3C75 Binary Black Hole System (VLA Archive)
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Herschel PACS and SPIRE Imaging of CW Leonis*
A&A 518, L141 (2010) Astronomy DOI: 10.1051/0004-6361/201014658 & c ESO 2010 Astrophysics Herschel: the first science highlights Special feature Letter to the Editor Herschel PACS and SPIRE imaging of CW Leonis D. Ladjal1,M.J.Barlow2,M.A.T.Groenewegen3,T.Ueta4,J.A.D.L.Blommaert1, M. Cohen5, L. Decin1,6, W. De Meester1,K.Exter1,W.K.Gear7,H.L.Gomez7,P.C.Hargrave7, R. Huygen1,R.J.Ivison8, C. Jean1, F. Kerschbaum9,S.J.Leeks10,T.L.Lim10, G. Olofsson11, E. Polehampton10,12,T.Posch9,S.Regibo1,P.Royer1, B. Sibthorpe8,B.M.Swinyard10, B. Vandenbussche1 , C. Waelkens1, and R. Wesson2 1 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium e-mail: [email protected] 2 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 3 Koninklijke Sterrenwacht van België, Ringlaan 3, 1180 Brussels, Belgium 4 Dept. of Physics and Astronomy, University of Denver, Mail Stop 6900, Denver, CO 80208, USA 5 Radio Astronomy Laboratory, University of California at Berkeley, CA 94720, USA 6 Sterrenkundig Instituut Anton Pannekoek, Universiteit van Amsterdam, Kruislaan 403, 1098 Amsterdam, The Netherlands 7 School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff, Wales CF24 3YB, UK 8 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 9 University Vienna, Department of Astronomy, Türkenschanzstrasse 17, 1180 Wien, Austria 10 Space Science and Technology Department, Rutherford Appleton Laboratory, Oxfordshire, OX11 0QX, UK 11 Dept. of Astronomy, Stockholm University, AlbaNova University Center, Roslagstullsbacken 21, 10691 Stockholm, Sweden 12 Department of Physics, University of Lethbridge, Alberta, Canada Received 31 March 2010 / Accepted 15 April 2010 ABSTRACT Herschel PACS and SPIRE images have been obtained over a 30 × 30 area around the well-known carbon star CW Leo (IRC +10 216). -
Gillian R. Knapp - Curriculum Vitae Born: Widnes, United Kingdom, October 10, 1944
Gillian R. Knapp - Curriculum Vitae Born: Widnes, United Kingdom, October 10, 1944. B.Sc. (Hons.) Physics, University of Edinburgh, 1966. Ph.D. Astronomy, University of Maryland, 1972. Professional Societies American Astronomical Society, Royal Astronomical Society, International Union of Radio Science, International Astronomical Union Positions held Teaching associate, University of Maryland, l971-3. Research fellow, Senior Research Fellow, Research Associate, California Institute of Technology, 1974-9. Research astronomer, Princeton University, 1980-4. Associate Professor, Professor, Princeton University, 1984- Visiting Assistant Professor, University of Washington, spring 1979. Visiting Associate Professor, UCLA, spring 1980. Visiting Fellow, University of Groningen, The Netherlands, summer 1981. Visiting astronomer, Bell Laboratories, 1980-92. Visiting professor, Institute for Astronomy, University of Hawaii, Fall 1989 Awards Tinsley Centennial Professor, University of Texas, Fall 1985. Distinguished Alumnus Award, University of Maryland, 2003 Leadership Alliance Mentorship Award, 2007 Current and Recent National/ International Committees Caltech Submillimeter Observatory Director’s Advisory Committee: NAIC Arecibo Advi- sory Committee: Spitzer Science Center Users’ Committee: NAIC Arecibo Large Projects Oversight Committee: Review Board, DARK Cosmology Institute Current and Recent Princeton University and Department Activities EEEO officer, Coordinator for Undergraduate Summer Research, and Director of Graduate Studies, Astrophysics: -
Active Galactic Nuclei - Suzy Collin, Bożena Czerny
ASTRONOMY AND ASTROPHYSICS - Active Galactic Nuclei - Suzy Collin, Bożena Czerny ACTIVE GALACTIC NUCLEI Suzy Collin LUTH, Observatoire de Paris, CNRS, Université Paris Diderot; 5 Place Jules Janssen, 92190 Meudon, France Bożena Czerny N. Copernicus Astronomical Centre, Bartycka 18, 00-716 Warsaw, Poland Keywords: quasars, Active Galactic Nuclei, Black holes, galaxies, evolution Content 1. Historical aspects 1.1. Prehistory 1.2. After the Discovery of Quasars 1.3. Accretion Onto Supermassive Black Holes: Why It Works So Well? 2. The emission properties of radio-quiet quasars and AGN 2.1. The Broad Band Spectrum: The “Accretion Emission" 2.2. Optical, Ultraviolet, and X-Ray Emission Lines 2.3. Ultraviolet and X-Ray Absorption Lines: The Wind 2.4. Variability 3. Related objects and Unification Scheme 3.1. The “zoo" of AGN 3.2. The “Line of View" Unification: Radio Galaxies and Radio-Loud Quasars, Blazars, Seyfert 1 and 2 3.2.1. Radio Loud Quasars and AGN: The Jet and the Gamma Ray Emission 3.3. Towards Unification of Radio-Loud and Radio-Quiet Objects? 3.4. The “Accretion Rate" Unification: Low and High Luminosity AGN 4. Evolution of black holes 4.1. Supermassive Black Holes in Quasars and AGN 4.2. Supermassive Black Holes in Quiescent Galaxies 5. Linking the growth of black holes to galaxy evolution 6. Conclusions Acknowledgements GlossaryUNESCO – EOLSS Bibliography Biographical Sketches SAMPLE CHAPTERS Summary We recall the discovery of quasars and the long time it took (about 15 years) to build a theoretical framework for these objects, as well as for their local less luminous counterparts, Active Galactic Nuclei (AGN). -
Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis, -
(NASA/Chandra X-Ray Image) Type Ia Supernova Remnant – Thermonuclear Explosion of a White Dwarf
Stellar Evolution Card Set Description and Links 1. Tycho’s SNR (NASA/Chandra X-ray image) Type Ia supernova remnant – thermonuclear explosion of a white dwarf http://chandra.harvard.edu/photo/2011/tycho2/ 2. Protostar formation (NASA/JPL/Caltech/Spitzer/R. Hurt illustration) A young star/protostar forming within a cloud of gas and dust http://www.spitzer.caltech.edu/images/1852-ssc2007-14d-Planet-Forming-Disk- Around-a-Baby-Star 3. The Crab Nebula (NASA/Chandra X-ray/Hubble optical/Spitzer IR composite image) A type II supernova remnant with a millisecond pulsar stellar core http://chandra.harvard.edu/photo/2009/crab/ 4. Cygnus X-1 (NASA/Chandra/M Weiss illustration) A stellar mass black hole in an X-ray binary system with a main sequence companion star http://chandra.harvard.edu/photo/2011/cygx1/ 5. White dwarf with red giant companion star (ESO/M. Kornmesser illustration/video) A white dwarf accreting material from a red giant companion could result in a Type Ia supernova http://www.eso.org/public/videos/eso0943b/ 6. Eight Burst Nebula (NASA/Hubble optical image) A planetary nebula with a white dwarf and companion star binary system in its center http://apod.nasa.gov/apod/ap150607.html 7. The Carina Nebula star-formation complex (NASA/Hubble optical image) A massive and active star formation region with newly forming protostars and stars http://www.spacetelescope.org/images/heic0707b/ 8. NGC 6826 (Chandra X-ray/Hubble optical composite image) A planetary nebula with a white dwarf stellar core in its center http://chandra.harvard.edu/photo/2012/pne/ 9. -
Orbital Elements of Double Stars
Orbital elements of double stars: ADS 1548 Marco Scardia, Jean-Louis Prieur, Luigi Pansecchi, Robert Argyle, Josefina Ling, Eric Aristidi, Alessio Zanutta, Lyu Abe, Philippe Bendjoya, Jean-Pierre Rivet, et al. To cite this version: Marco Scardia, Jean-Louis Prieur, Luigi Pansecchi, Robert Argyle, Josefina Ling, et al.. Orbital elements of double stars: ADS 1548. 2018, pp.1. hal-02357208 HAL Id: hal-02357208 https://hal.archives-ouvertes.fr/hal-02357208 Submitted on 23 Nov 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. INTERNATIONAL ASTRONOMICAL UNION COMMISSION G1 (BINARY AND MULTIPLE STAR SYSTEMS) DOUBLE STARS INFORMATION CIRCULAR No. 194 (FEBRUARY 2018) NEW ORBITS ADS Name P T e Ω(2000) 2018 Author(s) α2000δ n a i ! Last ob. 2019 1548 A 819 AB 135y4 2011.06 0.548 153◦8 39◦7 000161 SCARDIA 01570+3101 2◦6587 000424 50◦5 189◦7 2017.833 49.4 0.163 et al. (*) - HDS 333 49.54 1981.14 0.60 252.6 253.8 0.542 TOKOVININ 02332-5156 7.2665 0.413 57.4 150.9 2018.073 255.7 0.519 - COU 691 61.76 1964.53 0.059 68.6 276.2 0.109 DOCOBO 03423+3141 5.8290 0.160 -
Distant Arm - NGC772
29 September 2016, Zeiss Cas 150/2250 Distant Arm - NGC772 Telescope: Zeiss Cassegrain 150/2250 Eyepieces: ATC53P - ATC Plossl, f=53mm, (42×, 530) ATC20K - ATC Kellner, f=20mm, (113×, 220) A-16 - Zeiss Abbe Ortho, f=16mm, (141×, 200) O-12.5 - CZJ Ortho, f=12.5mm, (180×, 140) Time: 2016/09/29 19:30-21:40UT Location: R´ıˇcanyˇ Weather: Clear sky with slight haze and decaying small thin clouds. Mount: Zeiss 1b Accessories: Baader/Zeiss T2 prism This was my typical backyard session. I could go out only for a short time after I put all three kids in to their beds. The night was still warm. Normally, I would try to take an advantage of it and go to some darker place. As I was alone with the kids for the whole week I was bound to stay in our backyard. During last couple of years, I have learnt to live with this handicap. There is always something interesting to look at, even with small refractors. Recently, I was explor- ing the capability of my largest telescope, 150mm Cassegrain. For this night, the main targets were two galaxies, NGC 660 and NGC 772, which I had troubles to locate two days before in 80mm refractor. I was curios how much of help the larger telescope would be. I did not jump to these two galaxies im- mediately. They were still low in the slight haze enhanced by the street lamps. I started a little bit higher in Andromeda with beau- tiful edge-on galaxy NGC 891 (V=10.0, 13:50 ×2:50, PA22◦). -
Celestial Radio Sources Whitham D
Important Celestial Radio Sources Whitham D. Reeve Introduction The list of celestial radio sources presented below was obtained from the National Radio Astronomy Observatory (NRAO) library. Each column heading is defined below. As presented here, the list is sorted in order of flux density as received on Earth. As an aid in visualizing the location of the more powerful radio sources in the sky with respect to the Milky Way galaxy, an annotated radio map also is provided along with explanations of its important features. Listing – Definition of column headings The information below is necessarily brief. Additional information may be found by using an online encyclopedia (for example, http://en.wikipedia.org/wiki/Main_Page ) or visiting other online sources such as the National Radio Astronomy Observatory website ( http://www.nrao.edu/ ). Object Name: Each object is named according its original catalog listing (for celestial object naming conventions, see Tom Crowley’s article “Introduction to Astronomical Catalogs” in the October- November 2010 issue of Radio Astronomy ). Most of the objects in the list originally were listed in the 3rd Cambridge catalog (3C) but some are in NRAO’s catalog (NRAO). Right Ascension and Declination: The right ascension and declination are used together to define the location of an object in the sky according to the equatorial coordinate system . Right ascension is given in hour minute second format and abbreviated RA . RA is the angle measured in hours, minutes and seconds from the Vernal equinox (intersection of celestial equator and ecliptic). The declination, abbreviated Dec , is the number of degrees, minutes and seconds above (0° to +90°) or below (0° to – 90°) the celestial equator. -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
VLBA Polarimetric Observations of the CSS Quasar 3C 147
A&A 504, 741–749 (2009) Astronomy DOI: 10.1051/0004-6361/200811190 & c ESO 2009 Astrophysics VLBA polarimetric observations of the CSS quasar 3C 147 A. Rossetti1,F.Mantovani1, D. Dallacasa1,2, W. Junor3,C.J.Salter4, and D. J. Saikia5 1 Istituto di Radioastronomia – INAF, via Gobetti 101, 40129, Bologna, Italy e-mail: [email protected] 2 Dipartimento di Astronomia, Università degli Studi, via Ranzani 1, 40127 Bologna, Italy 3 Los Alamos National Laboratory, Los Alamos, NM 87545, USA 4 Arecibo Observatory, HC3 Box 53995, Arecibo 00612, Puerto Rico 5 National Centre for Astrophysics, TIFR, Post Bag 3, Ganeshkhind, Pune 411 007, India Received 20 October 2008 / Accepted 24 April 2009 ABSTRACT Aims. We report new VLBA polarimetric observations of the compact steep-spectrum (CSS) quasar 3C 147 (B0538 + 498) at 5 and 8.4 GHz. Methods. By using multifrequency VLBA observations, we derived milliarcsecond-resolution images of the total intensity, polarisa- tion, and rotation measure distributions, by combining our new observations with archival data. Results. The source shows a one-sided structure, with a compact region, and a component extending about 200 mas to the south-west. The compact region is resolved into two main components with polarised emission, a complex rotation measure distribution, and a magnetic field dominated by components perpendicular to the source axis. Conclusions. By considering all the available data, we examine the possible location of the core component, and discuss two possible interpretations of the observed structure of this source: core-jet and lobe-hot spot. Further observations to unambiguously determine the location of the core would help distinguish between the two possibilities discussed here. -
X-Ray Observations of Neutron Stars with XMM-Newton & Chandra
X-Ray Observations of Neutron Stars with XMM-Newton & Chandra Hui Chung Yue M¨unchen2007 X-Ray Observations of Neutron Stars with XMM-Newton & Chandra Hui Chung Yue Dissertation an der Fakult¨atf¨urPhysik der Ludwig–Maximilians–Universit¨at M¨unchen vorgelegt von Hui Chung Yue aus Hong Kong M¨unchen, den 6 November 2007 Erstgutachter: Priv. Doz. Dr. Werner Becker Zweitgutachter: Prof. Dr. Harald Lesch Tag der m¨undlichen Pr¨ufung:27 November 2007 Contents Summary xiii 1 Introduction 1 1.1 A Brief History of Neutron Stars ....................... 1 1.2 The Physics of Neutron Stars ......................... 4 1.2.1 Formation ................................ 4 1.2.2 Global structure ............................. 5 1.2.3 Composition ............................... 7 1.2.4 Thermal evolution ........................... 9 1.2.5 Pulsar magnetosphere and high energy radiation . 11 1.3 Manifestations of Isolated Neutron Stars ................... 18 1.3.1 Rotation-powered pulsars ....................... 19 1.3.2 Soft γ−ray repeaters/Anomalous X-ray pulsars . 19 1.3.3 Central compact objects in supernova remnants . 20 1.3.4 Dim thermal isolated neutron stars . 21 1.3.5 Rotating RAdio Transients (RRATs) . 21 1.4 Studying Neutron Stars with XMM-Newton & Chandra . 22 1.4.1 Chandra ................................. 22 1.4.2 XMM-Newton .............................. 23 2 X-ray observations of RX J0822-4300 and Puppis-A 25 2.1 Introduction ................................... 25 2.2 Observations ................................... 27 2.2.1 XMM-Newton Observations ...................... 27 2.2.2 Chandra Observations ......................... 28 2.3 Data Analysis .................................. 29 2.3.1 Spatial Analysis ............................. 29 2.3.2 Spectral Analysis ............................ 31 2.3.3 Timing Analysis ............................ -
A Guide to Hubble Space Telescope Objects
James L. Chen A Guide to Hubble Space Telescope Objects Their Selection, Location, and Signifi cance Graphics by Adam Chen The Patrick Moore The Patrick Moore Practical Astronomy Series More information about this series at http://www.springer.com/series/3192 A Guide to Hubble Space Telescope Objects Their Selection, Location, and Signifi cance James L. Chen Graphics by Adam Chen Author Graphics Designer James L. Chen Adam Chen Gore , VA , USA Baltimore , MD , USA ISSN 1431-9756 ISSN 2197-6562 (electronic) The Patrick Moore Practical Astronomy Series ISBN 978-3-319-18871-3 ISBN 978-3-319-18872-0 (eBook) DOI 10.1007/978-3-319-18872-0 Library of Congress Control Number: 2015940538 Springer Cham Heidelberg New York Dordrecht London © Springer International Publishing Switzerland 2015 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifi cally the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfi lms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specifi c statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication.