ID LUMINOSITY FUNCTION; STELLAR OBJECTS; RADIO-SOURCES; CATALOG; CONSTRAINTS; GALAXIES AB We have used an efficient method of finding new BL Lacertae objects in the Einstein Slew Survey suggested by Stocke et al, By exploiting the unique broadband (radio / optical / X-ray) spectra of X-ray-selected BL Lac objects, we have identified 29 new BL Lac objects out of 32 candidates observed, effectively doubling the size of the Slew Survey BL Lac sample, which now includes 62 objects. Six more BL Lac candidates have yet to be observed, and seven blank field radio sources cannot be ruled out as optically faint BL Lac objects, although this is unlikely. The correct classification of one BL Lac candidate remains uncertain, We present finding charts, optical spectroscopy, radio images, and optical polarimetry for these new BL Lac objects, Based upon nearly complete radio imaging and optical spectroscopy observations, we present the northern, high-latitude Slew Survey BL Lac sample, in the area bounded by delta greater than or equal to -40 degrees and \ b(II) \ greater than or equal to 15 degrees and excluding the region within 5 degrees of M31, This sample contains 48 BL Lac objects, five BL Lac candidates, and five blank fields which may contain possible BL Lac candidates, This is considerably larger than any previous complete sample of BL Lac objects. We compare this sample with the X-ray-selected Extended Medium-Sensitivity Survey (EMSS) sample of BL Lac objects as well as the radio-selected 1 Jy sample. C1 UNIV COLORADO, CTR ASTROPHYS & SPACE ASTRON, BOULDER, CO 80309 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NEW MEXICO STATE UNIV, DEPT ASTRON, LAS CRUCES, NM 88003 USA. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. CORNELL UNIV, ITHACA, NY 14846 USA. RI Urry, Claudia/G-7381-2011; OI Urry, Claudia/0000-0002-0745-9792; Perlman, Eric/0000-0002-3099-1664 NR 58 TC 176 Z9 178 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 1996 VL 104 IS 2 BP 251 EP 285 DI 10.1086/192300 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UM568 UT WOS:A1996UM56800005 ER PT J AU Wagner, RH Schug, MD Morton, ES AF Wagner, RH Schug, MD Morton, ES TI Condition dependent control of paternity by female purple martins: Implications for coloniality SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE coloniality; purple martin; Progne subis; cuckoldry; lek ID EXTRA-PAIR COPULATIONS; SPERM COMPETITION; SEXUAL SELECTION; RAZORBILLS; MALES; FERTILIZATIONS; PARASITISM; EVOLUTION; BEHAVIOR; MARKERS AB Proposed causal links between extra-pair copulation (EPC) and colony formation in socially monogamous birds hinge on the question of which sex controls fertilizations. We examined in colonial purple martins Progne subis (1) whether EPCs were forced or accepted by females, and (2) the degree to which apparently receptive females were able to obtain EPCs against their mates' paternity defenses, Paternity analyses of multilocus DNA fingerprinting confirmed previous findings of a marked relationship between age class and extra-pair fertilizations (EPFs), with young males losing paternity of 43% (n = 53) of their putative offspring compared to 4% (n = 85) by old males, All assignable extra-pair offspring were sired by old males, with one male obtaining most EPFs each year, Contrary to the hypothesis that EPCs are forced, EPF frequency within age class did not increase with seasonal increases in the number of males per fertile female. Whereas the male control hypothesis predicted that the male age class that mate-guarded more would be cuckolded less, the reverse was true: young males guarded significantly more intensely. The male age class difference in cuckoldry could not be explained by the possibility that young and inexperienced females (which are usually paired to young males) were more vulnerable to forced copulation because EPFs were unrelated to female age, These findings suggest that females (1) pair with old males and avoid EPCs, or (2) pursue a mixed mating strategy of pairing with young males and accepting EPCs from old males. The receptivity to EPCs by females paired to young males put them in conflict with their mates. Two factors determined the paternity achieved by young males: (1) the relative size of the male to the female, with young males achieving much higher paternity when they were larger than their mates, and (2) the intensity of mate-guarding, Both variables together explained 77% of the variance in paternity and are each aspects of male-female conflict. Given female receptivity to EPCs, mate-guarding can be viewed as male interference with female mating strategies. We conclude that EPCs are rarely or never forced, but the opportunity for females paired to young males to obtain EPCs is relative to the ability of their mates to prevent them from encountering other males, Evidence of mixed mating strategies by females, combined with other features of the martin mating system, is consistent with the female-driven ''hidden lek hypothesis'' of colony formation which predicts that males are drawn to colonies when females seek extrapair copulations. C1 CORNELL UNIV,DEPT GENET & DEV,ITHACA,NY 14853. SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RP Wagner, RH (reprint author), YORK UNIV,DEPT BIOL,4700 KEELE ST,N YORK,ON M3J 1P3,CANADA. NR 43 TC 91 Z9 91 U1 2 U2 32 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD JUN PY 1996 VL 38 IS 6 BP 379 EP 389 DI 10.1007/s002650050255 PG 11 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA UU503 UT WOS:A1996UU50300003 ER PT J AU Louton, J Gelhaus, J Bouchard, R AF Louton, J Gelhaus, J Bouchard, R TI The aquatic macrofauna of water-filled bamboo (Poaceae: Bambusoideae: Guadua) internodes in a Peruvian lowland tropical forest SO BIOTROPICA LA English DT Article DE aquatic insects; bamboo; community ecology; helicopter damselfly; mosquitos; Peru; phytotelmata; tropical ecology ID TREE-HOLES; ECOLOGY; FOOD AB In the lowland tropical forest at Pakitza, Peru, bamboo (Guadua weberbaueri Pilger) internodes with lateral perforations contain a diverse aquatic fauna. We found a community of 29 species dominated by Diptera, primarily mosquitos, and an undescribed helicopter damselfly (Mecistogaster). Although most studies of bamboo concern broken or cut culms filled with rainwater, the water in the live bamboo internodes that we studied was supplied by plant secretions. This results in an aquatic habitat that persists even during the pronounced local dry season. The lateral openings typically consist of closely-spaced rows of parallel slots and are possibly formed by the activities of ovipositing female katydids (Leiobliastes laevis Beier) and secondarily enlarged by various means. Succession in this community was found to follow the steps in development of the lateral opening; with increases in the average number of species and individuals, and percent of the total fauna present, as the opening size increased. We explored patterns of community structure by descriptive statistical analyses and constructed a tentative food web diagram of this simple aquatic ecosystem. Pairwise comparisons of ranked abundances of aquatic insects failed co show correlation, but internodes that contained a predator had higher average simple diversity of mosquito species than chose without, indicating a possible ''Paine effect.'' While species counts and counts of total individuals were not significantly correlated with type of lateral perforation, counts of individuals of all taxa per internode were correlated with size of lateral perforation. Number of mosquito species was signifcantly correlated with volume of water held in the internodes. C1 ACAD NAT SCI PHILADELPHIA, PHILADELPHIA, PA 19103 USA. RP Louton, J (reprint author), SMITHSONIAN INST, NATL MUSEUM NAT HIST, WASHINGTON, DC 20560 USA. NR 53 TC 38 Z9 44 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD JUN PY 1996 VL 28 IS 2 BP 228 EP 242 DI 10.2307/2389077 PG 15 WC Ecology SC Environmental Sciences & Ecology GA UT497 UT WOS:A1996UT49700008 ER PT J AU Lubar, S AF Lubar, S TI The machine in America: A social history of technology - Pursell,C SO BUSINESS HISTORY REVIEW LA English DT Book Review RP Lubar, S (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DIV HIST TECHNOL,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BUSINESS HISTORY REVIEW PI BOSTON PA TEELE HALL 304 HARVARD BUS SCH PUBL SOLDIERS FIELD, BOSTON, MA 02163-0014 SN 0007-6805 J9 BUS HIST REV JI Bus. Hist. Rev. PD SUM PY 1996 VL 70 IS 2 BP 275 EP 277 DI 10.2307/3116889 PG 3 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA VR602 UT WOS:A1996VR60200010 ER PT J AU Wise, MA Cerny, P AF Wise, MA Cerny, P TI The crystal chemistry of the Tapiolite series SO CANADIAN MINERALOGIST LA English DT Article DE tapiolite series; crystal chemistry; order-disorder; tantalum; granitic pegmatite ID ELEMENT GRANITIC PEGMATITES; GEOCHEMISTRY; MINERALOGY; WODGINITE; FENB2O6; IRON AB Ferrotapiolite-manganotapiolite-group minerals [(Fe,Mn)Ta2O6] are formed as accessory phases in rare-element granitic pegmatites exhibiting moderate to high degrees of fractionation. Despite their relative paucity, 94 sets of unit-cell parameters and 194 chemical compositions were compiled to characterize the crystal chemistry of the tapiolite series. X-ray-diffraction studies indicate that the degree of order and compositional variations strongly influence unit-cell dimensions of tapiolite. Natural tapiolite shows wide ranges of structural state. Crystallization of disordered phases at low temperatures is suggested; however, the available data are not unambiguous. Tapiolite chemistry is typically uniform (Fe > Mn, Ta > Nb), and compositional variations are the result of limited, but effective homovalent and heterovalent substitutions: (1) Mn2+Fe-12+; (2) Nb5+Ta-15+; (3) Fe3+(Ti,Sn)Fe-4+(-1)2+(Ta,Nb)(-1)(5+) and (4) (Ti,Sn)(3)(4+)(Fe,Mn)(-1)(2+)(Nb,Ta)(-2)(5+). In association with other Nb,Ta,Sn-bearing minerals, tapiolite shows a distinct preference for Fe2+ and Ta over Mn and Nb. Enrichment in Nb, Ti and Sn appears to be common in tapiolite from moderately fractionated pegmatites, whereas extreme Mn enrichment is typical of highly fractionated pegmatites of the petalite subtype or metasomatic units. C1 UNIV MANITOBA,DEPT GEOL SCI,WINNIPEG,MB R3T 2N2,CANADA. RP Wise, MA (reprint author), SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560, USA. NR 74 TC 25 Z9 26 U1 0 U2 3 PU MINERALOGICAL ASSOC CANADA PI NEPEAN PA CITYVIEW 78087, NEPEAN ON K2G 5W2, CANADA SN 0008-4476 J9 CAN MINERAL JI Can. Mineral. PD JUN PY 1996 VL 34 BP 631 EP 647 PN 3 PG 17 WC Mineralogy SC Mineralogy GA UY791 UT WOS:A1996UY79100012 ER PT J AU Consigliere, S Stanyon, R Koehler, U Agoramoorthy, G Wienberg, J AF Consigliere, S Stanyon, R Koehler, U Agoramoorthy, G Wienberg, J TI Chromosome painting defines genomic rearrangements between red howler monkey subspecies SO CHROMOSOME RESEARCH LA English DT Article DE homologies; New World monkeys; phylogeny; platyrrhini; speciation ID ALOUATTA-BELZEBUL; OWL MONKEY; PLATYRRHINI; EVOLUTION; AOTUS; HYBRIDIZATION; PRIMATES; KARYOTYPES; SENICULUS; SAIMIRI AB We hybridized whole human chromosome-specific DNA libraries to chromosomes of two supposed subspecies of Alouatta seniculus: Alouatta seniculus sara and Alouatta seniculus arctoidea. The number of hybridization signals per haploid set is 42 in A. s. sara and 43 in A, s. arctoidea; the two karyotypes differ by at least 16 chromosomal rearrangements, including numerous translocations. An unusual sex chromosome system is shared by bath taxa. The sex chromosome system results from a Y translocation with a chromosome homologous to parts of human chromosome 3/15 and can be described as X(1)X(2)Y(1)Y(2)/X(1)X(1)X(2)X(2) (male/female). Both red howlers also have microchromosomes, a highly unusual karyological trait not found in other higher primates. These microchromosomes are not hybridized by any human chromosome paint and therefore are probably composed of repetitive DNA. It is well known that New World monkeys have high karyological variability. It is probable that molecular cytogenetic analyses including chromosome painting will permit an accurate reconstruction of the phylogeny of these monkeys and help establish the ancestral karyotype for higher primates. C1 UNIV GENOA,INST PHYS ANTHROPOL,GENOA,ITALY. UNIV MUNICH,INST ANTHROPOL & HUMAN GENET,D-8000 MUNICH,GERMANY. SMITHSONIAN INST,CONSERVAT & RES CTR,WASHINGTON,DC 20560. UNIV CAMBRIDGE,DEPT PATHOL,CAMBRIDGE CB2 1TN,ENGLAND. OI Stanyon, Roscoe/0000-0002-7229-1092 NR 37 TC 56 Z9 57 U1 0 U2 1 PU RAPID SCIENCE PUBLISHERS PI LONDON PA 2-6 BOUNDARY ROW, LONDON, ENGLAND SE1 8NH SN 0967-3849 J9 CHROMOSOME RES JI Chromosome Res. PD JUN PY 1996 VL 4 IS 4 BP 264 EP 270 DI 10.1007/BF02263675 PG 7 WC Biochemistry & Molecular Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Genetics & Heredity GA UX423 UT WOS:A1996UX42300002 PM 8817065 ER PT J AU Coddington, JA Scharff, N AF Coddington, JA Scharff, N TI Problems with ''soft'' polytomies SO CLADISTICS-THE INTERNATIONAL JOURNAL OF THE WILLI HENNIG SOCIETY LA English DT Article ID MISSING ENTRIES; CLADOGRAMS; CHARACTERS; PARSIMONY AB The ''soft'' assumption attributes polytomies to lack of data, not simultaneous cladogenesis (the ''hard'' assumption). Most systematists prefer the first interpretation, but most parsimony programs implicitly use the second. Results can thus be inconsistent with initial assumptions. Under certain circumstances that seem especially typical for large data sets treating higher taxa, it may be valid to eliminate both compatible and incompatible polytomous trees from consideration. Consistent treatment of soft polytomies can reduce the ambiguity of cladistic solutions and improve the resolution, and testability, of phylogenetic hypotheses. (C) 1996 The Willi Hennig Society. C1 ZOOL MUSEUM,DEPT ENTOMOL,DK-2100 COPENHAGEN,DENMARK. RP Coddington, JA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST NHB 105,DEPT ENTOMOL,WASHINGTON,DC 20560, USA. RI Scharff, Nikolaj/A-4787-2013 OI Scharff, Nikolaj/0000-0001-6809-2878 NR 15 TC 22 Z9 22 U1 0 U2 1 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0748-3007 J9 CLADISTICS JI Cladistics-Int. J. Willi Hennig Soc. PD JUN PY 1996 VL 12 IS 2 BP 139 EP 145 PG 7 WC Evolutionary Biology SC Evolutionary Biology GA WG862 UT WOS:A1996WG86200003 ER PT J AU Aiello, A Stockwell, HP AF Aiello, A Stockwell, HP TI The golden-cage weevil, Isorhinus undatus (Champion) (Coleoptera: Curculionidae) SO COLEOPTERISTS BULLETIN LA English DT Article AB Larvae of Isorhinus undatus (Champion) feed externally on young leaves of Pseudobombax septenatum (Jacq.) Dug. (Bombacaceae) and cover themselves with their own excrement. Pupation takes place in the open in a cage-like cocoon secreted by the larva and later eaten by the newly emerged adult. RP Aiello, A (reprint author), SMITHSONIAN TROP RES INST,BOX 2072,BALBOA,ANCON,PANAMA. NR 5 TC 2 Z9 2 U1 0 U2 0 PU COLEOPTERISTS SOC PI NATCHEZ PA P.O. BOX 767, NATCHEZ, MS 39121 SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD JUN PY 1996 VL 50 IS 2 BP 192 EP 194 PG 3 WC Entomology SC Entomology GA UV568 UT WOS:A1996UV56800016 ER PT J AU Winker, K AF Winker, K TI The crumbling infrastructure of biodiversity: The avian example SO CONSERVATION BIOLOGY LA English DT Article ID BIRDS; SPECIMENS; PRINCIPLES; TAXONOMY; SURVIVAL AB The successful conservation of biodiversity depends in part upon an accurate assessment of the diversity to be preserved. This assessment is in the domain of systematics, taxonomy, and general comparative biology. Specimens play a central role in this science, and research collections thus represent the touchstone of biodiversity. The massive job of describing and understanding avian diversity is far from complete, yet the specimen basis for much-needed work is not being added to jour collections; current holdings are inadequate. The dwindling influx of specimens is due primarily to opposition to collecting, which is fueled by (1) focusing conservation at the level of the individual; (2) unfamiliarity with population biology; (3) misunderstanding of scientific research; (4) typological thinking; and (5) misplace morality. Specimen-based avian research has a long and scientifically strong history; and the benefits of this research have been extensive. Our research collection must serve as functional biological libraries. the majority of avian populations can easily withstand the relatively tiny levels of collecting required to keep this science vigorous. Insofar as avian conservation necessarily includes the presentation of a myriad of species comprising the ecosystems upon which birds rely, this problem has broad implications for the conservation of biodiversity. RP Winker, K (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,MSC MRC 534,WASHINGTON,DC 20560, USA. RI Winker, Kevin/M-2042-2014 OI Winker, Kevin/0000-0002-8985-8104 NR 43 TC 39 Z9 45 U1 1 U2 14 PU BLACKWELL SCIENCE INC PI CAMBRIDGE PA 238 MAIN ST, CAMBRIDGE, MA 02142 SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD JUN PY 1996 VL 10 IS 3 BP 703 EP 707 DI 10.1046/j.1523-1739.1996.10030703.x PG 5 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA VA572 UT WOS:A1996VA57200004 ER PT J AU Kraft, NO AF Kraft, NO TI The acquisitions module: Stepchild of the IOLS SO ELECTRONIC LIBRARY LA English DT Article AB The article questions whether integrated online library systems effectively serve all the needs of libraries and encourage the development of each module to its fullest potential. It suggests that the needs of Acquisitions Departments are not, in most cases, being met, and that a devotion to integration might in the long run be counterproductive. C1 SMITHSONIAN INST LIB,CATALOGING DEPT,WASHINGTON,DC. SMITHSONIAN INST LIB,ACQUISIT DEPT,WASHINGTON,DC. NR 16 TC 0 Z9 0 U1 0 U2 0 PU LEARNED INFORMATION LTD PI OXFORD PA WOODSIDE, HINKSEY HILL, OXFORD, ENGLAND OX1 5AU SN 0264-0473 J9 ELECTRON LIBR JI Electron. Libr. PD JUN PY 1996 VL 14 IS 3 BP 211 EP 214 DI 10.1108/eb045469 PG 4 WC Information Science & Library Science SC Information Science & Library Science GA UT498 UT WOS:A1996UT49800004 ER PT J AU Beehler, BM Dumbacher, JP AF Beehler, BM Dumbacher, JP TI More examples of fruiting trees visited predominantly by birds of paradise SO EMU LA English DT Article ID SEED DISPERSAL; COEVOLUTION; PLANTS; CONSTRAINTS; FRUGIVORES; FOREST; SIZE AB Based on observations at Varirata National Park, Papua New Guinea, we document and characterise two Papuan tree species in the mahogany family (Meliaceae) whose fruit were consumed only by birds of paradise (family Paradisaeidae), and a third tree of the nutmeg family (Myristicaceae) whose fruit were predominantly consumed by birds of paradise. These three plant species exhibited differing degrees of forages specificity, with the Raggiana Bird of Paradise Paradisaea raggiana being the numerically dominant forager at all three plants (80% to 97% of all foraging records). All three plants produce structurally protected fruit. By contrast, parallel observations of avian foraging at two foodplants with structurally unprotected fruit documented visitation by diverse frugivore assemblages at selected tree species in a forest in the uplands of the northern watershed of Papua New Guinea, and point to the existence of what may be a specialised plant/frugivore syndrome. C1 CLEMSON UNIV,DEPT BIOL SCI,CLEMSON,SC 29634. RP Beehler, BM (reprint author), SMITHSONIAN INST,DIV BIRDS,MRC 116,WASHINGTON,DC 20560, USA. NR 36 TC 9 Z9 9 U1 2 U2 6 PU ROYAL AUSTRALASIAN ORNITHOL UN PI MOONEE PONDS PA 21 GLADSTONE ST, MOONEE PONDS VICTORIA 3039, AUSTRALIA SN 0158-4197 J9 EMU JI Emu PD JUN PY 1996 VL 96 BP 81 EP 88 PN 2 PG 8 WC Ornithology SC Zoology GA VB207 UT WOS:A1996VB20700002 ER PT J AU Briceno, RD Ramos, D Eberhard, WG AF Briceno, RD Ramos, D Eberhard, WG TI Courtship behavior of male Ceratitis capitata (Diptera: Tephritidae) in captivity SO FLORIDA ENTOMOLOGIST LA English DT Article DE medflies; Ceratitis; courtship; behavior ID MEDITERRANEAN FRUIT-FLIES; MATING-BEHAVIOR AB Video recordings of Ceratitis capitata courtship behavior revealed several hitherto unreported details. The droplet of pheromone at the tip of the male's abdomen during wing vibration was partially or completely retracted during wing buzzing and head reeking. Wing vibration gave way to wing buzzing and head rocking during the last 1-2 sec before the male attempted to mount the female; the male ceased rocking his head during the last 0.3 sec before a mounting attempt. Immediately after landing on the female, the male performed up to three additional types of apparent courtship before achieving intromission. The circumstances in which males attempted to mount females differed ii om these in which males abandoned courtship. the male was closer to the female and the two flies were oriented more directly toward each other. Neither reductions in distance nor more precise orientations appeared to be the immediate cues releasing mounting attempts, however. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP Briceno, RD (reprint author), UNIV COSTA RICA,ESCUELA BIOL,CIUDAD UNIV,SAN JOSE,COSTA RICA. NR 14 TC 32 Z9 33 U1 2 U2 3 PU FLORIDA ENTOMOLOGICAL SOC PI GAINESVILLE PA BOX GAINESVILLE, FL 32604 SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD JUN PY 1996 VL 79 IS 2 BP 130 EP 143 DI 10.2307/3495810 PG 14 WC Entomology SC Entomology GA UV842 UT WOS:A1996UV84200004 ER PT J AU Gribble, RF Stern, RJ Bloomer, SH Stuben, D OHearn, T Newman, S AF Gribble, RF Stern, RJ Bloomer, SH Stuben, D OHearn, T Newman, S TI MORB mantle and subduction components interact to generate basalts in the southern Mariana Trough back-arc basin SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ISLAND-ARC; NORTHERN MARIANA; VOLCANIC-ROCKS; ISOTOPIC COMPOSITION; MARGINAL BASINS; WESTERN PACIFIC; MIDOCEAN RIDGES; PHILIPPINE SEA; ZONE MAGMATISM; TRACE-ELEMENT AB We report the results of the first geochemical and isotopic survey of basaltic glasses dredged along the spreading ridge of the southern Mariana Trough (SMT; 15-17 degrees N). This ridge is divided into two segments that have different axial depths, major and trace element compositions, water contents, and isotopic compositions of Sr, Nd, and Pb. Glasses from the shallower, northern segment (N-SMT; 16-17 degrees N) are OL- and QZ-tholeiites that have compositions consistent with a higher degree of mantle melting relative to that of the OL tholeiites from the southern ridge segment (S-SMT; 15-16 degrees N). The N-SMT glasses are similar to basalts erupted near 18 degrees N in the Mariana Trough that have been the focus of previous studies. The more extensive melting inferred for the N-SMT correlates well with higher abundances of water and relative abundances of large ion lithophile and light Rare Earth elements that indicate involvement of a subduction component. The southern ridge segment is deeper and erupts compositions characteristic of lower degrees of melting; this correlates well with a lower proportion of the subduction component, including a suite that is indistinguishable from MORE. The strong correlation between degree of melting, water contents, and LIL elements indicates that hydrous fluxing as well as adiabatic decompression control melting of MORE-like mantle beneath back-are basins. Details regarding the nature of this hydrous fluxing agent are not known, but it could be water-rich melts related to behind-the-arc volcanoes. These melts may be diverted by the back-are convective regime, to become entrained in the zone of adiabatic upwelling, where they further stimulate melting. C1 OREGON STATE UNIV,DEPT GEOSCI,CORVALLIS,OR 97331. UNIV KARLSRUHE,INST PETROG & GEOCHEM,D-76128 KARLSRUHE,GERMANY. SMITHSONIAN INST,WASHINGTON,DC 20560. CALTECH,DIV GEOL & PLANETARY SCI,PASADENA,CA 91125. RP Gribble, RF (reprint author), UNIV TEXAS,CTR LITHOSPHER STUDIES,POB 830688,RICHARDSON,TX 75083, USA. NR 61 TC 131 Z9 152 U1 0 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 1996 VL 60 IS 12 BP 2153 EP 2166 DI 10.1016/0016-7037(96)00078-6 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA UR780 UT WOS:A1996UR78000007 ER PT J AU Hofmann, DJ Oltmans, SJ Koenig, GL Bodhaine, BA Harris, JM Lathrop, JA Schnell, RC Barnes, J Chin, J Kuniyuki, D Ryan, S Uchida, R Yoshinaga, A Neale, PJ Hayes, DR Goodrich, VR Komhyr, WD Evans, RD Johnson, BJ Quincy, DM Clark, M AF Hofmann, DJ Oltmans, SJ Koenig, GL Bodhaine, BA Harris, JM Lathrop, JA Schnell, RC Barnes, J Chin, J Kuniyuki, D Ryan, S Uchida, R Yoshinaga, A Neale, PJ Hayes, DR Goodrich, VR Komhyr, WD Evans, RD Johnson, BJ Quincy, DM Clark, M TI Record low ozone at Mauna Loa observatory during winter 1994-1995: A consequence of chemical and dynamical synergism? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID STRATOSPHERIC CIRCULATION; ERUPTION; PINATUBO AB During two days in late December 1994, total ozone measured at the Mauna Loa Observatory on the island of Hawaii, dropped below 200 Dobson Units (DU) for the first time since ozone measurements began at this site over 30 years ago. Total ozone values this low have not previously occurred over populated areas except on rare occasions when the edges of the springtime Antarctic ozone hole temporarily pass over the southern tip of Argentina. The monthly total ozone average for January 1995 was 216 DU, about 14 % below the 1964-1981 baseline value. Ultraviolet radiation measured at Mauna Loa on clear days during this period increased inversely with ozone as expected, more than tripling in relative intensity at 295 MI. The normal annual minimum in total ozone occurs in winter at Mauna Loa; however, some winters experience considerably lower values than others. This was the case during the winter of 1994-1995. Although the general decline in global ozone, which began about 1980 and also appears in the Mauna Loa record, may he related to chemical ozone depletion, the unusually low values during some winters at Mauna Loa appear to be related to ozone transport from the tropics, and the timing of phase transitions of the QBO. This analysis provides an accurate method of forecasting low-ozone, high-UV winters in Hawaii. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NOAA,CMDL,MAUNA LOA OBSERV,HILO,HI 96721. UNIV COLORADO,COOPERAT INST RES ENVIRONM SCI,BOULDER,CO 80309. RP Hofmann, DJ (reprint author), NOAA,CLIMATE MONITORING & DIAGNOST LAB,325 BROADWAY,BOULDER,CO 80303, USA. RI Neale, Patrick/A-3683-2012; Evans, Robert/D-4731-2016 OI Evans, Robert/0000-0002-8693-9769 NR 11 TC 9 Z9 9 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 1 PY 1996 VL 23 IS 12 BP 1533 EP 1536 DI 10.1029/96GL00150 PG 4 WC Geosciences, Multidisciplinary SC Geology GA UP857 UT WOS:A1996UP85700021 ER PT J AU Walter, CM Marley, MS Hunten, DM Sprague, AL Wells, WK Dayal, A Hoffmann, WF Sykes, MV Deutsch, LK Fazio, GG Hora, JL AF Walter, CM Marley, MS Hunten, DM Sprague, AL Wells, WK Dayal, A Hoffmann, WF Sykes, MV Deutsch, LK Fazio, GG Hora, JL TI A search for seismic waves from the impact of the SL/9 R fragment SO ICARUS LA English DT Article ID JOVIAN OSCILLATIONS; JUPITER AB Jupiter was observed in the aftermath of its impact with fragment R of Comet Shoemaker-Levy/9 to search for seismic waves excited by the collision, Observations were made in the 7.8 mu m methane emission band with the MIRAC2 camera at the IRTF in an attempt to detect the local perturbation to the equilibrium stratospheric temperature profile induced by the wave. Detection of a jovian seismic wave would provide the tightest constraint to date on interior models of Jupiter, Seismic waves were detected in neither direct images of the planet nor in a composite time-distance diagram which utilizes all of the available imagery. This non-detection allows us to place an upper limit on the energy of the fragment R impact of 1 x 10(28) erg, assuming a seismic wave excitation efficiency of 15%. (C) 1996 Academic Press, Inc. C1 UNIV ARIZONA,LUNAR & PLANETARY LAB,TUCSON,AZ 85721. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. UNIV MASSACHUSETTS,FIVE COLL ASTRON DEPT,AMHERST,MA 01003. SMITHSONIAN ASTROPHYS OBSERV,OPT & INFRARED ASTRON DIV,CAMBRIDGE,MA 02138. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. RP Walter, CM (reprint author), NEW MEXICO STATE UNIV,DEPT ASTRON,DEPT 4500,BOX 30001,LAS CRUCES,NM 88003, USA. RI Marley, Mark/I-4704-2013; OI Hora, Joseph/0000-0002-5599-4650 NR 28 TC 7 Z9 7 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD JUN PY 1996 VL 121 IS 2 BP 341 EP 350 DI 10.1006/icar.1996.0092 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UP571 UT WOS:A1996UP57100012 ER PT J AU Padin, S Woody, DP Stern, JA LeDuc, HG Blundell, R Tong, CYE Pospieszalski, MW AF Padin, S Woody, DP Stern, JA LeDuc, HG Blundell, R Tong, CYE Pospieszalski, MW TI An integrated SIS mixer and HEMT IF amplifier SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article ID RECEIVERS; NOISE AB Design details are given for a 205-270 GHz fixed-tuned SIS receiver in which the SIS mixer and HEMT IF amplifier are integrated into a single compact unit, The mixer and IF amplifier are connected with an inductor which provides the reactive part of the optimum input impedance for the HEMT. This simple coupling circuit gives an IF bandwidth of similar to 4 GHz. The receiver has a DSB noise temperature in the range 35-80K over the 205-270 GHz local oscillator band and 0.5-4.5 GHz IF band. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NATL RADIO ASTRON OBSERV,CHARLOTTESVILLE,VA 22903. RP Padin, S (reprint author), CALTECH,OWENS VALLEY RADIO OBSERV,PASADENA,CA 91125, USA. OI Tong, Edward/0000-0002-7736-4203 NR 10 TC 20 Z9 20 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD JUN PY 1996 VL 44 IS 6 BP 987 EP 990 DI 10.1109/22.506643 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA UQ576 UT WOS:A1996UQ57600030 ER PT J AU Miller, E Ragsdale, BD Ortner, DJ AF Miller, E Ragsdale, BD Ortner, DJ TI Accuracy in dry bone diagnosis: A comment on palaeopathological methods SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE palaeopathology; diagnosis; disease category AB The objectives of palaeopathological research include: (i) diagnosis of specific diseases in archaeological human remains; (ii) analysis of the impact of various diseases in human populations through time and space; and (iii) clarification of evolutionary interactions between humans and disease. Basic to all these objectives is the need for accuracy in diagnosing diseases in archaeological human remains. Tests of diagnostic accuracy made during workshops in dry bone diagnosis held during the annual meetings of the Paleopathology Association (PPA) in 1989, 1990, 1991 and 1992 suggest important limitations that need to be considered in the development of methods in palaeopathology. Although the conditions do not approximate those found in most field or laboratory situations, these tests indicate an overall accuracy of 28.6 per cent for specific disease recognition and 42.9 per cent accuracy for correct recognition of the more general categories of disease. The factors in diagnostic accuracy are complex and include the knowledge and experience of the observer. Another factor is the often substantial morphological overlap between different diseases. In the classificatory system used for the workshops there are seven general categories of disease, each of which has recognizable, although often non-specific, hallmarks in dry bone specimens. A differential diagnosis with these seven general possibilities in mind rather than hundreds of specific diseases can be a powerful tool for the palaeopathologist in providing data that are more comparable between observers. This improvement in classificatory agreement has important methodological implications in the development of a data protocol in palaeopathological research. The identification of general disease category is recommended as part of descriptive and diagnostic reports on palaeopathological specimens. C1 ARIZONA STATE UNIV,TEMPE,AZ 85287. SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ANTHROPOL,WASHINGTON,DC 20560. RP Miller, E (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,OFF REPATRIAT,WASHINGTON,DC 20560, USA. NR 5 TC 22 Z9 22 U1 1 U2 8 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX, ENGLAND PO19 1UD SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD JUN PY 1996 VL 6 IS 3 BP 221 EP 229 DI 10.1002/(SICI)1099-1212(199606)6:3<221::AID-OA267>3.0.CO;2-2 PG 9 WC Anthropology; Archaeology SC Anthropology; Archaeology GA UW640 UT WOS:A1996UW64000001 ER PT J AU Hardesty, V AF Hardesty, V TI Untitled SO JOURNAL OF AMERICAN HISTORY LA English DT Letter RP Hardesty, V (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ORGAN AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47401 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD JUN PY 1996 VL 83 IS 1 BP 307 EP 309 PG 3 WC History SC History GA UT488 UT WOS:A1996UT48800171 ER PT J AU Eberhard, WG Kariko, SJ AF Eberhard, WG Kariko, SJ TI Copulation behavior inside and outside the beetle Macrohaltica jamaicensis (Coleoptera, Chrysomelidae) SO JOURNAL OF ETHOLOGY LA English DT Article ID CRYPTIC FEMALE CHOICE; SPERM REMOVAL; INSECTS; COURTSHIP AB Copulation behavior in Macrohaltica jamaicensis involved a complex, relatively stereotyped series of events both inside and outside the female. Only incomplete sperm transfer occurred in many copulations. Some aspects of male copulatory courtship behavior performed during and following copulation were consistently coordinated with particular stages in sperm transfer. This coordination suggests that copulatory courtship may function to induce critical internal female responses which sometimes do not occur, such as relaxing the bursal muscles to permit deeper penetration, and allowing sperm transfer to occur before the spermatophore is discarded. RP Eberhard, WG (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 12 TC 19 Z9 19 U1 0 U2 6 PU JAPAN ETHOL SOC PI SAKYO PA C/O DEPT ZOOL, FAC SCI KYOTO UNIV, SAKYO KYOTO 606, JAPAN SN 0289-0771 J9 J ETHOL JI J. Ethol. PD JUN PY 1996 VL 14 IS 1 BP 59 EP 72 DI 10.1007/BF02350093 PG 14 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA VA392 UT WOS:A1996VA39200009 ER PT J AU Sakai, K Bilek, AM Oteiza, E Walsworth, RL Balamore, D Jolesz, FA Albert, MS AF Sakai, K Bilek, AM Oteiza, E Walsworth, RL Balamore, D Jolesz, FA Albert, MS TI Temporal dynamics of hyperpolarized Xe-129 resonances in living rats SO JOURNAL OF MAGNETIC RESONANCE SERIES B LA English DT Article ID SPIN-EXCHANGE; GAS C1 HARVARD UNIV,SCH MED,BOSTON,MA 02115. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NASSAU COMMUNITY COLL,DEPT ENGN PHYS & TECHNOL,GARDEN CITY,NY 11530. RP Sakai, K (reprint author), HARVARD UNIV,BRIGHAM & WOMENS HOSP,DEPT RADIOL,221 LONGWOOD AVE,BOSTON,MA 02115, USA. NR 17 TC 87 Z9 89 U1 1 U2 6 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 1064-1866 J9 J MAGN RESON SER B JI J. Magn. Reson. Ser. B PD JUN PY 1996 VL 111 IS 3 BP 300 EP 304 DI 10.1006/jmrb.1996.0098 PG 5 WC Physics, Atomic, Molecular & Chemical SC Physics GA UQ678 UT WOS:A1996UQ67800013 PM 8661297 ER PT J AU Murray, A Mecklenburg, MF Fortunko, CM Green, RE AF Murray, A Mecklenburg, MF Fortunko, CM Green, RE TI Air-coupled ultrasonic system: A new technology for detecting flaws in paintings on wooden panels SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article AB Air-coupled ultrasound, a noncontact, nondestructive testing technique, has detected splits, checks, delaminations, cleavage, and voids in various materials. The system has inspected highly anisotropic and inhomogeneous materials such as wood and wood products, with surfaces layers of gesso, gesso and linen, paper, and wood veneer. Two paintings were tested; one was an oak-cradled panel painting and the other was illustration board mounted on hardboard. The air-coupled ultrasound technique yielded information additional to that provided by visual examination, xeroradiography, and infrared thermography. C1 SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. NATL INST STAND & TECHNOL,DIV MAT RELIABIL,MAT SCI & ENGN LAB,COMPOSITE MAT CHARACTERIZAT GRP,BOULDER,CO 80303. JOHNS HOPKINS UNIV,DEPT MAT SCI & ENGN,BALTIMORE,MD 21218. JOHNS HOPKINS UNIV,CTR NONDESTRUCT EVALUAT,BALTIMORE,MD 21218. RP Murray, A (reprint author), QUEENS UNIV,ART CONSERVAT PROGRAM,CTR EXTENS,KINGSTON,ON K7L 3N6,CANADA. NR 13 TC 8 Z9 8 U1 0 U2 3 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SUM PY 1996 VL 35 IS 2 BP 145 EP 162 DI 10.2307/3179993 PG 18 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA VF436 UT WOS:A1996VF43600005 ER PT J AU Condit, R Hubbell, SP Foster, RB AF Condit, R Hubbell, SP Foster, RB TI Assessing the response of plant functional types to climatic change in tropical forests SO JOURNAL OF VEGETATION SCIENCE LA English DT Article; Proceedings Paper CT GCTE Workshop on Plant Functional Types and Climatic Change CY OCT 26-30, 1994 CL POTSDAM INST CLIMAT IMPACT RES, POTSDAM, GERMANY HO POTSDAM INST CLIMAT IMPACT RES DE demography; growth form; moisture requirement; phenology; tropical tree ID NEOTROPICAL FOREST; RAIN-FORESTS; TREE; GROWTH; STRATEGIES; DIVERSITY; CANOPY; CLASSIFICATION; RECRUITMENT; VEGETATION AB We propose and test a classification of plant functional types for tropical trees based on demography, growth form, phenology, and moisture requirements, using data from a 50-ha forest dynamics plot in Panama. Correlations among demographic variables for individual species - mortality, growth, and the tendency to colonize light gaps - were strong, and a single principal component (PC) accounted for a large fraction of the demographic variability. Most species - shade-tolerants - were clustered at the low end of the PC axis (low growth, low mortality), while the rest were continuously distributed over a wide range. Three demographic guilds could be defined from scores on this axis: we call these pioneer, building phase, and shade-tolerant trees, following earlier terminology. Leaf lifetime correlated negatively with the demographic axis, and there was a weak relationship between demography and moisture-preference: no species with high demographic scores also had high moisture requirements. There was no significant relationship between deciduousness and the demographic axis, but deciduousness was negatively correlated with leaf lifetime and moisture index. Altogether, Il different combinations of demographic variables, deciduousness, moisture needs, and growth form (canopy vs. understory species) were identified. We evaluated how these functional types changed in abun dance between 1982 and 1995. Because of a recent run of dry years and long dry seasons, we predicted that deciduous species, canopy species, pioneers, and drought-tolerant species would be increasing at the expense of their counterparts. Only one aspect of this prediction was borne out: moisture-demanding species declined sharply in abundance relative to drought-tolerant species. Neither deciduousness nor growth form was associated with population change, and pioneer species declined in abundance more often than shade-tolerants. The overall structure of the forest - the density of deciduous, pioneer, and understory species - did not change much, but the decline of the moisture-demanding guild indicates that a change in composition is preceding a structural change. RP Condit, R (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO,AA 34002, USA. NR 54 TC 122 Z9 135 U1 2 U2 29 PU OPULUS PRESS UPPSALA AB PI KNIVSTA PA APELSINVAGEN 47, S 741 00 KNIVSTA, SWEDEN SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD JUN PY 1996 VL 7 IS 3 BP 405 EP 416 DI 10.2307/3236284 PG 12 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA VB056 UT WOS:A1996VB05600012 ER PT J AU Taylor, SK Citino, SB Zdziarski, JM Bush, RM AF Taylor, SK Citino, SB Zdziarski, JM Bush, RM TI Radiographic anatomy and barium sulfate transit time of the gastrointestinal; Tract of the leopard tortoise (Testudo pardalis) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE leopard tortoise; Testudo pardalis; anatomy; transit time; gastrointestinal tract; barium contrast study AB Six adult (three female and three male) leopard tortoises (Testudo pardalis) were studied to document the radiographic anatomy of the gastrointestinal tract and the transit time of barium sulfate. Tortoises were chemically immobilized with succinylcholine and dosed orally with barium contrast suspension. Both dorsoventral and lateral radiographs were taken. The lateral radiographs were extremely difficult to interpret because of the overlapping of the gastrointestinal tract and other soft tissue organs. Complete gastric emptying occurred between 5 and 9 hr after barium administration. Barium entered the small intestine at 0.21 hr and the large intestine between 5 and 8 hr. The contrast material began to exit the colon between 144 and 166 hr. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,WASHINGTON,DC 20008. NR 9 TC 10 Z9 11 U1 0 U2 4 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 1996 VL 27 IS 2 BP 180 EP 186 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA UZ764 UT WOS:A1996UZ76400004 ER PT J AU Swanson, WF Brown, JL Wildt, DE AF Swanson, WF Brown, JL Wildt, DE TI Influence of seasonality on reproductive traits of the male Pallas' cat (Felis manul) and implications for captive management SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Pallas' cat; Felis manul; seasonality; reproduction; captive management ID CLOUDED LEOPARD; DOMESTIC CAT; PITUITARY; HORMONE; TESTOSTERONE; PHYSIOLOGY AB A male Pallas' cat (Felis manul) was housed under natural lighting conditions in an outdoor pen for 20 mo and subjected to bimonthly reproductive evaluations consisting of blood sampling for hormonal analysis, testicular volume and body weight measurement, and electroejaculation. Distinct seasonal reproductive patterns were identified; sperm production and quality in the breeding season (December-April) was significantly higher (P < 0.01) than that in the nonbreeding season (June-October). Testicular volume did not differ(P > 0.05) between seasons, but body weight gain and loss occurred (P < 0.01) 1-2 mo before the breeding and nonbreeding seasons, respectively. Although serum testosterone concentrations were similar (P > 0.05) in both seasons, serum luteinizing hormone (LH) concentrations were greater (P < 0.01) during the breeding season, and sperm concentration, total number of sperm per ejaculate, percentage of morphologically normal sperm, sperm motility, and serum LH concentration were correlated (r = 0.60-0.99; P < 0.05). The male Pallas' cat exhibits a pronounced reproductive seasonality, which has important implications for captive breeding management and genome resource banking. RP Swanson, WF (reprint author), SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630, USA. NR 23 TC 25 Z9 27 U1 0 U2 8 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 1996 VL 27 IS 2 BP 234 EP 240 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA UZ764 UT WOS:A1996UZ76400011 ER PT J AU Murray, S Bush, M Tell, LA AF Murray, S Bush, M Tell, LA TI Medical management of postpartum problems in an Asian elephant (Elephas maximus) cow and calf SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE passive transfer; retained placenta; Asian elephant; Elephas maximus; immunoglobulin ID PROGESTERONE; SECRETION; BEER AB An 18-yr-old female Asian elephant (Elephas maximus) gave birth to a 120-kg female calf following 22 mo of gestation. immediately after parturition, the cow became agitated and aggressive towards the calf Before the keepers were able to safely intervene and remove the calf, the cow stepped on the calf's head and right front leg. Within 30 min, the cow calmed down, allowing the calf's safe reintroduction under close keeper supervision and control. The cow had a retained placenta, poor mammary development, and low milk production. The calf's injuries, in combination with the cow's low milk production, impeded the calf's ability to nurse and gain weight. Within 10 days, the calf lost 10% of its weight. Serum protein electrophoresis indicated failure of passive transfer of maternal immunoglobulin. On day 10, the calf received a transfusion of concentrated immunoglobulin extracted and concentrated from the cow's previously banked plasma. On day 13, the calf developed a urinary tract infection, as diagnosed by white blood cells and bacteria in the urine. Following immunoglobulin administration and antibiotic therapy, clinical signs slowly resolved and the calf gained weight. The cow passed the fetal membranes during parturition, but the placenta was retained. Despite prophylactic systemic antibiotics and vaginal flushing, the cow became depressed and developed a leukocytosis and an anemia. A mucopurulent vaginal discharge and ventral edema were noted on day 3, and milk production was minimal. Because decreased milk production has been reported as a common sequel to retained placenta, efforts were focused on removing the placenta. Intermittent oxytocin therapy on days 2-14 did not result in expulsion of the placenta and produced only transient abdominal contractions and minimal increases in milk letdown. On day 15, 10 mg estradiol cypionate was administered i.m. followed by 200 IU oxytocin i.v. An additional 10 IU oxytocin was administered i.v. on day 16. The friable placenta was palpable within the vaginal vault on day 17. The remaining placenta was removed by gentle traction applied by a modified weighted blood pressure cuff. Once the placenta was removed, the cow's clinical problems slowly resolved and the calf continued to gain weight. C1 UNIV CALIF DAVIS,SCH VET MED,DEPT MED & EPIDEMIOL,DAVIS,CA 95616. RP Murray, S (reprint author), NATL ZOOL PK,CONSERVAT RES CTR,1500 REMOUNT RD,FRONT ROYAL,VA 22630, USA. NR 18 TC 9 Z9 9 U1 0 U2 4 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 1996 VL 27 IS 2 BP 255 EP 258 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA UZ764 UT WOS:A1996UZ76400014 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Theories and documents of contemporary art: A sourcebook of artists' writings - Stiles,K, Selz,P SO LIBRARY JOURNAL LA English DT Book Review RP Kalfatovic, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 1996 VL 121 IS 10 BP 104 EP 104 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA UP802 UT WOS:A1996UP80200057 ER PT J AU Riley, SM AF Riley, SM TI The last time I saw mother - Chai,AJ SO LIBRARY JOURNAL LA English DT Book Review RP Riley, SM (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 1996 VL 121 IS 10 BP 148 EP 148 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA UP802 UT WOS:A1996UP80200187 ER PT J AU Oji, T AF Oji, T TI Is predation intensity reduced with increasing depth? Evidence from the west Atlantic stalked crinoid Endoxocrinus parrae (Gervais) and implications for the Mesozoic marine revolution SO PALEOBIOLOGY LA English DT Article ID COMATULID CRINOIDS; ECHINODERMATA; REGENERATION; EOCENE; ISLAND AB The number of regenerated arms was counted on specimens of two distinct phenotypes of the stalked crinoid Endoxocrinus parrae (Gervais) from a wide bathymetric range in the Caribbean (178-723 m). In one phenotype, the sample was divided into two groups, one from shallower (< 500 m) depths, the other from deeper (greater than or equal to 500 m); in the other phenotype the group divided at 550 m. In both phenotypes, the frequency of regenerated arms is significantly higher in specimens from shallower water than in those from deeper water. If the regenerated arms in Endoxocrinus parrae were the result of sublethal predation, as previously suggested, then predation intensity is higher in shallow water than deep water. These results are consistent with the idea of the late Mesozoic marine revolution-that there has been stronger predation on various invertebrates in shallow-water environments since the late Mesozoic. The stalked crinoids may have been unable to cope with increased predation in shelf environments, and they migrated to offshore environments. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. RI Oji, Tatsuo/A-1840-2009 OI Oji, Tatsuo/0000-0002-1034-1111 NR 32 TC 65 Z9 67 U1 1 U2 7 PU PALEONTOLOGICAL SOC INC PI ITHACA PA 1259 TRUMANSBURG ROAD, ITHACA, NY 14850 SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SUM PY 1996 VL 22 IS 3 BP 339 EP 351 PG 13 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA VK597 UT WOS:A1996VK59700004 ER PT J AU Wagner, PJ AF Wagner, PJ TI Ghost taxa, ancestors, assumptions, and expectations: A reply SO PALEOBIOLOGY LA English DT Article ID CONFIDENCE-INTERVALS; PHYLOGENETIC ESTIMATION; STRATIGRAPHIC RANGES; CHARACTERS; ACCURACY; DIVERSIFICATION; PATTERNS; MODEL RP Wagner, PJ (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,NHB121,WASHINGTON,DC 20506, USA. RI Wagner, Peter/A-5514-2009 OI Wagner, Peter/0000-0002-9083-9787 NR 38 TC 9 Z9 9 U1 0 U2 1 PU PALEONTOLOGICAL SOC INC PI ITHACA PA 1259 TRUMANSBURG ROAD, ITHACA, NY 14850 SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SUM PY 1996 VL 22 IS 3 BP 456 EP 460 PG 5 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA VK597 UT WOS:A1996VK59700012 ER PT J AU Hoston, W You, L AF Hoston, W You, L TI Interference of two condensates SO PHYSICAL REVIEW A LA English DT Article AB We propose an experimental scheme to probe the relative global phase of two condensates and thus demonstrate the spontaneous symmetry breaking of global gauge invariance id Bose-Einstein condensation. A positive measurement would justify the standard view of the condensate wave function as a coherent state when there are interparticle interactions. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. RP Hoston, W (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,MS 14,CAMBRIDGE,MA 02138, USA. NR 21 TC 48 Z9 54 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 1996 VL 53 IS 6 BP 4254 EP 4256 DI 10.1103/PhysRevA.53.4254 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA UR605 UT WOS:A1996UR60500075 ER PT J AU Abraham, ERI McAlexander, WI Gerton, JM Hulet, RG Cote, R Dalgarno, A AF Abraham, ERI McAlexander, WI Gerton, JM Hulet, RG Cote, R Dalgarno, A TI Singlet s-wave scattering lengths of Li-6 and Li-7 SO PHYSICAL REVIEW A LA English DT Article ID FREQUENCY-SHIFT; PHOTOASSOCIATION; ATOMS AB Photoassociation of ultracold lithium atoms into bound vibrational levels of the A (1) Sigma(u)(+) excited state is used to probe the X(1) Sigma(g)(+) ground-state interaction potential of Li-6(2) and Li-7(2). It had been predicted that the s-wave photoassociation signal strength would pass through a minimum as a function of vibrational level for positive s-wave scattering length. We report the observation of this novel effect, and use the location of the minimum to precisely determine the singlet s-wave scattering length for both isotopes. The sensitivity of this technique is demonstrated by distinguishing the minima for collisions involving Li-7 atoms in different hyperfine states. C1 RICE UNIV,RICE QUANTUM INST,HOUSTON,TX 77251. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Abraham, ERI (reprint author), RICE UNIV,DEPT PHYS,HOUSTON,TX 77251, USA. RI Abraham, Eric/B-5729-2011 NR 24 TC 37 Z9 37 U1 1 U2 7 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 1996 VL 53 IS 6 BP R3713 EP R3715 PG 3 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA UR605 UT WOS:A1996UR60500003 ER PT J AU Bao, MQ Starace, AF AF Bao, MQ Starace, AF TI Static-electric-field effects on high harmonic generation SO PHYSICAL REVIEW A LA English DT Article ID MULTIPHOTON IONIZATION; THRESHOLD IONIZATION; RARE-GASES; DETACHMENT; RADIATION; ATOMS AB High harmonic generation in the presence of a static electric field is analyzed theoretically by an extension of the zero-range potential model treatment of Becker et al. [Phys. Rev. A 50, 1540 (1994)]. For H- and a CO2 laser of 5 x 10(10) W/cm(2) intensity, a static electric field of 100 kV/cm is shown to produce a plateau from the 3rd to the 23rd harmonic in which neighboring even and odd harmonics are of comparable intensify. Furthermore, odd harmonics on the plateau are one or more orders of magnitude more intense than in the absence of the static electric field. Dependence of emission rates on laser intensity and results for harmonic generation by Ar are also presented. C1 QUANTUM DEV CORP, CLAYMONT, DE 19703 USA. UNIV NEBRASKA, DEPT PHYS & ASTRON, LINCOLN, NE 68588 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, 60 GARDEN ST MS-14, CAMBRIDGE, MA 02138 USA. NR 32 TC 56 Z9 56 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 1996 VL 53 IS 6 BP R3723 EP R3726 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA UR605 UT WOS:A1996UR60500006 ER PT J AU Ribas-Carbo, M Lennon, AM GonzalezMeler, M Giles, L Siedow, JN AF Ribas-Carbo, M Lennon, AM GonzalezMeler, M Giles, L Siedow, JN TI Effect of light-starvation in the electron partitioning between the cytochrome and alternative pathways in soybean cotyledons SO PLANT PHYSIOLOGY LA English DT Meeting Abstract C1 DUKE UNIV, DEPT BOT, DCMB GRP, DURHAM, NC 27708 USA. UNIV NAVARRA, FAC CIENCIAS, DEPT FISIOL VEGETAL, E-31008 PAMPLONA, SPAIN. SMITHSONIAN ENVIRONM RES CTR, EDGEWATER, MD 21037 USA. DUKE UNIV, DEPT BOT, DURHAM, NC 27708 USA. RI Ribas-Carbo, Miquel/N-1634-2013 OI Ribas-Carbo, Miquel/0000-0002-7337-2089 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC PLANT PHYSIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD JUN PY 1996 VL 111 IS 2 SU S BP 86 EP 86 PG 1 WC Plant Sciences SC Plant Sciences GA UR534 UT WOS:A1996UR53400130 ER PT J AU Small, AM Adey, WH Lutz, SM Reese, EG Roberts, DL AF Small, AM Adey, WH Lutz, SM Reese, EG Roberts, DL TI A macrophyte-based rapid biosurvey of stream water quality: Restoration at the watershed scale SO RESTORATION ECOLOGY LA English DT Article ID CHESAPEAKE BAY; ANOXIA; FISH AB The restoration of chemically degraded rivers, lakes, and estuaries with large watersheds and pollution sources that are primarily diffuse in nature requires the grading of thousands of kilometers of tributary streams. Many population- and community-oriented biomonitoring methods have been developed that avoid the cost limitations of chemical/biomarker/bioassay approaches and the serious limitations of single-factor analysis as related to complex systems. In this study of the coastal plain and piedmont geomorphologic provinces of the Chesapeake Bay watershed, we have demonstrated a set of quantitative measures based on analysis of macrophyte populations that provide statistically significant separation of streams in accordance with their state-issued water quality rating. Macrophytes can be abundant and diverse in lower-order streams, and they demonstrate patterns of community structure and diversity similar to those of other organisms developed for biomonitoring of stream degradation. Unlike organisms previously and extensively used in biomonitoring techniques, however, macrophytes are considerably easier to identify and quantify. In addition, macrophyte techniques provide a range of measures of increasing sensitivity from species numbers at a few sites, to the presence/absence and abundance of indicator species, and, finally, to a diversity analysis based on easily identified species at an extended number of sites. We suggest that the ease of utilization of this methodology will allow repeated surveys of all streams in large water-sheds with the invertebrate, fish and diatom biomonitoring to biomarking and chemical bioassays and finally analytical chemistry, progressively applied to verify and then identify specific pollution sources (''hot spots'') in a more limited number of problem streams. RP Small, AM (reprint author), SMITHSONIAN INST, NMNH, MARINE SYST LAB, WASHINGTON, DC USA. NR 68 TC 7 Z9 9 U1 4 U2 12 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1061-2971 J9 RESTOR ECOL JI Restor. Ecol. PD JUN PY 1996 VL 4 IS 2 BP 124 EP 145 DI 10.1111/j.1526-100X.1996.tb00114.x PG 22 WC Ecology SC Environmental Sciences & Ecology GA UR754 UT WOS:A1996UR75400003 ER PT J AU Lang, MA AF Lang, MA TI Smithsonian's scientific diving program SO SEA TECHNOLOGY LA English DT Editorial Material RP Lang, MA (reprint author), SMITHSONIAN INST,OFF PROVOST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU COMPASS PUBL INC PI ARLINGTON PA SUITE 1000 1117 N 19 ST, ARLINGTON, VA 22209 SN 0093-3651 J9 SEA TECHNOL JI Sea Technol. PD JUN PY 1996 VL 37 IS 6 BP 125 EP 125 PG 1 WC Engineering, Ocean SC Engineering GA UT536 UT WOS:A1996UT53600016 ER PT J AU HEYMAN, IM AF HEYMAN, IM TI SMITHSONIAN PERSPECTIVES + IN ITS EARLY DAYS, THE INSTITUTION FACED THE CIVIL-WAR, A DISASTROUS FIRE AND A VASTLY UNCERTAIN FUTURE SO SMITHSONIAN LA English DT Editorial Material RP HEYMAN, IM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD JUN PY 1996 VL 27 IS 3 BP 14 EP 14 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA UP858 UT WOS:A1996UP85800001 ER PT J AU Quintero, D Cambra, RA AF Quintero, D Cambra, RA TI Timulla centroamericana (Dalla Torre) (Hymenoptera: Mutillidae), a parasitoid of Liris (Hymenoptera: Sphecidae) SO SOUTHWESTERN ENTOMOLOGIST LA English DT Article C1 UNIV PANAMA, PANAMA CITY, PANAMA. RP Quintero, D (reprint author), SMITHSONIAN TROP RES INST, UNIT 0948, APO, AA 34002 USA. NR 14 TC 3 Z9 3 U1 0 U2 0 PU SOUTHWESTERN ENTOMOLOGICAL SOC PI DALLAS PA 17360 COIT RD, DALLAS, TX 75252-6599 USA SN 0147-1724 J9 SOUTHWEST ENTOMOL JI Southw. Entomol. PD JUN PY 1996 VL 21 IS 2 BP 205 EP 207 PG 3 WC Entomology SC Entomology GA UY323 UT WOS:A1996UY32300012 ER PT J AU Steel, MA Cooper, A Penny, D AF Steel, MA Cooper, A Penny, D TI Confidence intervals for the divergence time of two clades SO SYSTEMATIC BIOLOGY LA English DT Article DE aligned sequences; clades; divergence times; molecular clock; phylogeny ID NUCLEOTIDE SUBSTITUTION; EVOLUTIONARY DISTANCE; DNA; SEQUENCES AB We describe a simple method for generating tighter confidence intervals for the date of divergence of two monophyletic groups of taxa. This technique exploits the variation that exists within each of two groups that have evolved separately from a common ancestor. We illustrate the method (plus a technique to test the molecular clock hypothesis) using sequence dissimilarity within the orders of ratites and of tinamous (small birds from South America commonly regarded as the closest relative to ratites). C1 SMITHSONIAN INST, NATL ZOOL PK, WASHINGTON, DC 20008 USA. MASSEY UNIV, SCH BIOL SCI, PALMERSTON NORTH, NEW ZEALAND. RP Steel, MA (reprint author), UNIV CANTERBURY, DEPT MATH & STAT, CHRISTCHURCH 1, NEW ZEALAND. RI Penny, David/E-9410-2011; Cooper, Alan/E-8171-2012 OI Cooper, Alan/0000-0002-7738-7851 NR 23 TC 28 Z9 28 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 EI 1076-836X J9 SYST BIOL JI Syst. Biol. PD JUN PY 1996 VL 45 IS 2 BP 127 EP 134 DI 10.2307/2413610 PG 8 WC Evolutionary Biology SC Evolutionary Biology GA UQ213 UT WOS:A1996UQ21300002 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI INDIANS AT HAMPTON-INSTITUTE, 1877-1923 - LINDSEY,DF SO VIRGINIA MAGAZINE OF HISTORY AND BIOGRAPHY LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU VIRGINIA HISTORICAL SOC PI RICHMOND PA BOX 7311, RICHMOND, VA 23221 SN 0042-6636 J9 VA MAG HIST BIOG JI VA. Mag. Hist. Biogr. PD SUM PY 1996 VL 104 IS 3 BP 412 EP 413 PG 2 WC History SC History GA VG983 UT WOS:A1996VG98300016 ER PT J AU WARD, DC AF WARD, DC TI THE 'INFORMATION' - AMIS,M SO VIRGINIA QUARTERLY REVIEW LA English DT Book Review RP WARD, DC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV VIRGINIA PI CHARLOTTESVILLE PA 1 W RANGE, CHARLOTTESVILLE, VA 22903 SN 0042-675X J9 VA QUART REV JI VA. Q. Rev. PD SUM PY 1996 VL 72 IS 3 BP 561 EP 564 PG 4 WC Literary Reviews SC Literature GA UT544 UT WOS:A1996UT54400141 ER PT J AU Harvey, JW Hill, F Hubbard, RP Kennedy, JR Leibacher, JW Pintar, JA Gilman, PA Noyes, RW Title, AM Toomre, J Ulrich, RK Bhatnagar, A Kennewell, JA Marquette, W Patron, J Saa, O Yasukawa, E AF Harvey, JW Hill, F Hubbard, RP Kennedy, JR Leibacher, JW Pintar, JA Gilman, PA Noyes, RW Title, AM Toomre, J Ulrich, RK Bhatnagar, A Kennewell, JA Marquette, W Patron, J Saa, O Yasukawa, E TI The Global Oscillation Network Group (GONG) project SO SCIENCE LA English DT Article ID SOLAR AB Helioseismology requires nearly continuous observations of the oscillations of the solar surface for long periods of time in order to obtain precise measurements of the sun's normal modes of oscillation. The GONG project acquires velocity images from a network of six identical instruments distributed around the world. The GONG network began full operation in October 1995. It has achieved a duty cycle of 89 percent and reduced the magnitude of spectral artifacts by a factor of 280 in power, compared with single-site observations. The instrumental noise is less than the observed solar background. C1 NATL CTR ATMOSPHER RES,HIGH ALTITUDE OBSERV,BOULDER,CO 80307. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. LOCKHEED SOLAR & ASTROPHYS LAB,PALO ALTO,CA 94304. UNIV COLORADO,JILA,BOULDER,CO 80309. UNIV CALIF LOS ANGELES,DEPT PHYS & ASTRON,LOS ANGELES,CA 90024. PHYS RES LAB,UDAIPUR SOLAR OBSERV,UDAIPUR,INDIA. IPS RADIO & SPACE SERV,LEARMONTH SOLAR OBSERV,EXMOUTH,WA,AUSTRALIA. BIG BEAR SOLAR OBSERV,BIG BEAR CITY,CA 92314. CALTECH,PASADENA,CA 91125. INST ASTROFIS CANARIAS,OBSERV TEIDE,E-38200 LA LAGUNA,TENERIFE,SPAIN. NATL OPT ASTRON OBSERV,CERRO TOLOLO INTER AMER OBSERV,LA SERENA,CHILE. MAUNA LOA SOLAR OBSERV,HILO,HI 96720. RP Harvey, JW (reprint author), NATL OPT ASTRON OBSERV,NATL SOLAR OBSERV,POB 26732,TUCSON,AZ 85726, USA. NR 26 TC 217 Z9 220 U1 0 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAY 31 PY 1996 VL 272 IS 5266 BP 1284 EP 1286 DI 10.1126/science.272.5266.1284 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UN472 UT WOS:A1996UN47200031 ER PT J AU Hill, F Stark, PB Stebbins, RT Anderson, ER Antia, HM Brown, TM Duvall, TL Haber, DA Harvey, JW Hathaway, DH Howe, R Hubbard, RP Jones, HP Kennedy, JR Korzennik, SG Kosovichev, AG Leibacher, JW Libbrecht, KG Pintar, JA Rhodes, EJ Schou, J Thompson, MJ Tomczyk, S Toner, CG Toussaint, R Williams, WE AF Hill, F Stark, PB Stebbins, RT Anderson, ER Antia, HM Brown, TM Duvall, TL Haber, DA Harvey, JW Hathaway, DH Howe, R Hubbard, RP Jones, HP Kennedy, JR Korzennik, SG Kosovichev, AG Leibacher, JW Libbrecht, KG Pintar, JA Rhodes, EJ Schou, J Thompson, MJ Tomczyk, S Toner, CG Toussaint, R Williams, WE TI The solar acoustic spectrum and eigenmode parameters SO SCIENCE LA English DT Article ID FREQUENCIES; OSCILLATIONS; CYCLE AB The Global Oscillation Network Group (GONG) project estimates the frequencies, amplitudes, acid linewidths of more than 250,000 acoustic resonances of the sun from data sets lasting 36 days. The frequency resolution of a single data set is 0.321 microhertz. For frequencies averaged over the azimuthal order m, the median formal error is 0.044 microhertz, and the associated median fractional error is 1.6 x 10(-5). For a 3-year data set, the fractional error is expected to be 3 x 10(-6). The GONG m-averaged frequency measurements differ from other helioseismic data sets by 0.03 to 0.08 microhertz. The differences arise from a combination of systematic errors, random errors, and possible changes in solar structure. C1 UNIV CALIF BERKELEY,DEPT STAT,BERKELEY,CA 94720. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. TATA INST FUNDAMENTAL RES,BOMBAY 400005,MAHARASHTRA,INDIA. NATL CTR ATMOSPHER RES,HIGH ALTITUDE OBSERV,BOULDER,CO 80307. STANFORD UNIV,NASA,GODDARD SPACE FLIGHT CTR,CTR ASTROPHYS & SPACE SCI,STANFORD,CA. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV LONDON QUEEN MARY & WESTFIELD COLL,ASTRON UNIT,LONDON E1 4NS,ENGLAND. NATL OPT ASTRON OBSERV,NASA,GODDARD SPACE FLIGHT CTR,TUCSON,AZ 85726. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CALTECH,PASADENA,CA 91125. UNIV SO CALIF,DEPT PHYS & ASTRON,LOS ANGELES,CA 90089. RP Hill, F (reprint author), NATL OPT ASTRON OBSERV,NATL SOLAR OBSERV,POB 26732,TUCSON,AZ 85726, USA. RI Duvall, Thomas/C-9998-2012; Stebbins, Robin/G-5009-2013; OI Stark, Philip/0000-0002-3771-9604 NR 27 TC 132 Z9 132 U1 0 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAY 31 PY 1996 VL 272 IS 5266 BP 1292 EP 1295 DI 10.1126/science.272.5266.1292 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UN472 UT WOS:A1996UN47200033 ER PT J AU Thompson, MJ Toomre, J Anderson, ER Antia, HM Berthomieu, G Burtonclay, D Chitre, SM ChristensenDalsgaard, J Corbard, T DeRosa, M Genovese, CR Gough, DO Haber, DA Harvey, JW Hill, F Howe, R Korzennik, SG Kosovichev, AG Leibacher, JW Pijpers, FP Provost, J Rhodes, EJ Schou, J Sekii, T Stark, PB Wilson, PR AF Thompson, MJ Toomre, J Anderson, ER Antia, HM Berthomieu, G Burtonclay, D Chitre, SM ChristensenDalsgaard, J Corbard, T DeRosa, M Genovese, CR Gough, DO Haber, DA Harvey, JW Hill, F Howe, R Korzennik, SG Kosovichev, AG Leibacher, JW Pijpers, FP Provost, J Rhodes, EJ Schou, J Sekii, T Stark, PB Wilson, PR TI Differential rotation and dynamics of the solar interior SO SCIENCE LA English DT Review ID STELLAR CONVECTIVE DYNAMOS; ANGULAR-MOMENTUM TRANSPORT; MODE FREQUENCY SPLITTINGS; MAIN-SEQUENCE STARS; MAGNETIC-FIELDS; NUMERICAL SIMULATIONS; LATITUDE DEPENDENCE; INTERNAL-ROTATION; RADIATIVE ZONES; SUNS ROTATION AB Splitting of the sun's global oscillation frequencies by large-scale flows can be used to investigate how rotation varies with radius and latitude within the solar interior. The nearly uninterrupted observations by the Global Oscillation Network Group (GONG) yield oscillation power spectra with high duty cycles and high signal-to-noise ratios. Frequency splittings derived from GONG observations confirm that the variation of rotation rate with latitude seen at the surface carries through much of the convection zone, at the base of which is an adjustment layer leading to latitudinally independent rotation at greater depths. A distinctive shear layer just below the surface is discernible at low to mid-latitudes. C1 UNIV COLORADO, JOINT INST LAB ASTROPHYS, BOULDER, CO 80309 USA. NATL OPT ASTRON OBSERV, NATL SOLAR OBSERV, TUCSON, AZ 85726 USA. TATA INST FUNDAMENTAL RES, BOMBAY 400005, MAHARASHTRA, INDIA. OBSERV COTE AZUR, F-06304 NICE 4, FRANCE. UNIV SYDNEY, SCH MATH, SYDNEY, NSW 2006, AUSTRALIA. AARHUS UNIV, THEORET ASTROPHYS CTR, DK-8000 AARHUS C, DENMARK. CARNEGIE MELLON UNIV, DEPT STAT, PITTSBURGH, PA 15213 USA. UNIV CAMBRIDGE, INST ASTRON, CAMBRIDGE CB3 0HA, ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA USA. STANFORD UNIV, HANSEN EXPT PHYS LAB ANNEX, STANFORD, CA 94305 USA. UNIV SO CALIF, DEPT PHYS & ASTRON, LOS ANGELES, CA 90089 USA. UNIV CALIF BERKELEY, DEPT STAT, BERKELEY, CA 94720 USA. RP UNIV LONDON QUEEN MARY & WESTFIELD COLL, ASTRON UNIT, MILE END RD, LONDON E1 4NS, ENGLAND. RI Pijpers, Frank/A-1734-2009; OI Pijpers, Frank/0000-0001-7572-9435; Stark, Philip/0000-0002-3771-9604 NR 109 TC 278 Z9 279 U1 0 U2 8 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 31 PY 1996 VL 272 IS 5266 BP 1300 EP 1305 DI 10.1126/science.272.5266.1300 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UN472 UT WOS:A1996UN47200035 ER PT J AU Kelson, DD Illingworth, GD Freedman, WF Graham, JA Hill, R Madore, BF Saha, A Stetson, PB Kennicutt, RC Mould, JR Hughes, SM Ferrarese, L Phelps, R Turner, A Cook, KH Ford, H Hoessel, JG Huchra, J AF Kelson, DD Illingworth, GD Freedman, WF Graham, JA Hill, R Madore, BF Saha, A Stetson, PB Kennicutt, RC Mould, JR Hughes, SM Ferrarese, L Phelps, R Turner, A Cook, KH Ford, H Hoessel, JG Huchra, J TI The Extragalactic Distance Scale Key Project .3. The discovery of cepheids and a new distance to M101 using the Hubble Space Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; distance scale; galaxies, distances and redshifts; galaxies, individual (M101) ID FIELD PLANETARY CAMERA; BVRI CCD PHOTOMETRY; NEARBY GALAXIES; MAGELLANIC CLOUDS; CONSTANT; STARS; NGC-2403; STEPS AB We report on the discovery of 29 Cepheid variables in the galaxy M101 using the original Wide Field Camera (WFC) and the new Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope. We observed a field in M101 at 17 independent epochs in V (F555W), five epochs in I (F785LP/F814W), and one epoch in B (F439W), with a time interval baseline of 381 days. We have found Cepheids with periods ranging from 10 to 60 days. The data have been calibrated using WFPC2 observations with zero points derived from omega Cen, Pal 4, and NGC 2419 observations. This calibration has been verified by using the Medium Deep Survey (MDS) WFC photometric zero points, and groundbased secondary standards in V and I. The V calibrations agree to +/-0.06 mag, and the I calibrations agree to +/-0.04 mag. We have constructed V and I period-luminosity (PL) relations and have derived apparent distance moduli based on a distance modulus for the Large Magellanic Cloud (LMC) of 18.50 mag and a reddening of E(B-V) = 0.10 mag to the LMC Cepheids. Period-residual minimization was used to minimize the effects of Malmquist bias on the period-luminosity relation fitting process. Using a Galactic extinction law and the apparent V and I distance moduli, we have found a mean reddening for the M101 sample of E(B-V) = 0.03 mag and a true distance modulus to M101 of 29.34 +/- 0.17 mag, corresponding to a distance of 7.4 +/- 0.6 Mpc. The sources of error have been rigorously tracked through an error budget; systematic and random errors contribute roughly equally to the quoted error. The mean gas-phase metal abundances in the LMC and in the M101 outer field are similar so we expect metallicity effects to be minimal. These Cepheids will be used in conjunction with results from a Key Project search for Cepheids in an inner field, where the metallicity is larger by a factor of 5, to probe the effects of abundance on the Cepheid period-luminosity relation. C1 CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,WASHINGTON,DC 20015. CALTECH,JET PROP LAB,NASA,INFRARED PROC & ANAL CTR,IPAC EXTRAGALACT DATABAS,PASADENA,CA 91125. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. DOMINION ASTROPHYS OBSERV,NATL RES COUNCIL,VICTORIA,BC V8X 4M6,CANADA. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,WESTON,ACT 2611,AUSTRALIA. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0EZ,ENGLAND. LAWRENCE LIVERMORE NATL LAB,LIVERMORE,CA 94550. UNIV WISCONSIN,DEPT ASTRON,MADISON,WI 53706. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Kelson, DD (reprint author), UNIV CALIF SANTA CRUZ,LICK OBSERV,UCO,SANTA CRUZ,CA 95064, USA. NR 66 TC 104 Z9 104 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1996 VL 463 IS 1 BP 26 EP & DI 10.1086/177221 PN 1 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UL339 UT WOS:A1996UL33900004 ER PT J AU Gilliland, RL Dupree, AK AF Gilliland, RL Dupree, AK TI First image of the surface of a star with the Hubble Space Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars, chromospheres; stars, individual (alpha Orionis); supergiants; ultraviolet, stars ID ALPHA-ORIONIS; BETELGEUSE; RESOLUTION AB A direct image of the surface of a star, Betelgeuse (=alpha Ori; M2 Iab), has been obtained with the Faint Object Camera on the Hubble Space Telescope. Images in two similar to 300 Angstrom-wide bands centered at 2550 and 2800 Angstrom cover similar to 10 resolution elements on the stellar disk. The ultraviolet diameter of Betelgeuse of 125 +/- 5 mas at 2500 Angstrom (corresponding to 108 +/- 4 mas, FWHM) is a factor of 2.2 larger than the optical diameter, thus indicating a substantially extended chromosphere in this supergiant. A single bright, unresolved area is present in the southwest quadrant of the disk (P.A. = 235 degrees) in both images, with a peak amplitude of 1.3-1.8 as compared to the surrounding disk and a temperature differential in excess of 200 K. This feature may be the result of magnetic activity, atmospheric convection, or global pulsations and shock structures that heat the chromosphere. Spatially resolved spectroscopy of the Mg II lambda lambda 2795, 2802 doublet with the Goddard High Resolution Spectrograph suggests complicated dynamics, with outflowing material in the chromosphere indicated by the Mg II emission. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Gilliland, RL (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 25 TC 73 Z9 73 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1996 VL 463 IS 1 BP L29 EP & DI 10.1086/310043 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UL341 UT WOS:A1996UL34100008 ER PT J AU Cameron, AGW AF Cameron, AGW TI Supernovae and nucleosynthesis: An investigation of the history of matter, from the big bang to the present - Arnett,D SO NATURE LA English DT Book Review RP Cameron, AGW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD MAY 16 PY 1996 VL 381 IS 6579 BP 204 EP 204 DI 10.1038/381204a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UL249 UT WOS:A1996UL24900039 ER PT J AU Tennyson, J AF Tennyson, J TI A new algorithm for Hamiltonian matrix construction in electron-molecule collision calculations SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID IMPACT EXCITATION AB A method is presented for constructing configuration-interaction (CI) Hamiltonians for electron-molecule collision calculations based on close-coupling expansions. This method utilizes the structure of the wavefunction used in scattering calculations to greatly reduce the computational cost compared to conventional procedures. In particular, CI target configurations are treated only at the prototype configuration state function stage of the calculation. Only then are these prototype configurations expanded over all scattering functions using an improved version of a previous algorithm by Morgan and Tennyson. This new algorithm has been implemented as part of the UK R-matrix codes. Test calculations show that it leads to a large reduction in both the number of integrals and matrix elements which need to be explicitly constructed and evaluated. Use of this new program should allow significantly more sophisticated target wavefunctions to be employed in future scattering calculations. C1 UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, LONDON WC1E 6BT, ENGLAND. RP Tennyson, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Tennyson, Jonathan/I-2222-2012 OI Tennyson, Jonathan/0000-0002-4994-5238 NR 22 TC 68 Z9 68 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAY 14 PY 1996 VL 29 IS 9 BP 1817 EP 1828 DI 10.1088/0953-4075/29/9/024 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA UL611 UT WOS:A1996UL61100024 ER PT J AU Green, PJ Mathur, S AF Green, PJ Mathur, S TI Broad absorption line quasars observed by the ROSAT PSPC SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies, active; quasars, absorption lines; X-rays, galaxies ID ACTIVE GALACTIC NUCLEI; STELLAR OBJECTS; CATALOG; QSOS; EXTINCTION; SPECTRA; SAMPLE AB Recent results from the ROSAT All-Sky Survey have shown that broad absorption line (BAL) QSOs are either highly absorbed or underluminous in the soft X-ray bandpass. Here we extend this work by analyzing all known bona fide BAL QSOs observed within the inner 20' of the ROSAT Position Sensitive Proportional Counter. This sample includes both targeted and serendipitous exposures ranging from 8 to 75 ks. Despite these deep exposures, most of the BAL QSOs are undetected and have unusually weak X-ray emission, as evidenced by large optical-to-X-ray slopes alpha(ox). Large values of alpha(ox) (greater than or similar to 1.8) may prove to be a defining characteristic of BAL QSOs. We predict that samples of QSO candidates with large alpha(ox) will yield a higher percentage of BAL QSOs, particularly at low redshift. As a corollary, X-ray-selected QSO samples should yield fewer BAL QSOs. The optical/UV emission line spectra of BAL and non-BAL QSOs are quite similar, suggesting that their intrinsic spectral energy distributions are similar as well. Absorption thus seems the likely reason for the X-ray-quiet nature of BAL QSOs. To constrain the total absorbing column of the BAL clouds, we compare our measured soft X-ray fluxes or upper limits with those expected from normal radio-quiet QSOs of comparable optical continuum magnitude and redshift. From sensitive X-ray observations, we derive column densities of greater than or similar to 2 x 10(22) Cm-2 for intrinsic cold absorbers of solar metallicity. These new results suggest columns at least an order of magnitude larger than the columns previously estimated from optical/UV spectra alone. RP Green, PJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 45 TC 117 Z9 117 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1996 VL 462 IS 2 BP 637 EP 642 DI 10.1086/177178 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UH187 UT WOS:A1996UH18700006 ER PT J AU NoriegaCrespo, A Garnavich, PM Raga, AC Canto, J Bohm, KH AF NoriegaCrespo, A Garnavich, PM Raga, AC Canto, J Bohm, KH TI HH 110 jet near-infrared imaging: The outflow mixing layer SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared, ISM, lines and bands; ISM, individual (HH 110); ISM, jets and outflows; ISM, molecules; stars, pre-main sequence ID HERBIG-HARO OBJECTS; MOLECULAR OUTFLOWS; EMISSION AB We present near-infrared images of the Herbig-Haro 110 jet centered at the molecular hydrogen lines v = 1-0 (2.121 mu m) and v = 2-1 (2.248 mu m). In young stellar objects these lines are mostly excited by low-velocity shocks and the energy released by turbulent processes. The ratio of these lines provides us with a preliminary diagnostic of the molecular gas excitation. The HH 110 jet was selected for four reasons: (1) it has a complicated optical ''turbulent'' morphology, (2) it is close to a high-density circumstellar environment (a molecular core), (3) it does not have an obvious driving source, and (4) theoretical models suggest that this object corresponds to the early stages of a jet-cloud collision. We find that the molecular hydrogen emission follows the optical H alpha and [S II] emission in a ''straight'' section of the jet (the northern similar to 1'), but it becomes shifted westward and separated from the optical emission afterward. We suggest that these morphological properties of the molecular hydrogen emission are consistent with that of a boundary layer. The 2.248 mu m emission is faint in most condensations, except for the B1, El, I-Il, and P1 knots, where it is dearly detected. The ratio of the 2.121 mu m to the 2.248 mu m lines for these knots ranges from 4.5 to 7.5, which implies excitation temperatures of similar to 2400-3100 K. The brightest condensation, H, however, has a smaller ratio (similar to 1.9) and a higher temperature (similar to 5900 K), which suggests a nonisothermal jet structure. In those cases where the H-2 emission is likely to be due to shocks, the line ratios are small enough to be explained by either C- or J-type shocks. C1 MARIA MITCHELL OBSERV, NANTUCKET, MA 02554 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. UNIV WASHINGTON, DEPT ASTRON, SEATTLE, WA 98195 USA. RP NoriegaCrespo, A (reprint author), CALTECH, CTR INFRARED PROC & ANAL, JPL, PASADENA, CA 91125 USA. NR 30 TC 27 Z9 27 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1996 VL 462 IS 2 BP 804 EP 812 DI 10.1086/177195 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UH187 UT WOS:A1996UH18700023 ER PT J AU Elosegui, P Davis, JL Johansson, JM Shapiro, II AF Elosegui, P Davis, JL Johansson, JM Shapiro, II TI Detection of transient motions with the global positioning system SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID CRUSTAL DEFORMATION MEASUREMENTS; LANDERS EARTHQUAKE SEQUENCE; RESOLUTION AB To assess the capability of Global Positioning System (GPS) phase measurements for the determination of transient velocity, we have made measurements with a GPS antenna on a moving platform. The antenna was translated in the horizontal plane ai a constant velocity of 1 mm h(-1) for a period of somewhat more than 24 hours while GPS data were recorded simultaneously. Other stationary antennas at distances of 10 m to similar to 1000 km were also simultaneously recording GPS data. We calculated an average velocity of the moving antenna by modeling its time-dependent position as a random walk and fitting a straight line to the stochastic estimates. We have found that the accuracy of the resulting velocity estimates is dependent on the observing period and the baseline length. For 24-hour data time spans, rms horizontal velocity errors were less than 0.2 mm h(-1) for all baseline lengths; for similar time spans, rms vertical velocity errors were 0.3-0.9 mm for lengths between 100 and 1000 km, and less than or similar to 0.2 mm for baselines less than or equal to 1000 m. We found it convenient to define a quantity xi, which we term the dynamic resolution, equal to the ratio of the rms velocity variation to the mean velocity. For a random walk process, xi(rw) can be used to calculate the variance per unit time sigma(rw)(2) required by filter-based analysis software. We also investigated the power spectral density (PSD) of our estimates of time-dependent position and found that for the frequency range sampled (0.07-16 mHz), the PSD could be well modeled by nu(alpha), where nu is the frequency and the spectral index alpha depends on the value of xi. For strongly constrained (yet unbiased) estimates (obtained by choosing xi(rw) = 10 and sigma(rw) = 0.05 mm h(-1/2)), the resultant value for alpha is -4, indicating a strong filtering of high-frequency noise. C1 CHALMERS UNIV TECHNOL, ONSALA SPACE OBSERV, S-43900 ONSALA, SWEDEN. RP Elosegui, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, MS 42, CAMBRIDGE, MA 02138 USA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 32 TC 11 Z9 11 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD MAY 10 PY 1996 VL 101 IS B5 BP 11249 EP 11261 DI 10.1029/96JB00327 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA UL090 UT WOS:A1996UL09000008 ER PT J AU Orton, G Ortiz, JL Baines, K Bjoraker, G Carsenty, U Colas, F Dayal, A Deming, D Drossart, P Frappa, E Friedson, J Goguen, J Golisch, W Griep, D Hernandez, C Hoffmann, W Jennings, D Kaminski, C Kuhn, J Laques, P Limaye, S Lin, H Lecacheux, J Martin, T McCabe, G Momary, T Parker, D Puetter, R Ressler, M Reyes, G Sada, P Spencer, J Spitale, J Stewart, S Varsik, J Warell, J Wild, W YanamandraFisher, P Fazio, G Hora, J Deutsch, L AF Orton, G Ortiz, JL Baines, K Bjoraker, G Carsenty, U Colas, F Dayal, A Deming, D Drossart, P Frappa, E Friedson, J Goguen, J Golisch, W Griep, D Hernandez, C Hoffmann, W Jennings, D Kaminski, C Kuhn, J Laques, P Limaye, S Lin, H Lecacheux, J Martin, T McCabe, G Momary, T Parker, D Puetter, R Ressler, M Reyes, G Sada, P Spencer, J Spitale, J Stewart, S Varsik, J Warell, J Wild, W YanamandraFisher, P Fazio, G Hora, J Deutsch, L TI Earth-based observations of the Galileo probe entry site SO SCIENCE LA English DT Article ID JUPITER; ATMOSPHERE AB Earth-based observations of Jupiter indicate that the Galileo probe probably entered Jupiter's atmosphere just inside a region that has less cloud cover and drier conditions than more than 99 percent of the rest of the planet. The visual appearance of the clouds at the site was generally dark at longer wavelengths. The tropospheric and stratospheric temperature fields have a strong longitudinal wave structure that is expected to manifest itself in the vertical temperature profile. C1 INST ASTROFIS ANDALUCIA,CSIC,E-18080 GRANADA,SPAIN. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. DLR,INST PLANETARY EXPLORAT,D-12489 BERLIN,GERMANY. BUR LONGITUDES,F-75015 PARIS,FRANCE. UNIV ARIZONA,STEWART OBSERV,TUCSON,AZ 85721. OBSERV PARIS,DESPA,F-92195 MEUDON,FRANCE. OBSERV MIDI PYRENEES,F-65200 BAGNERES BIGORRE,FRANCE. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. NATL SOLAR OBSERV,SUNSPOT,NM 88349. UNIV WISCONSIN,CTR SPACE SCI & ENGN,MADISON,WI 53706. UNIV CALIF LOS ANGELES,LOS ANGELES,CA 90024. UNIV CALIF SAN DIEGO,CASS,LA JOLLA,CA 92093. LOWELL OBSERV,FLAGSTAFF,AZ 86001. CALTECH,DIV GEOL & PLANETARY SCI,PASADENA,CA 91125. UPPSALA ASTRON OBSERV,S-75120 UPPSALA,SWEDEN. UNIV CHICAGO,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. UNIV MASSACHUSETTS,FIVE COLL RADIO ASTRON OBSERV,AMHERST,MA 01003. RP Orton, G (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. RI Bjoraker, Gordon/D-5032-2012; OI Frappa, Eric/0000-0001-5327-7781; Hora, Joseph/0000-0002-5599-4650; Stewart, Sarah/0000-0001-9606-1593 NR 18 TC 52 Z9 53 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAY 10 PY 1996 VL 272 IS 5263 BP 839 EP 840 DI 10.1126/science.272.5263.839 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UK757 UT WOS:A1996UK75700045 ER PT J AU Li, AS Stoecker, DK Coats, DW Adam, EJ AF Li, AS Stoecker, DK Coats, DW Adam, EJ TI Ingestion of fluorescently labeled and phycoerythrin-containing prey by mixotrophic dinoflagellates SO AQUATIC MICROBIAL ECOLOGY LA English DT Article DE Chesapeake Bay; ciliates; CMFDA-labeled protists; cryptophytes; dinoflagellates; grazing; mixotrophy ID CHESAPEAKE-BAY; PHYTOPLANKTON; BACTERIA; WATERS; MARINE; GREEN AB In order to experimentally investigate feeding by mixotrophic dinoflagellates, we developed protocols for the use of live protistan prey as markers of ingestion. CMFDA (5-chloromethyl-fluorescein diacetate), a vital green fluorescent stain, was used to label cultures of photosynthetic nanoflagellates, a diatom, and an oligotrichous ciliate. Cryptophytes were not readily stained with CMFDA, but phycoerythrin-containing members of this phylum have a distinct yellow-orange fluorescence and thus can be used unstained to demonstrate ingestion. With these complementary techniques, we qualitatively demonstrated feeding by the dinoflagellates Ceratium furca, Gymnodinium sanguineum, Gyrodinium estuariale, Prorocentrum minimum (= mariae-lebouriae) and Peridinium brevipes in natural assemblages from Chesapeake Bay, USA. We also used CMFDA-stained Isochrysis galbana (Prymnesiophyta) and unstained Cryptomonas sp. (Cryptophyta) in laboratory and field studies, respectively, to examine prevalence of feeding by G. estuariale as a function of prey density. However, determination of in situ grazing rates for mixotrophic dinoflagellates proved difficult, as only a small percentage of cells contained labeled food vacuoles following short incubations (less than or equal to 4 h) with stained prey added at tracer concentrations. The use oi CMFDA-stained cells and phycoerythrin-containing prey as markers of ingestion should also be applicable to species-specific feeding studies with other phagotrophic protists and micro-metazoa. The protocols presented here have advantages over the use of fluorescent microspheres or fluorescently labeled heat-killed algae (FLA) for investigating grazing or predation because many micrograzers do not readily ingest, or discriminate against, inert particles. C1 SMITHSONIAN ENVIRONM RES CTR, EDGEWATER, MD 21037 USA. RP Li, AS (reprint author), UNIV MARYLAND, CTR ENVIRONM & ESTUARINE STUDIES, HORN POINT ENVIRONM LAB, CAMBRIDGE, MD 21613 USA. RI stoecker, diane/F-9341-2013 NR 35 TC 105 Z9 114 U1 1 U2 13 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0948-3055 EI 1616-1564 J9 AQUAT MICROB ECOL JI Aquat. Microb. Ecol. PD MAY 9 PY 1996 VL 10 IS 2 BP 139 EP 147 DI 10.3354/ame010139 PG 9 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA UM062 UT WOS:A1996UM06200005 ER PT J AU Wills, MA AF Wills, MA TI Classification of the arthropod Fuxianhuia SO SCIENCE LA English DT Article ID BURGESS SHALE; BRITISH-COLUMBIA; DISPARITY; PHYLOGENY; FOSSILS; ORIGIN; FAUNA RP Wills, MA (reprint author), SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT PALEOBIOL,MRC-121,WASHINGTON,DC 20560, USA. NR 32 TC 11 Z9 12 U1 2 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAY 3 PY 1996 VL 272 IS 5262 BP 746 EP 747 DI 10.1126/science.272.5262.746 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA UJ051 UT WOS:A1996UJ05100059 ER PT J AU Doering, ZD Pekarik, A Bickford, A AF Doering, ZD Pekarik, A Bickford, A TI Science doesn't scare museum-goers SO ACADEME-BULLETIN OF THE AAUP LA English DT Letter RP Doering, ZD (reprint author), SMITHSONIAN INST,INST STUDIES OFF,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSN UNIV PROFESSORS PI WASHINGTON PA SUITE 500 1012 14TH ST, NW, WASHINGTON, DC 20005 SN 0190-2946 J9 ACADEME JI Academe-Bull. AAUP PD MAY-JUN PY 1996 VL 82 IS 3 BP 3 EP 4 PG 2 WC Education & Educational Research SC Education & Educational Research GA UM648 UT WOS:A1996UM64800002 ER PT J AU Thorne, BL Haverty, MI Collins, MS AF Thorne, BL Haverty, MI Collins, MS TI Antillean termite named for a locality in Central America: Taxonomic memorial to a perpetuated error SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Nasutitermes acajutlae; Nasutitermes nigriceps; Isoptera; Termitidae; Nasutitermitinae AB The syntype series of the Antillean termite Nasutitermes acajutlae (Holmgren) (Isoptera: Termitidae; Nasutitermitinae) is reexamined. We discovered that one of the specimens, collected from Acajutla, San Salvador, did not come from the island of San Salvador in the Bahamas, as had been assumed since its description in 1910. Instead, it was collected from a locality near the capital of the Central American country of El Salvador. That specimen can now be identified as N. nigriceps (Haldeman). We designate the soldier from the St. Thomas, Virgin Island, syntype series as the lectotype for the species N. acajutlae. C1 US FOREST SERV,PACIFIC SW RES STN,USDA,BERKELEY,CA 94701. SMITHSONIAN INST,MUSEUM SUPPORT CTR,SUITLAND,MD 20746. RP Thorne, BL (reprint author), UNIV MARYLAND,DEPT ENTOMOL,COLLEGE PK,MD 20742, USA. NR 9 TC 3 Z9 3 U1 0 U2 1 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD MAY PY 1996 VL 89 IS 3 BP 346 EP 347 PG 2 WC Entomology SC Entomology GA UP235 UT WOS:A1996UP23500005 ER PT J AU Carilli, CL Lane, W deBruyn, AG Braun, R Miley, GK AF Carilli, CL Lane, W deBruyn, AG Braun, R Miley, GK TI Redshifted H I 21 cm line observations of damped LY alpha absorption systems SO ASTRONOMICAL JOURNAL LA English DT Article ID CENTIMETER ABSORPTION; NEUTRAL HYDROGEN; EMISSION; GALAXIES; GAS; ABSORBERS; SPECTRUM; Z=2.04; SEARCH AB We have used the Westerbork Synthesis Radio Telescope to search for HI 21 cm absorption associated with high redshift damped Ly alpha systems. We calculate limits to harmonic mean spin temperatures, [T-s], for these systems, and find typical lower limits approximate to 10(3) K, consistent with previous results for other damped Ly alpha systems. We then analyze the relationship between the total HI column density and the integrated 21 cm absorption line equivalent width, EW(21), for damped Ly alpha systems. We compare these results with similar results for lines of sight through our own galaxy. A trend is seen in which the damped Ly alpha systems show systematically lower EW(21) values at a given total N(HI) than Galactic lines of sight, by a factor approximate to 3-5. In the context of a two-temperature-phase model for the absorbing gas, these results suggest that for a given total neutral hydrogen column density, the damped Ly alpha systems contain a larger percentage of warm gas than is seen in typical Galactic lines of sight. We derive upper limits to H I 21 cm emission from the vicinity of the damped Ly alpha absorbers. The mass limits are adequate to ruleout a substantial contribution by protoclusters of the type hypothesized by Oort [A&A, 139, 211 (1984)] to the observed statistics of damped Ly alpha systems at high redshift. Lastly, we derive a lower limit to the molecular hydrogen fraction in the cold gas phase for the absorption system towards 0528-2505 of: F = 2N(H-2)/N(HI)>2%. (C) 1996 American Astronomical Society. C1 LEIDEN OBSERV, 2300 RA LEIDEN, NETHERLANDS. RICE UNIV, DEPT PHYS, HOUSTON, TX 77005 USA. NETHERLANDS FDN RES ASTRON, 7990 AA DWINGELOO, NETHERLANDS. RP Carilli, CL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 48 TC 57 Z9 57 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1996 VL 111 IS 5 BP 1830 EP 1838 DI 10.1086/117921 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG899 UT WOS:A1996UG89900006 ER PT J AU Perlman, ES Carilli, CL Stocke, JT Conway, J AF Perlman, ES Carilli, CL Stocke, JT Conway, J TI Multifrequency VLBI observations of PKS 1413+135: A very young radio galaxy SO ASTRONOMICAL JOURNAL LA English DT Article ID VLA OBSERVATIONS; SPECTRUM; NGC-1068; GHZ; PKS-1413+135; ABSORPTION; EMISSION; HYDROGEN; OBJECTS AB We present high-dynamic range VLBA maps of the radio galaxy/BL Lac object PKS 1413+135 at 3.6, 6, 13, and 18 cm. These observations reveal that PKS 1413+135 possesses complex, two-sided parsec-scale structure, similar to that of other compact symmetric objects (CSOs). Its morphology appears to be that of a miniature wide-angle-tail (WAT) radio source, and its total power is at the upper extreme of that seen in WATs. Comparison of these maps with previous data reveals no evidence for superluminal motion, and supports the hypothesis that the milliarcsecond-scale structure of PKS 1413+135, unlike most BL Lacs and flat radio spectrum quasars, is not a product of relativistic beaming. However, beaming is likely present within the core seen at 3.6 cm, due to its high brightness temperature. These new VLBA maps allow a more precise, but not completely unambiguous, interpretation of the various absorption data, suggesting that the A(v)>30 mag is due to a normal molecular cloud complex in the disk of the optical spiral galaxy at z=0.247, greater than or similar to few kpc away from its nucleus. The absence of scatter broadening of the core source at 1.6 and 2.3 GHz and the lack of multiple images add to the evidence against the hypothesis (originally suggested by Stocke et al.) that PKS 1413+135 is background to the spiral galaxy at z=0.247, in which the AGN appears centered. But if the AGN is within the spiral, the absence of reprocessed radiation (e.g., near-IR dust continuum and emission lines) remains difficult to understand, since the very high extinction is unlikely to cover the entire dust and line emitting regions. Whether within or background to the optical galaxy, PKS 1413+135 is similar to other CSOs in being a young radio source (of age less than or similar to 10(4) yr), with evidence for absorption along our line of sight. (C) 1996 American Astronomical Society. C1 SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. UNIV COLORADO, CTR ASTROPHYS & SPACE ASTRON, BOULDER, CO 80309 USA. ONSALA SPACE OBSERV, S-43992 ONSALA, SWEDEN. RP Perlman, ES (reprint author), NASA, GODDARD SPACE FLIGHT CTR, LHEA, USRA, MAIL CODE 660 2, GREENBELT, MD 20771 USA. NR 69 TC 36 Z9 36 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1996 VL 111 IS 5 BP 1839 EP 1851 DI 10.1086/117922 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG899 UT WOS:A1996UG89900007 ER PT J AU Lada, CJ Alves, J Lada, EA AF Lada, CJ Alves, J Lada, EA TI Near-infrared imaging of embedded clusters: NGC 1333 SO ASTRONOMICAL JOURNAL LA English DT Article ID YOUNG STELLAR OBJECTS; HERBIG-HARO OBJECTS; OB1 MOLECULAR CLOUD; IRAS OBSERVATIONS; DARK CLOUDS; NGC-1333; IMAGES; EXTINCTION; PHOTOMETRY; STARS AB We present the results of an extensive near-infrared (JHK) imaging survey of the NGC 1333 star forming region. Our survey covers an area more than 4 times larger than the previous imaging survey of this cloud reported by Aspin et al. [A&AS, 106, 165 (1994)] and is sufficiently sensitive to render an accurate census of the embedded stellar population in the cloud. We detected 275 sources with m(K) < 14.5 magnitudes within the 432 square arcminute region surveyed. The spatial distribution of these sources is found to be significantly clustered with approximately 45% of the sources contained within two adjacent stellar clusters which together occupy an area less than 16% of the entire region surveyed. From comparison with observations of nearby control fields we estimate that roughly 143 of the sources detected over the entire region are physically associated with or embedded in the NGC 1333 molecular cloud. The majority (94 or 66%) of these are also found within the boundaries of the double cluster. From analysis of the JHK colors of the stars in the NGC 1333 region we find that roughly 30% of all sources display detectable infrared excess. This corresponds to more than 50% of all the sources embedded in the cloud. The infrared-excess sources display a higher degree of clustering than the general K band source population with roughly 75% of all excess sources located within the boundaries of the double cluster. Moreover, infrared excess sources comprise roughly 60% of the sources within the cluster suggesting that it is extremely young (less than or equal to 1-2 x 10(6) years). We also find that the stars in the cluster suffer from significant amounts of differential extinction indicating that the cluster is deeply embedded in molecular material. We construct the K luminosity function (KLF) for the NGC 1333 cloud and compare it to that of the control fields off the cloud. We find that background field stars dominate the KLF at faint magnitudes and that the vast majority of stars associated with the cloud are brighter than our completeness limit. We use the infrared colors to de-redden the stars in the cluster and construct their (de-reddened) K luminosity function. The resulting KLF of the NGC 1333 cluster is compared to the KLFs of the Trapezium cluster in Orion and IC 348, a rich young cluster located within the same GMC complex as NGC 1333. The KLFs of NGC 1333 and the Trapezium cluster are found to be very similar in shape and extent while the KLFs of NGC 1333 and IC 348 are found to differ. We attribute this to the effects of luminosity evolution in these young clusters and suggest that the NGC 1333 cluster is similar in age to the Trapezium cluster (i.e., less than or equal to 10(6) years) and significantly younger than IC 348 (i.e., <5-7X10(6) years). This is consistent with both the large population of excess sources and outflow sources [Hodapp & Ladd (ApJ, 1995) (in Press)] contained in the NGC 1333 cluster. However, we derive a star formation rate of 4 x 10(-5) M. yr(-1) for NGC 1333 which is essentially the same as that characterizing IC 348 and nearly an order of magnitude lower than that found for the Trapezium cluster. The two most active star forming regions in the Perseus cloud complex have now been throughly surveyed with comparable sensitivities at near-infrared wavelengths. Both regions have produced embedded stellar clusters, which are forming stars at a similar rate, but which appear to be in very different stages of evolution. (C) 1996 American Astronomical Society. C1 UNIV MARYLAND, DEPT ASTRON, COLLEGE PK, MD 20742 USA. RP Lada, CJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 54 TC 146 Z9 146 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1996 VL 111 IS 5 BP 1964 EP + DI 10.1086/117933 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG899 UT WOS:A1996UG89900018 ER PT J AU Schlegel, EM Kirshner, RP Huchra, JP Schild, RE AF Schlegel, EM Kirshner, RP Huchra, JP Schild, RE TI The peculiar type II SN1987B in NGC 5850 SO ASTRONOMICAL JOURNAL LA English DT Article ID IB SUPERNOVAE; LIGHT CURVES; OPTICAL-SPECTRA; RADIO-EMISSION; SN-1986J; NGC-891; NGC-991; HELIUM; 1987A; STARS AB Nine photometric and five spectroscopic observations of the peculiar Type II supernova SN1987B in NGC 5850 are presented. The light curve is different from any of the typical supernova light curves. The light curve falls as slowly as a Type IIP light curve for similar to 50 days, then steepens considerably, in contrast to the spectroscopically similar object SN1988Z. Both SN1987B and SN1988Z have been considered as representative of ''Type IIn'' supernovae, those supernovae that show circumstellar signatures in their spectra. The spectra of SN1987B show weak hydrogen emission lines with a narrow core (FWZI similar to 1000 km s(-1)) and weak, low-contrast emission lines of hydrogen with a FWZI of similar to 8000 km s(-1). Both photometric and spectroscopic evidence suggests SN1987B had a low-mass envelope. (C) 1996 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Schlegel, EM (reprint author), NASA,GODDARD SPACE FLIGHT CTR,CODE 668,GREENBELT,MD 20771, USA. NR 54 TC 10 Z9 10 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1996 VL 111 IS 5 BP 2038 EP 2046 DI 10.1086/117939 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG899 UT WOS:A1996UG89900024 ER PT J AU Dobrzycka, D Kenyon, SJ Proga, D Mikolajewska, J Wade, RA AF Dobrzycka, D Kenyon, SJ Proga, D Mikolajewska, J Wade, RA TI The hot component of RS Ophiuchi SO ASTRONOMICAL JOURNAL LA English DT Article ID T-CORONAE BOREALIS; SECONDARY OUTBURST MAXIMUM; EMISSION-LINE SPECTRUM; SYMBIOTIC STARS; RECURRENT NOVAE; INHOMOGENEOUS-MEDIUM; COOL COMPONENTS; INFRARED PHOTOMETRY; ANGULAR-MOMENTUM; ACCRETION DISK AB We analyze optical and ultraviolet spectrophotometry of the quiescent recurrent nova RS Ophiuchi, Our preferred model for this binary consists of an M-type giant and a B-type shell star with a luminosity of L(h) similar to 100-600 L.. The ejecta from the recent outburst are slightly enhanced in helium relative to the solar abundance, which agrees with previous estimates from model fits to the optical and ultraviolet light curve. These results indicate that the hot component has a mass close to the Chandrasekhar limit. Although the hot component luminosity is consistent with the high accretion rate needed for recurrent nova eruptions in this system, our effective temperature estimate is not consistent with predicted cooling curves for massive white dwarfs. (C) 1996 American Astronomical Society. C1 COPERNICUS ASTRON CTR,PL-00716 WARSAW,POLAND. PENN STATE UNIV,DEPT ASTRON & ASTROPHYS,DAVEY LAB 525,UNIVERSITY PK,PA 16802. RP Dobrzycka, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 95 TC 33 Z9 33 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1996 VL 111 IS 5 BP 2090 EP 2098 DI 10.1086/117945 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG899 UT WOS:A1996UG89900030 ER PT J AU Evans, NR Teays, TJ Taylor, LL Lester, JB Hindsley, RB AF Evans, NR Teays, TJ Taylor, LL Lester, JB Hindsley, RB TI The temperature of the supergiant alpha Per SO ASTRONOMICAL JOURNAL LA English DT Article ID ENERGY-DISTRIBUTIONS; PHOTOMETRIC SYSTEMS; ANGULAR DIAMETERS; MODEL ATMOSPHERES; F-SUPERGIANTS; OPEN CLUSTERS; STARS; CALIBRATION; SCALE; COLORS AB Because the bright supergiant alpha Per is located in cluster, and because its angular diameter has been measured, its log g is known observationally, as is its atmospheric microturbulence. Using these observed parameters, we compare its energy distribution derived from IUE spectra and B, V, R, I, J, and K with model atmospheres convolved with instrumental sensitivity functions. The two most important advances in this study as compared with previous work are the use of well-calibrated ultraviolet fluxes and the use of models with an appropriate microturbulence. Because the ultraviolet flux is sensitive to log g and microturbulence, as well as temperature, we fix log g at 1.5 and microturbulence at 4 km s(-1), and derive the temperature from the best fit to the energy distribution (6270 K). Other recent temperature determinations are discussed, as are the sources of error. (C) 1996 American Astronomical Society. C1 YORK UNIV,DEPT PHYS & ASTRON,N YORK,ON M3J 1P3,CANADA. COMP SCI CORP,CTR SCI RES,SCI PROGRAMS,LANHAM,MD 20706. UNIV TORONTO,ERINDALE COLL,DEPT ASTRON,MISSISSAUGA,ON L5L 1C6,CANADA. USN OBSERV,ASTROMETRY DEPT,WASHINGTON,DC 20392. RP Evans, NR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MAIL STOP 4,CAMBRIDGE,MA 02138, USA. NR 50 TC 8 Z9 8 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1996 VL 111 IS 5 BP 2099 EP 2105 DI 10.1086/117946 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG899 UT WOS:A1996UG89900031 ER PT J AU Larsson, M Lepp, S Dalgarno, A Stromholm, C Sundstrom, G Zengin, V Danared, H Kallberg, A afUgglas, M Datz, S AF Larsson, M Lepp, S Dalgarno, A Stromholm, C Sundstrom, G Zengin, V Danared, H Kallberg, A afUgglas, M Datz, S TI Dissociative recombination of H2D+ and the cosmic abundance of deuterium SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE atomic data; ISM, abundances; ISM, molecules ID INTERSTELLAR CLOUDS; FRACTIONATION; LINE AB Deuterated molecules in interstellar clouds constitute a unique source of information on three interstellar parameters: the deuterium/hydrogen abundance ratio [D]/[H], the fractional ionization in dense clouds, and the galactic ionizing flux (Dalgarno & Lepp 1984, Millar 1990). The molecular ion H2D+ plays a key role in the formation of deuterated molecules. Dissociative recombination with electrons is a major loss channel and a potential source of deuterium atoms. An ion storage ring has been used to obtain the total recombination rate coefficient, and the probabilities for decay into H+H+D, HD+H and H-2+D. Using them in a model of the cloud L1529 we derive from observational data on HCO+ and DCO+ an upper limit to the fractional ionization of 2 x 10(-6), a [D]/[H] ratio of 1.7 x 10(-5) and an atomic D/H ratio of 2.7 x 10(-3). C1 UNIV NEVADA, DEPT PHYS, LAS VEGAS, NV 89154 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV STOCKHOLM, MANNE SIEGBAHN LAB, S-10405 STOCKHOLM, SWEDEN. OAK RIDGE NATL LAB, DIV PHYS, OAK RIDGE, TN 37831 USA. RP Larsson, M (reprint author), ROYAL INST TECHNOL, DEPT PHYS 1, S-10044 STOCKHOLM, SWEDEN. NR 18 TC 44 Z9 44 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 1996 VL 309 IS 1 BP L1 EP L3 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UK343 UT WOS:A1996UK34300001 ER PT J AU McCarthy, MC Travers, MJ Kovacs, A Gottlieb, CA Thaddeus, P AF McCarthy, MC Travers, MJ Kovacs, A Gottlieb, CA Thaddeus, P TI Laboratory detection of the C8H radical SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE line, identification; molecular data; techniques, spectroscopic; ISM, molecules; radio lines, ISM ID PARAMETERS; MOLECULES; SPECTRUM AB The C8H radical has been detected in an argon-acetylene discharge, conclusively confirming the identification by Cernicharo and Guelin in the accompanying Letter of their new linear molecule in IRC+10216. In addition to the ground (2) Pi(3/2) rotational ladder, the (2) Pi(1/2) ladder 19 cm(-1) above ground has been detected, and the entire fine structure-rotational spectrum calculated. The standard (2) Pi Hamiltonian fits the laboratory measurements of more than 30 radio lines between 80 and 100 GHz to high accuracy; yields precise values for the rotational, fine structure, and lambda-doubling constants; and allows the astronomically most interesting lines in the radio spectrum to be predicted to an uncertainty of 0.1 km s(-1) or better. C1 HARVARD UNIV, DIV APPL SCI, CAMBRIDGE, MA 02138 USA. RP McCarthy, MC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Kovacs, Attila/C-1171-2010 OI Kovacs, Attila/0000-0001-8991-9088 NR 13 TC 30 Z9 30 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 1996 VL 309 IS 2 BP L31 EP L33 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UK956 UT WOS:A1996UK95600002 ER PT J AU Narayan, R AF Narayan, R TI Advection-dominated models of luminous accreting black holes SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies, active; X-rays, stars ID ACTIVE GALACTIC NUCLEI; OBSCURING DUST TORI; NOVA-MUSCAE 1991; CYGNUS X-1; PAIR EQUILIBRIUM; INFRARED-SPECTRA; BINARY-SYSTEMS; SOFT PHOTONS; DISKS; COMPTONIZATION AB It has been found that a class of optically thin two-temperature advection-dominated accretion solutions explains many observations of low-luminosity accreting black holes. Here it is shown that these models give a satisfactory description also of higher luminosity systems, provided the viscosity parameter a is large. The models reproduce the spectra of black hole X-ray binaries in the low state and explain the transition from the low state to the high state at a critical mass accretion rate. The models also show that the X-ray/gamma-ray spectra of X-ray binaries and active galactic nuclei should be similar, as confirmed by observations. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 59 TC 95 Z9 97 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1996 VL 462 IS 1 BP 136 EP 141 DI 10.1086/177136 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG298 UT WOS:A1996UG29800015 ER PT J AU Lasota, JP Abramowicz, MA Chen, X Krolik, J Narayan, R Yi, I AF Lasota, JP Abramowicz, MA Chen, X Krolik, J Narayan, R Yi, I TI Is the accretion flow in NGC 4258 advection dominated? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies, individual (NGC 4258); galaxies, nuclei ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; COLD MATTER; GALAXIES; IONIZATION AB The mass of the central black hole in the active galaxy NGC 4258 (M106) has been measured to be M = 3.6 x 10(7) M(.) by Miyoshi et al. The Eddington luminosity corresponding to this mass is L(E) = 4.5 x 10(45) ergs s(-1). By contrast, the X-ray luminosity of the nucleus of NGC 4258 between 2 and 10 keV is (4 +/- 1) x 10(40) ergs s(-1) while the optical/UV luminosity is less than 1.5 x 10(42) ergs s(-1). The luminosity of NGC 4258 is therefore extremely sub-Eddington: L similar to 10(-5)L(E) in X-rays and L similar to 3 x 10(-4)L(E) even if we take the maximum optical/UV luminosity. Assuming the usual accretion efficiency of 0.1 would imply accretion rates orders of magnitude lower than in Seyfert galaxies and quasars. We show that the properties of the active galactic nuclei (AGNs) in NGC 4258 can be explained by an accretion flow in the form of a very hot, optically thin plasma that advects most of the viscously generated thermal energy into the central black hole and radiates only a small fraction of the energy. In this case, the accretion rate in Eddington units could be as high as similar to 0.16 alpha, where alpha is the standard viscosity parameter; and the size of the hot disk should be larger than similar to 10 times the Schwarzschild radius. We compare the predictions of this model with observations and discuss its application to other low-luminosity AGNs. C1 OBSERV PARIS,SECT MEUDON,DARC,F-92195 MEUDON,FRANCE. GOTHENBURG UNIV,DEPT ASTRON & ASTROPHYS,S-41296 GOTHENBURG,SWEDEN. CHALMERS UNIV TECHNOL,S-41296 GOTHENBURG,SWEDEN. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Lasota, JP (reprint author), CNRS,UPR 176,1 PL A BRIAND,F-92195 MEUDON,FRANCE. OI Narayan, Ramesh/0000-0002-1919-2730 NR 47 TC 164 Z9 166 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1996 VL 462 IS 1 BP 142 EP 146 DI 10.1086/177137 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG298 UT WOS:A1996UG29800016 ER PT J AU Wilner, DJ Ho, PTP Zhang, Q AF Wilner, DJ Ho, PTP Zhang, Q TI Searching for infall: Aperture synthesis HCO+(1-0) and SiO(2-1) observations of the G45.47+0.05 region SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; ISM, individual (G45.47+0.05); ISM, kinematics and dynamics; ISM, molecules; radio lines, ISM ID H-II REGIONS; EARLY-TYPE STARS; G10.6-0.4; EMISSION; COLLAPSE; AMMONIA; RADIO; CORE; MASER AB We report 5 '' resolution observations of the HCO+(1-0) and SiO(2-1) lines toward the G45.47+0.05 ultracompact H II region obtained with the OVRO millimeter array. We find no evidence for the spherical infall suggested by inverse P Cygni profiles observed in high-excitation NH3 lines at 40 '' resolution. Instead, we find multiple velocity components in HCO+ and SiO emission that suggest the presence of a protocluster of OB stars. We speculate that emission and absorption from separate sites of activity in the region conspire to mimic the inverse P Cygni infall signature. However, the observations do not entirely rule out a collapse localized to the ultracompact H II region, since absorption in the HCO+(1-0) line from low-excitation foreground gas may mask emission at velocities associated with infalling material. A new VLA 8.4 GHz D-array observation shows that the nearby ''cometary'' ultracompact H II region G45.45+0.06 lies within the northwest wall of an ionized shell with similar to 30 '' diameter. Unfortunately, this bright source within the VLA field of view precluded a search for faint centimeter continuum sources associated with the molecular line peaks. RP Wilner, DJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 28 TC 14 Z9 14 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1996 VL 462 IS 1 BP 339 EP 346 DI 10.1086/177155 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG298 UT WOS:A1996UG29800034 ER PT J AU Kenyon, SJ Yi, I Hartmann, L AF Kenyon, SJ Yi, I Hartmann, L TI A magnetic accretion disk model for the infrared excesses of T Tauri stars SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; infrared, stars; stars, magnetic fields; stars, pre-main-sequence ID YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; X-RAY SOURCES; BALMER LINE-PROFILES; HERBIG AE/BE STARS; NEUTRON STARS; OBSERVATIONAL APPEARANCE; ROTATING PROTOSTARS; CIRCUMSTELLAR DISKS; INSTABILITY MODEL AB We describe a magnetic accretion disk model for the infrared colors of T Tauri stars in the Taurus-Auriga molecular cloud. In this model, the stellar magnetic field truncates the disk several stellar radii above the stellar photosphere; material then flows along magnetic field lines and forms a bright ring at which the accretion stream impacts the star. The model successfully reproduces the observations for reasonable values of the magnetic field strength, 100-500 G; the stellar rotational period, 4-10 days; and the mass accretion rate, 10(-8) to 10(-6) M. yr(-1). The truncation radius, R(0), lies well inside the corotation radius, R(c). We estimate R(0)/R(c) approximate to 0.6-0.8 for classical T Tauri stars in our sample. This result constrains models for the rotational evolution and bipolar outflows of pre-main-sequence stars. Magnetic disk models make several testable predictions. The near-IR colors should correlate with the stellar magnetic field and the rotational period. The magnitude of the near-IR veiling should correlate strongly with the stellar rotational period. Strong CO emission or absorption features should be present only in stars with high accretion rates. Observations also discriminate between various types of magnetic disk geometries if intrinsic stellar parameters, such as the stellar radius and magnetic field strength, are well known. RP Kenyon, SJ (reprint author), SMITHSONIAN ASTORPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 120 TC 63 Z9 63 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1996 VL 462 IS 1 BP 439 EP 455 DI 10.1086/177163 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG298 UT WOS:A1996UG29800042 ER PT J AU Liu, WH Dalgarno, A AF Liu, WH Dalgarno, A TI The ultraviolet spectrum of the Jovian dayglow SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites, individual (Jupiter); ultraviolet, solar system ID ELECTRON-IMPACT EXCITATION; THRESHOLD VIBRATIONAL-EXCITATION; LY ALPHA-EMISSION; MOLECULAR-HYDROGEN; CROSS-SECTION; TRANSITION-PROBABILITIES; ELASTIC-SCATTERING; B3-SIGMA-U+ STATE; BAND SYSTEMS; WERNER-BAND AB The ultraviolet spectra of molecular hydrogen H-2 and HD due to solar fluorescence and photoelectron excitation are calculated and compared with the Jovian equatorial dayglow spectrum measured at 3 Angstrom resolution at solar maximum. The dayglow emission is accounted for in both brightness and spectral shape by the solar fluorescence and photoelectron excitation and requires no additional energy source. The emission is characterized by an atmospheric temperature of 530 K and an H-2 column density of 10(20) cm(-2). The dayglow spectrum contains a cascade contribution to the Lyman band emission from high-lying E and F states. Its relative weakness at short wavelengths is due to both self-absorption by H-2 and absorption by CH4. Strong wavelength coincidences of solar emission lines and absorption lines of H-2 and HD produce unique line spectra that can be identified in the dayglow spectrum. The strongest fluorescence is due to absorption of the solar Ly beta line at 1025.72 Angstrom by the P(1) line of the (6, 0) Lyman band of H-2 at 1025.93 Angstrom. The fluorescence lines due to absorption of the solar O VI line at 1031.91 Angstrom by vibrationally excited H-2 via the Q(3) line of the (1, 1) Werner band at 1031.86 Angstrom are identified. The fluorescence lines provide a sensitive measure of the atmospheric temperature. There occurs an exact coincidence of the solar O VI line at 1031.91 Angstrom and the R(0) line of the (6, 0) Lyman band of HD at 1031.91 Angstrom but HD on Jupiter is difficult to detect because of the dominance of the H-2 emission where the HD emission is particularly strong. Higher spectral resolution and higher sensitivity may make possible such a detection. The high-resolution (0.3 Angstrom) spectra of H-2 and HD are presented to stimulate search for the HD on Jupiter with the Hubble Space Telescope. RP Liu, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 66 TC 48 Z9 48 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1996 VL 462 IS 1 BP 502 EP 518 DI 10.1086/177168 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG298 UT WOS:A1996UG29800047 ER PT J AU Chen, W Novick, SE McCarthy, MC Travers, MJ Gottlieb, CA Cooksy, AL Thaddeus, P AF Chen, W Novick, SE McCarthy, MC Travers, MJ Gottlieb, CA Cooksy, AL Thaddeus, P TI Laboratory measurement of the hyperfine structure of HCCCO SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, molecules; line, identification; molecular data; molecular processes; radio lines, ISM ID MOLECULE; TMC-1 AB The two lowest hyperfine-split transitions of HCCCO (N = 1 --> 0 and 2 --> 1) have been measured with a Fourier transform microwave spectrometer. The frequencies, accurate to better than 0.20 km s(-1), should help guide future searches for interstellar HCCCO. C1 HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV MISSISSIPPI,DEPT CHEM,UNIVERSITY,MS 38677. RP Chen, W (reprint author), WESLEYAN UNIV,DEPT CHEM,MIDDLETOWN,CT 06459, USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 13 TC 2 Z9 2 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1996 VL 462 IS 1 BP 561 EP 562 DI 10.1086/177172 PN 1 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA UG298 UT WOS:A1996UG29800051 ER PT J AU Parenti, LR Maciolek, JA AF Parenti, LR Maciolek, JA TI Sicyopterus rapa, new species of sicydiine goby (Teleostei: Gobiidae), from Rapa, French Polynesia SO BULLETIN OF MARINE SCIENCE LA English DT Article AB Sicyopterus rapa, apparently endemic to one of the two southernmost islands of French Polynesia in the south central Pacific Ocean, is distinguished from congeners by a low number of premaxillary teeth and an unsealed ventral surface of the body in largest adults. Its putative closest living relatives are in the Marquesas and Indonesia. RP Parenti, LR (reprint author), SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT VERTEBRATE ZOOL, DIV FISHES, WASHINGTON, DC 20560 USA. NR 21 TC 4 Z9 4 U1 0 U2 2 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD MAY PY 1996 VL 58 IS 3 BP 660 EP 667 PG 8 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA UP205 UT WOS:A1996UP20500003 ER PT J AU Kensley, B AF Kensley, B TI The genus Paraxiopsis De Man, with descriptions of new species from the western Atlantic (Crustacea: Decapoda: Axiidae) SO BULLETIN OF MARINE SCIENCE LA English DT Article ID THALASSINIDEA AB The axiid shrimp genus Paraxiopsis De Man is reinstated, and separated from Eutrichocheles Wood Mason on the basis of five characters. Nine species are assigned to Paraxiopsis, two from the Pacific and seven from the western Atlantic. Five of the latter are previously undescribed: P. foveolata from the eastern Gull of Mexico; P. gracilimana from South Carolina to Tobaga, Belize, and the Gulf of Mexico; P. granulimana from Trinidad and the Florida Shelf; P. hispida from the Yucatan; and P. spinipleura from Belize and the Florida Keys. The type species, P. brocki De Man from the Indo-Pacific is redescribed, as is P. defensus Rathbun from the Caribbean. The species range from the intertidal to 95 m, in a variety of habitats including coral buttresses, coarse rubble, sand and mud. RP Kensley, B (reprint author), SMITHSONIAN INST,DEPT INVERTEBRATE ZOOL,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560, USA. NR 22 TC 7 Z9 12 U1 0 U2 1 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD MAY PY 1996 VL 58 IS 3 BP 709 EP 729 PG 21 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA UP205 UT WOS:A1996UP20500008 ER PT J AU Grube, M Gargas, A DePriest, PT AF Grube, M Gargas, A DePriest, PT TI A small insertion in the SSU rDNA of the lichen fungus Arthonia lapidicola is a degenerate group-I intron SO CURRENT GENETICS LA English DT Article DE ribosomal DNA; small subunit; 18s; degenerate introns; ascomycetes ID RNA SECONDARY STRUCTURE; CATALYTIC CORE; SEQUENCE; GENE; MODEL AB Insertions of less than 100 nt occurring in highly conserved regions of the small subunit ribosomal DNA (SSU rDNA) may represent degenerate forms of the group-I introns observed at the same positions in other organisms, A 63-nt insertion at SSU rDNA position 1512 (relative to the Escherichia coli SSU rDNA) of the lichen-forming fungus Arthonia lapidicola can be folded into a secondary structure with two stem loops and a pairing of the insertion and flanking sequences. The two stem loops may correspond to the P1 and P2, and the insertion-flanking pairing to the P10, of a group-I intron. Considering these small insertions as degenerate introns provides important clues to the evolution and catalytic function of group-I introns. C1 SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT BOT,WASHINGTON,DC 20560. GRAZ UNIV,INST BOT,A-8010 GRAZ,AUSTRIA. RI DePriest, Paula/K-6633-2015 NR 23 TC 26 Z9 26 U1 0 U2 0 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0172-8083 J9 CURR GENET JI Curr. Genet. PD MAY PY 1996 VL 29 IS 6 BP 582 EP 586 PG 5 WC Genetics & Heredity SC Genetics & Heredity GA UP319 UT WOS:A1996UP31900011 PM 8662198 ER PT J AU Lovejoy, TE AF Lovejoy, TE TI Beyond the concept of sustainable yield SO ECOLOGICAL APPLICATIONS LA English DT Article RP Lovejoy, TE (reprint author), SMITHSONIAN INST,1000 JEFFERSON DR SW,SUITE 320,WASHINGTON,DC 20560, USA. NR 2 TC 4 Z9 4 U1 0 U2 0 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD MAY PY 1996 VL 6 IS 2 BP 363 EP 363 DI 10.2307/2269370 PG 1 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA UH485 UT WOS:A1996UH48500003 ER PT J AU Kangas, P Adey, W AF Kangas, P Adey, W TI Mesocosms and ecological engineering SO ECOLOGICAL ENGINEERING LA English DT Editorial Material C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,MARINE SYST LAB,WASHINGTON,DC 20560. RP Kangas, P (reprint author), UNIV MARYLAND,NAT RESOURCES MANAGEMENT PROGRAM,COLLEGE PK,MD 20742, USA. RI Adey, Walter/G-2858-2011 NR 28 TC 19 Z9 19 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 J9 ECOL ENG JI Ecol. Eng. PD MAY PY 1996 VL 6 IS 1-3 BP 1 EP 5 DI 10.1016/0925-8574(95)00058-5 PG 5 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA UU947 UT WOS:A1996UU94700001 ER PT J AU Luckett, C Adey, WH Morrissey, J Spoon, DM AF Luckett, C Adey, WH Morrissey, J Spoon, DM TI Coral reef mesocosms and microcosms - Successes, problems, and the future of laboratory models SO ECOLOGICAL ENGINEERING LA English DT Article DE coral reef; mesocosm; microcosm; ecological engineering; Caribbean Sea; Great Barrier Reef; Biosphere 2; Bahamas AB Four coral reef mesocosms and microcosms, all established with the same basic approach to ecological engineering, are compared and contrasted. With some modifications, all use algal turf scrubbers as the primary device for controlling water quality, and thus leave the critical planktonic component undisturbed. The uses of engineering and applied ecology/biology to control and maintain these enclosed ecosystems has influenced their character and has contributed to both problems on some systems (patch formation, reduced reproduction and loss of plankton due to conventional pumping and filtration) and solutions on others (exterior control over predation and grazing, plankton friendly pumping and filtration) related to maintaining diverse, sustaining reef populations, As highly complex models, these systems can be unique tools for research on many aspects of the biology, ecology and restoration of coral reefs and on the effects of global change. Additionally, they support the view that the fragmentation of ecosystems can significantly alter community structure and diversity. C1 GREAT BARRIER REFF MARINE PK AUTHOR,GREAT BARRIER REEF AQUARIUM,TOWNSVILLE,QLD,AUSTRALIA. SBV,BIOSPHERE 2,ORACLE,AZ. RP Luckett, C (reprint author), SMITHSONIAN INST,MARINE SYST LAB,WASHINGTON,DC 20560, USA. NR 12 TC 8 Z9 9 U1 1 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 J9 ECOL ENG JI Ecol. Eng. PD MAY PY 1996 VL 6 IS 1-3 BP 57 EP 72 DI 10.1016/0925-8574(95)00051-8 PG 16 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA UU947 UT WOS:A1996UU94700004 ER PT J AU Craggs, RJ Adey, WH Jessup, BK Oswald, WJ AF Craggs, RJ Adey, WH Jessup, BK Oswald, WJ TI A controlled stream mesocosm for tertiary treatment of sewage SO ECOLOGICAL ENGINEERING LA English DT Article DE algal turf scrubber; heterogeneous community; mesocosm; primary production; tertiary treatment ID WATER TREATMENT FACILITY; NUTRIENT REMOVAL; PERIPHYTON; ENRICHMENT; BATCH AB Freshwater stream ecosystems are well known for their capabilities for ''self-purification'' of sewage and other wastewaters. Unfortunately, the efficiencies of treatment are low and concentrations and volumes now discharged cannot be treated by self-purification alone. This paper describes an experiment with a stream mesocosm, in central California, USA, using controlled ecosystem methodologies in the format of an algal turf scrubber (ATS(TM)). This system was used to drive primary production and export in the mesocosm to bring secondary sewage to tertiary levels. The mesocosm consisted of a natural, mixed assemblage of attached periphyton, microalgae and bacteria which colonized an inclined floway 152 m long and 6.7 m wide, over which wastewater flowed in a series of pulses. The capacity of the wastewater flow varied between 436 and 889 m(3) per day and various operational parameters were tested. Biomass was mechanically harvested from the floway at 1- or 2-week intervals depending upon the season. This paper presents the results for nitrogen and phosphorus removal as well as that of other contaminants and productivity of the algal turf. Nitrogen and phosphorus removal from the secondary wastewater was measured twice a week during four, 8-week quarters corresponding to the solar seasons. Nitrogen and phosphorus content of the harvested solids was also measured during these periods. Based on the percentage of nutrients in the harvested solids (3.1% N and 2.1% P) and the operational productivity of 35 g dry solids m(-2) day(-1), the yearly mean removal of nitrogen and phosphorus was 1.11 +/- 0.48 gNm(-2) day(-1) and 0.73 +/- 0.28 gP m(-2) day(-1), respectively. Results indicate the strong potential of controlled stream mesocosms for the removal of nutrients and other contaminants from wastewaters to achieve tertiary levels. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,MARINE SYST LAB,WASHINGTON,DC 20560. UNIV CALIF BERKELEY,ENVIRONM ENGN & HLTH SCI LAB,RICHMOND,CA 94804. NR 46 TC 54 Z9 55 U1 3 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 J9 ECOL ENG JI Ecol. Eng. PD MAY PY 1996 VL 6 IS 1-3 BP 149 EP 169 DI 10.1016/0925-8574(95)00056-9 PG 21 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA UU947 UT WOS:A1996UU94700009 ER PT J AU Adey, WH Finn, M Kangas, P Lange, L Luckett, C Spoon, DM AF Adey, WH Finn, M Kangas, P Lange, L Luckett, C Spoon, DM TI A Florida Everglades mesocosm - Model veracity after four years of self-organization SO ECOLOGICAL ENGINEERING LA English DT Article DE self-organization; Florida Everglades; mesocosm ID MULTIPLE AB Constructing functioning ecosystem models allows us to research the potential effects of degradation and fragmentation in ecosystems under pressure from human encroachment and points optimistically toward the potential for restoring degraded ecosystems. During 1987-1988, a complex, greenhouse-scale Mesocosm of a 50 km long transect of the Southwest Florida Everglades estuarine ecosystem (Gulf of Mexico shore to full fresh water) was constructed in Washington, DC, USA. At various times, a partial census that included the populations of vascular plants, macroalgae, protists, aquatic macroinvertebrates and fish was taken. This paper, based on a partial census of 369 species taken from November 1994 through January 1995, describes the self-organization of community structure, species populations and food webs that has occurred in the past 4 years of virtually complete isolation. Although many original species were lost as a result of smaller scale effects and a slightly skewed physical environment, the key vascular plants, algae and protists, as well as many secondary species, have largely maintained populations, provided community structuring elements and developed the base of a complex of food webs. Macro-invertebrate and fish populations have adjusted to the new environment with the basic character of their parent ecosystems intact. However, some significant species losses have occurred that clearly relate to the partial use of impeller pumps, and the consequent control of swimming larvae, the inability of the small system to support higher predators, and in some cases specifically suspect physical factors such as humidity and temperature. Methodologies of scaling, as it relates to different communities, and the degree and motivation for human intervention are discussed. C1 SBV,BIOSPHERE 2,ORACLE,AZ. GEORGETOWN UNIV,DEPT BIOL,WASHINGTON,DC 20057. UNIV MARYLAND,NAT RESOURCES MANAGEMENT PROGRAM,COLLEGE PK,MD 20742. RP Adey, WH (reprint author), SMITHSONIAN INST,NMNH,MARINE SYST LAB,WASHINGTON,DC 20560, USA. NR 49 TC 7 Z9 7 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 J9 ECOL ENG JI Ecol. Eng. PD MAY PY 1996 VL 6 IS 1-3 BP 171 EP 224 DI 10.1016/0925-8574(95)00057-7 PG 54 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA UU947 UT WOS:A1996UU94700010 ER PT J AU MacLeod, KG Huber, BT AF MacLeod, KG Huber, BT TI Strontium isotopic evidence for extensive reworking in sediments spanning the Cretaceous-Tertiary boundary at ODP Site 738 SO GEOLOGY LA English DT Article ID EXTINCTION AB The Maastrichtian and Danian intervals of Ocean Drilling Program (ODP) Hole 738C contain numerous microfossils above the level of their putative extinction, suggesting either (1) persistence of local communities long after species turnover occurred across the rest of the globe or (2) large-scale reworking. These interpretations have very different paleoenvironmental implications, but discriminating between them has proved difficult. To test the competing hypotheses, we measured the Sr-87/Sr-86 ratios of taxon-specific separates from a number of samples and compared these values both to each other and to expected seawater values at the time of deposition. Our results indicate extensive and pervasive reworking throughout Maastrichtian and lower Danian strata in ODP Hole 738C. We estimate that up to 30% of the mass of foraminifers in any sample can be contributed by individuals that have been reworked. RP MacLeod, KG (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,MRC NHB 121,WASHINGTON,DC 20560, USA. RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 NR 26 TC 15 Z9 16 U1 0 U2 1 PU GEOLOGICAL SOC AMERICA PI BOULDER PA PO BOX 9140 3300 PENROSE PLACE, BOULDER, CO 80301 SN 0091-7613 J9 GEOLOGY JI Geology PD MAY PY 1996 VL 24 IS 5 BP 463 EP 466 DI 10.1130/0091-7613(1996)024<0463:SIEFER>2.3.CO;2 PG 4 WC Geology SC Geology GA UK827 UT WOS:A1996UK82700020 ER PT J AU Evershed, RP Tuross, N AF Evershed, RP Tuross, N TI Proteinaceous material from potsherds and associated soils SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE potsherds; soils; amino acids; proteins; high performance liquid chromatography; polyacrylamide gel electrophoresis; collagen; gelatin ID CHROMATOGRAPHY MASS-SPECTROMETRY; GAS-CHROMATOGRAPHY; ORGANIC RESIDUES; BLOOD; BONE; ARCHAEOLOGY; COLLAGEN; REMAINS; LIPIDS; CARBON AB Amino acid and protein analyses of a range of archaeological potsherds and associated burial soils were performed by direct hydrolysis of powdered soils and potsherds samples, followed by high performance ion exchange chromatography. Detection of the eluting amino acids was by post-column derivatization, using o-phthalaldehyde and fluorescence monitoring. Microgram amounts of hydrolysed amino acids were detected in all the potsherds and soils analysed; free amino acids in both potsherd and soils were often below delectable limits (sherds recovered from the same archaeological context). The protein analyses involved extraction of powdered soil and potsherd samples with urea buffer,followed by polyacrylamide gel electrophoresis and protein staining. High sensitivity detection of the proteins used gold staining, following electrotransfer on to nitrocellulose. No obvious protein bands of molecular weight >10 kDa were detected in any of the potsherd samples that were studied. In general the amino acid and protein compositions of the individual potsherds were not sufficiently characteristic to suggest that HPLC ''fingerprinting'' of amino acids would significantly contribute to palaeodietary analysis or vessel use. Two potsherds, however, exhibited evidence of gelatin/collagen amino acid patterns. The presence of small amounts of gelatin were confirmed by the digestion of a >10 kDa protein extracted by bacterial collagenase. (C) 1996 Academic Press Limited C1 SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. RP Evershed, RP (reprint author), UNIV BRISTOL,SCH CHEM,CANTOCKS CLOSE,BRISTOL BS8 1TS,AVON,ENGLAND. NR 42 TC 26 Z9 27 U1 0 U2 20 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD MAY PY 1996 VL 23 IS 3 BP 429 EP 436 DI 10.1006/jasc.1996.0038 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA UM305 UT WOS:A1996UM30500009 ER EF