7000 List by Name
Total Page：16
File Type：pdf, Size：1020Kb
Load more
Recommended publications
-
John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C
VITA NAME: John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C. EDUCATION: 1970 B.A. George Washington University, Washington, D.C. 1972 M.S. Case Institute of Technology, Cleveland, OH 1976 Ph.D. University of Maryland, College Park, MD PROFESSIONAL EXPERIENCE: 2002–present David Ross Boyd Professor, University of Oklahoma, 2002–2002 Research Fellow, University of Texas, Austin, TX 1998–2002 Samuel Roberts Noble Foundation Presidential Professor, University of Oklahoma, Norman, OK 1997–1998 Big XIIFaculty Fellow,University ofOklahoma 1991–1992 Visiting Professor, Department of Astronomy, Columbia University, New York, NY 1989–present Professor, Department of Physics and Astronomy, University of Oklahoma, Norman, OK 1988–1994 Consultant and Participating Guest, Lawrence Livermore National Laboratory, Livermore, CA 1987–1988 Visiting Research Associate, Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 1984–1989 Associate Professor, University of Oklahoma 1979–1984 Assistant Professor, University of Oklahoma 1976–1979 Postdoctoral Research Fellow, Harvard-Smithsonian Center for Astrophysics, Harvard University PROFESSIONAL AND HONORARY SOCIETIES: American Astronomical Society International Astronomical Union Phi Beta Kappa RESEARCH INTERESTS: Stellar evolution, supernovae, nucleosynthesis and abundances Radio observations of supernovae and galaxies JOHN J. COWAN Page 2 PUBLICATIONS J. J. Cowan and W. K. Rose, “Production of 17O and 18O by Means of the Hot CNO Tri-Cycle,” Astrophys. J. (Letters) 201, L45 (1975) J. J. Cowan, M. Kafatos, and W. K. Rose, “Sources of Excitation of the Interstellar Gas and Galactic Structure,” Astrophys. J. 195, 47 (1975) M. F. A’Hearn and J. J. Cowan, “Molecular Production Rates in Comet Kohoutek,” As- tron. -
PCGS Certifies 1806 $5 Capped Bust Triple Struck Mint Error
TM minterrornews.com PCGS Certifies 1806 $5 Capped Bust Triple Struck Mint Error 18 Page Price Guide Issue 16 • Winter 2006 Inside! A Mike Byers Publication Al’s Coins Dealer in Mint Errors and Currency Errors alscoins.com pecializing in Mint Errors and Currency S Errors for 25 years. Visit my website to see a diverse group of type, modern mint and major currency errors. We also handle regular U.S. and World coins. I’m a member of CONECA and the American Numismatic Association. I deal with major Mint Error Dealers and have an excellent standing with eBay. Check out my show schedule to see which major shows I will be attending. I solicit want lists and will locate the Mint Errors of your dreams. Al’s Coins P.O. Box 147 National City, CA 91951-0147 Phone: (619) 442-3728 Fax: (619) 442-3693 e-mail: [email protected] Mint Error News Magazine Issue 16 • W i n t e r 2 0 0 6 Issue 16 • Winter 2006 Publisher & Editor - Table of Contents - Mike Byers Design & Layout Mike Byers’ Welcome 4 Sam Rhazi Off-Center Errors 5 Off-Metal & Clad Layer Split-Off Errors 17 Contributing Editors Buffalo 5¢ “Speared Bison” & WI 25¢ “Extra Leaves” 21 Tim Bullard Other Mint Error Types 24 Allan Levy PCGS Certifies 1806 $5 Capped Bust Triple Struck Mint Error 30 Contributing Writers NGC Certifies Double Struck 1873 $20 J-1344 34 Heritage Galleries & Auctioneers John Dannreuther • Mike Diamond Indian Cent Cu-Ni Reverse Die Cap 35 NGC • Rich Schemmer 1863 Indian Cent Reverse Die Cap 36 Bill Snyder • Fred Weinberg A Collection of Off-Metal Mint Errors Surfaces 38 Advertising 1973-S Kennedy Half Dollar Struck on Struck Aluminum Token 46 The ad space is sold out. -
Observational Studies of the Galaxy Peculiar Velocity Field
OBSERVATIONAL STUDIES OF THE GALAXY PECULIAR VELOCITY FIELD by Philip Andrew James Astrophysics Group Blackett Laboratory Imperial College of Science, Technology and Medicine London SW7 2BZ A thesis submitted for the degree of Doctor of Philosophy of the University of London and for the Diploma of Imperial College November 1988 1 ABSTRACT This thesis describes two observational studies of the peculiar velocity field of galaxies over scales of 50-100 Jr1 Mpc, and the consequences of these measurements for cosmological theories. An introduction is given to observational cosmology, emphasising the crucial questions of the nature of the dark matter and the formation of structure. The principal cosmological models are discussed, and the role of observations in developing these models is stressed. Consideration is given to those observations that are likely to prove good discriminators between the competing models, particular emphasis being given to studies of the coherent velocities of samples of galaxies. The first new study presented here uses optical photometry and redshifts, from the literature, for First Ranked Cluster Galaxies (FRCG’s). These galaxies are excellent standard candles, and thus ideal for peculiar velocity studies. A simple one dimensional analysis detects no relative motion between the Local Group of galaxies and 60 FRCG’s with redshifts of up to 15000 kms-1. This is shown to imply a streaming motion of the cluster galaxies of at least 600 kms_1 relative to the CBR. The second observational study is a reanalysis of the Rubin et al. (1976a,b) sample of Sc galaxies. Near-IR photometry is used in our reanalysis to minimise the effects of extinction and to facilitate the use of luminosity indicators in reducing the effects of selection biases. -
1. Introduction
THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other. -
Radio Sources in Low-Luminosity Active Galactic Nuclei
A&A 392, 53–82 (2002) Astronomy DOI: 10.1051/0004-6361:20020874 & c ESO 2002 Astrophysics Radio sources in low-luminosity active galactic nuclei III. “AGNs” in a distance-limited sample of “LLAGNs” N. M. Nagar1, H. Falcke2,A.S.Wilson3, and J. S. Ulvestad4 1 Arcetri Observatory, Largo E. Fermi 5, Florence 50125, Italy 2 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Germany e-mail: [email protected] 3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA Adjunct Astronomer, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] 4 National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801, USA e-mail: [email protected] Received 23 January 2002 / Accepted 6 June 2002 Abstract. This paper presents the results of a high resolution radio imaging survey of all known (96) low-luminosity active galactic nuclei (LLAGNs) at D ≤ 19 Mpc. We first report new 2 cm (150 mas resolution using the VLA) and 6 cm (2 mas resolution using the VLBA) radio observations of the previously unobserved nuclei in our samples and then present results on the complete survey. We find that almost half of all LINERs and low-luminosity Seyferts have flat-spectrum radio cores when observed at 150 mas resolution. Higher (2 mas) resolution observations of a flux-limited subsample have provided a 100% (16 of 16) detection rate of pc-scale radio cores, with implied brightness temperatures ∼>108 K. The five LLAGNs with the highest core radio fluxes also have pc-scale “jets”. -
Astronomy Astrophysics
A&A 433, 79–86 (2005) Astronomy DOI: 10.1051/0004-6361:20034537 & c ESO 2005 Astrophysics Asymmetrical structure of ionization and kinematics in the Seyfert galaxy NGC 5033 E. Mediavilla1, A. Guijarro2, A. Castillo-Morales3 , J. Jiménez-Vicente3, E. Florido3, S. Arribas4,, B. García-Lorenzo1, and E. Battaner3 1 Instituto de Astrofísica de Canarias, Tenerife, Spain e-mail: [email protected] 2 Centro Astronómico Hispano Alemán, Almería, Spain e-mail: [email protected] 3 Dpto. Física Teórica y del Cosmos, Universidad de Granada, Spain 4 Space Telescope Science Institute, Baltimore, USA Received 18 October 2003 / Accepted 29 November 2004 Abstract. We present integral field spectroscopy of NGC 5033, a low luminosity Seyfert galaxy. The observations were made with INTEGRAL, a fiber based system operating at the WHT. The intensity map of the Hβ emission line represents a spi- ral or ring-like pattern of HII regions. On the contrary, the [OIII] intensity map morphology is markedly anisotropic. The strong morphological differences imply that the [OIII] emitters represent highly ionized gas illuminated by the central source. The [OIII] map morphology is compatible with a biconical structure of ionization induced by strong extinction in the galaxy disc that also obscures half of the spheroidal stellar bulge. We identify the spectrum corresponding to the Seyfert 1 nucleus from the presence of Hβ broad emission lines. This spectrum is located in a region where strong extinction is expected but exhibits the bluest spectral energy distribution. The Seyfert 1 nucleus seems to be offcenter with respect to the stellar rotation center. This result has been also found in other Seyfert galaxies and interpreted in terms of a past merger. -
![Arxiv:1108.0403V1 [Astro-Ph.CO] 1 Aug 2011 Esitps Hleg Oglx Omto Oesadthe and Models Formation Galaxy at to Tion](https://docslib.b-cdn.net/cover/5126/arxiv-1108-0403v1-astro-ph-co-1-aug-2011-esitps-hleg-oglx-omto-oesadthe-and-models-formation-galaxy-at-to-tion-515126.webp)
Arxiv:1108.0403V1 [Astro-Ph.CO] 1 Aug 2011 Esitps Hleg Oglx Omto Oesadthe and Models Formation Galaxy at to Tion
Noname manuscript No. (will be inserted by the editor) Production of dust by massive stars at high redshift C. Gall · J. Hjorth · A. C. Andersen To be published in A&A Review Abstract The large amounts of dust detected in sub-millimeter galaxies and quasars at high redshift pose a challenge to galaxy formation models and theories of cosmic dust forma- tion. At z > 6 only stars of relatively high mass (> 3 M⊙) are sufficiently short-lived to be potential stellar sources of dust. This review is devoted to identifying and quantifying the most important stellar channels of rapid dust formation. We ascertain the dust production ef- ficiency of stars in the mass range 3–40 M⊙ using both observed and theoretical dust yields of evolved massive stars and supernovae (SNe) and provide analytical expressions for the dust production efficiencies in various scenarios. We also address the strong sensitivity of the total dust productivity to the initial mass function. From simple considerations, we find that, in the early Universe, high-mass (> 3 M⊙) asymptotic giant branch stars can only be −3 dominant dust producers if SNe generate . 3 × 10 M⊙ of dust whereas SNe prevail if they are more efficient. We address the challenges in inferring dust masses and star-formation rates from observations of high-redshift galaxies. We conclude that significant SN dust pro- duction at high redshift is likely required to reproduce current dust mass estimates, possibly coupled with rapid dust grain growth in the interstellar medium. C. Gall Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark Tel.: +45 353 20 519 Fax: +45 353 20 573 E-mail: [email protected] J. -
Radiation Hydrodynamics Experiments on Large High-Energy-Density-Physics Facilities That Are Relevant to Astrophysics
Radiation Hydrodynamics Experiments on Large High-Energy-Density-Physics Facilities that are Relevant to Astrophysics by Heath J. LeFevre A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Applied Physics) in The University of Michigan 2021 Doctoral Committee: Professor Emeritus R P. Drake, Chair Dr. Paul A. Keiter, Los Alamos National Laboratory, Co-Chair Associate Professor Eric Johnsen Associate Professor Carolyn C. Kuranz Associate Professor Ryan D. McBride Heath J. LeFevre [email protected] ORCID iD: 0000-0002-7091-4356 c Heath J. LeFevre 2021 ACKNOWLEDGEMENTS I want to thank my family and friends for supporting me and listening to my various plans on how I will finish my thesis and when I would graduate. You don't have to hear about my thesis anymore, but you will almost certainly have to suffer through more plans. I would also like to thank my advisors Paul Drake, Carolyn Kuranz, and Paul Keiter. I appreciate the opportunity you gave me to complete my PhD and the financial support you provided so that I could run around the country blowing things up, with lasers, for five years. Further thanks are due to my committee members Eric Johnsen and Ryan McBride who are unlucky enough to be the only people who have to read this thesis that did not sign up for the job when I entered grad school. ii TABLE OF CONTENTS ACKNOWLEDGEMENTS :::::::::::::::::::::::::: ii LIST OF FIGURES ::::::::::::::::::::::::::::::: vi LIST OF TABLES :::::::::::::::::::::::::::::::: xvi LIST OF APPENDICES :::::::::::::::::::::::::::: xvii LIST OF ABBREVIATIONS ::::::::::::::::::::::::: xviii ABSTRACT ::::::::::::::::::::::::::::::::::: xx CHAPTER I. Introduction .............................. 1 1.1 High-Energy-Density-Physics . -
2014 Observers Challenge List
2014 TMSP Observer's Challenge Atlas page #s # Object Object Type Common Name RA, DEC Const Mag Mag.2 Size Sep. U2000 PSA 18h31m25s 1 IC 1287 Bright Nebula Scutum 20'.0 295 67 -10°47'45" 18h31m25s SAO 161569 Double Star 5.77 9.31 12.3” -10°47'45" Near center of IC 1287 18h33m28s NGC 6649 Open Cluster 8.9m Integrated 5' -10°24'10" Can be seen in 3/4d FOV with above. Brightest star is 13.2m. Approx 50 stars visible in Binos 18h28m 2 NGC 6633 Open Cluster Ophiuchus 4.6m integrated 27' 205 65 Visible in Binos and is about the size of a full Moon, brightest star is 7.6m +06°34' 17h46m18s 2x diameter of a full Moon. Try to view this cluster with your naked eye, binos, and a small scope. 3 IC 4665 Open Cluster Ophiuchus 4.2m Integrated 60' 203 65 +05º 43' Also check out “Tweedle-dee and Tweedle-dum to the east (IC 4756 and NGC 6633) A loose open cluster with a faint concentration of stars in a rich field, contains about 15-20 stars. 19h53m27s Brightest star is 9.8m, 5 stars 9-11m, remainder about 12-13m. This is a challenge obJect to 4 Harvard 20 Open Cluster Sagitta 7.7m integrated 6' 162 64 +18°19'12" improve your observation skills. Can you locate the miniature coathanger close by at 19h 37m 27s +19d? Constellation star Corona 5 Corona Borealis 55 Trace the 7 stars making up this constellation, observe and list the colors of each star asterism Borealis 15H 32' 55” Theta Corona Borealis Double Star 4.2m 6.6m .97” 55 Theta requires about 200x +31° 21' 32” The direction our Sun travels in our galaxy. -
Lemmings. I. the Emerlin Legacy Survey of Nearby Galaxies. 1.5-Ghz Parsec-Scale Radio Structures and Cores
MNRAS 000,1{44 (2018) Preprint 8 February 2018 Compiled using MNRAS LATEX style file v3.0 LeMMINGs. I. The eMERLIN legacy survey of nearby galaxies. 1.5-GHz parsec-scale radio structures and cores R. D. Baldi1?, D. R. A. Williams1, I. M. McHardy1, R. J. Beswick2, M. K. Argo2;3, B. T. Dullo4, J. H. Knapen5;6, E. Brinks7, T. W. B. Muxlow2, S. Aalto8, A. Alberdi9, G. J. Bendo2;10, S. Corbel11;12, R. Evans13, D. M. Fenech14, D. A. Green15, H.-R. Kl¨ockner16, E. K¨ording17, P. Kharb18, T. J. Maccarone19, I. Mart´ı-Vidal8, C. G. Mundell20, F. Panessa21, A. B. Peck22, M. A. P´erez-Torres9, D. J. Saikia18, P. Saikia17;23, F. Shankar1, R. E. Spencer2, I. R. Stevens24, P. Uttley25 and J. Westcott7 1 School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK 2 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK 3 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 4 Departamento de Astrofisica y Ciencias de la Atmosfera, Universidad Complutense de Madrid, E-28040 Madrid, Spain 5 Instituto de Astrofisica de Canarias, Via Lactea S/N, E-38205, La Laguna, Tenerife, Spain 6 Departamento de Astrofisica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain 7 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK 8 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 43992 Onsala, Sweden 9 Instituto de Astrofisica de Andaluc´ıa(IAA, CSIC); Glorieta de la Astronom´ıa s/n, 18008-Granada, Spain 10 ALMA Regional Centre Node, UK 11 Laboratoire AIM (CEA/IRFU - CNRS/INSU - Universit´eParis Diderot), CEA DSM/IRFU/SAp, F-91191 Gif-sur-Yvette, France 12 Station de Radioastronomie de Nan¸cay, Observatoire de Paris, PSL Research University, CNRS, Univ. -
Perseus Perseus
Lateinischer Name: Deutscher Name: Per Perseus Perseus Atlas (2000.0) Karte Cambridge Star Kulmination um 2, 3 Atlas Mitternacht: Benachbarte 1, 4, Sky Atlas Sternbilder: 5 And Ari Aur Cam Cas 7. November Tau Tri Deklinationsbereich: 30° ... 59° Fläche am Himmel: 615° 2 Mythologie und Geschichte: Akrisios war der König von Argos und hatte eine hübsche Tochter namens Danae. Das Orakel von Delphi prophezeite ihm, sein Enkelsohn werde ihn einst töten. Aus Furcht vor diesem Orakelspruch ließ Akrisios seine Tochter Danae in einen Turm einschließen, damit sie keinen Mann empfangen könne. Akrisios konnte natürlich nicht wissen, dass Zeus selbst sich der liebreizenden Danae nähern wollte. Zeus tat dies auch und nahm dazu die Form eines goldenen Regens an, der durch die Wände, Fugen, Ritzen und Fenster drang. Danae gebar einen Sohn, welcher "Der aus fließendem Gold entstandene" oder auch "Der Goldgeborene" genannt wurde - eben den Perseus. Akrisios blieb dies natürlich nicht lange verborgen und er ließ seine Tochter und sein Enkelkind in einen Kasten einnageln, der dann ins Meer geworfen wurde. Danae und Perseus trieben lange Zeit auf dem Meer, bis sie schließlich an der Küste der steinigen Insel Seriphos strandeten und aus ihrem Gefängnis befreit wurden. Auf dieser Insel herrschte Polydektes, der bald jahrelang um die schöne Danae warb, jedoch vergebens. Entweder um Danae doch noch zur Ehe zu zwingen oder um Perseus aus dem Weg zu schaffen, schickte er den inzwischen zum Jüngling herangewachsenen Sohn der Danae aus, eine tödliche Aufgabe zu erledigen. Er solle das Haupt der Medusa zu holen. Die Medusa war eine der Gorgonen, eine der drei Töchter des Phorkys, die mit Schlangenhaaren ausgestattet waren und einen versteinernden Blick werfen konnten. -
A DEEP SEARCH for PROMPT RADIO EMISSION from THERMONUCLEAR SUPERNOVAE with the VERY LARGE ARRAY Laura Chomiuk1,11, Alicia M
Draft version July 1, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 A DEEP SEARCH FOR PROMPT RADIO EMISSION FROM THERMONUCLEAR SUPERNOVAE WITH THE VERY LARGE ARRAY Laura Chomiuk1;11, Alicia M. Soderberg2, Roger A. Chevalier3, Seth Bruzewski1, Ryan J. Foley4,5, Jerod Parrent2, Jay Strader1, Carles Badenes6 Claes Fransson7 Atish Kamble2, Raffaella Margutti8, Michael P. Rupen9, & Joshua D. Simon10 Draft version July 1, 2018 ABSTRACT Searches for circumstellar material around Type Ia supernovae (SNe Ia) are one of the most powerful tests of the nature of SN Ia progenitors, and radio observations provide a particularly sensitive probe of this material. Here we report radio observations for SNe Ia and their lower-luminosity thermonu- clear cousins. We present the largest, most sensitive, and spectroscopically diverse study of prompt (∆t . 1 yr) radio observations of 85 thermonuclear SNe, including 25 obtained by our team with the unprecedented depth of the Karl G. Jansky Very Large Array. With these observations, SN 2012cg joins SN 2011fe and SN 2014J as a SN Ia with remarkably deep radio limits and excellent temporal −1 _ −9 M yr coverage (six epochs, spanning 5{216 days after explosion, yielding M=vw . 5 × 10 100 km s−1 , assuming B = 0:1 and e = 0:1). All observations yield non-detections, placing strong constraints on the presence of circumstellar material. We present analytical models for the temporal and spectral evolution of prompt radio emission from thermonuclear SNe as expected from interaction with either wind-stratified or uniform density media. These models allow us to constrain the progenitor mass loss rates, with limits ranging _ −9 −4 −1 −1 from M .