Radio Galaxies Dominate the High-Energy Diffuse Gamma-Ray
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An Optical Spectroscopic Survey of the 3CR
A&A 560, A81 (2013) Astronomy DOI: 10.1051/0004-6361/201322842 & c ESO 2013 Astrophysics An optical spectroscopic survey of the 3CR sample of radio galaxies with z < 0.3 V. Implications for the unified model for FR IIs Ranieri D. Baldi1, Alessandro Capetti2, Sara Buttiglione3, Marco Chiaberge4,5,6, and Annalisa Celotti1,7,8 1 SISSA-ISAS, via Bonomea 265, 34136 Trieste, Italy e-mail: [email protected] 2 INAF − Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Italy 3 INAF − Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5 INAF − Istituto di Radio Astronomia, via P. Gobetti 101, 40129 Bologna, Italy 6 Center for Astrophysical Sciences, Johns Hopkins University, 3400 N. Charles Street Baltimore, MD 21218, USA 7 INAF − Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate, Italy 8 INFN − Sezione di Trieste, via Valerio 2, 34127 Trieste, Italy Received 14 October 2013 / Accepted 30 October 2013 ABSTRACT We explore the implications of our optical spectroscopic survey of 3CR radio sources with z < 0.3 for the unified model (UM) for radio-loud AGN, focusing on objects with a “edge-brightened” (FR II) radio morphology. The sample contains 33 high ionization galaxies (HIGs) and 18 broad line objects (BLOs). According to the UM, HIGs, the narrow line sources, are the nuclearly obscured counterparts of BLOs. The fraction of HIGs indicates a covering factor of the circumnuclear matter of 65% that corresponds, adopting a torus geometry, to an opening angle of 50◦ ± 5. -
The Jets in Radio Galaxies
The jets in radio galaxies Martin John Hardcastle Churchill College September 1996 A dissertation submitted in candidature for the degree of Doctor of Philosophy in the University of Cambridge i `Glaucon: ª...But how did you mean the study of astronomy to be reformed, so as to serve our pur- poses?º Socrates: ªIn this way. These intricate traceries on the sky are, no doubt, the loveliest and most perfect of material things, but still part of the visibleworld, and therefore they fall far short of the true realities Ð the real relativevelocities,in theworld of purenumber and all geometrical ®gures, of the movements which carry round the bodies involved in them. These, you will agree, can be conceived by reason and thought, not by the eye.º Glaucon: ªExactly.º Socrates: ªAccordingly, we must use the embroidered heaven as a model to illustrateour study of these realities, just as one might use diagrams exquisitely drawn by some consummate artist like Daedalus. An expert in geometry, meeting with such designs, would admire their ®nished workmanship, but he wouldthink it absurd to studythem in all earnest with the expectation of ®nding in their proportionsthe exact ratio of any one number to another...º ' Ð Plato (429±347 BC), The Republic, trans. F.M. Cornford. ii Contents 1 Introduction 1 1.1 Thisthesis...................................... ... 1 1.2 Abriefhistory................................... .... 2 1.3 Synchrotronphysics........ ........... ........... ...... 4 1.4 Currentobservationalknowledgeintheradio . ............. 5 1.4.1 Jets ........................................ 6 1.4.2 Coresornuclei ................................. 6 1.4.3 Hotspots ..................................... 7 1.4.4 Largescalestructure . .... 7 1.4.5 Theradiosourcemenagerie . .... 8 1.4.6 Observationaltrends . -
Extragalactic Radio Jets
Annual Reviews www.annualreviews.org/aronline Ann. Rev. Astron.Astrophys. 1984. 22 : 319-58 Copyright© 1984 by AnnualReviews Inc. All rights reserved EXTRAGALACTIC RADIO JETS Alan H. Bridle National Radio AstronomyObservatory, 1 Charlottesville, Virginia 22901 Richard A. Perley National Radio Astronomy Observatory, Socorro, New Mexico 87801 1. INTRODUCTION Powerful extended extragalactic radio sources pose two vexing astro- physical problems [reviewed in (147) and (157)]. First, from what energy reservoir do they draw their large radio luminosities (as muchas 10a8 W between 10 MHzand 100 GHz)?Second, how does the active center in the parent galaxy or QSOsupply as muchas 10~4 J in relativistic particles and fields to radio "lobes" up to several hundredkiloparsecs outside the optical object? Newaperture synthesis arrays (68, 250) and new image-processing algorithms (66, 101, 202, 231) have recently allowed radio imaging subarcsecond resolution with high sensitivity and high dynamicrange; as a result, the complexityof the brighter sources has been revealed clearly for the first time. Manycontain radio jets, i.e. narrow radio features between compact central "cores" and more extended "lobe" emission. This review examinesthe systematic properties of such jets and the dues they give to the by PURDUE UNIVERSITY LIBRARY on 01/16/07. For personal use only. physics of energy transfer in extragalactic sources. Wedo not directly consider the jet production mechanism,which is intimately related to the Annu. Rev. Astro. Astrophys. 1984.22:319-358. Downloaded from arjournals.annualreviews.org first problemnoted above--for reviews, see (207) and (251). 1. i Why "’Jets"? Baade & Minkowski(3) first used the term jet in an extragalactic context, describing the train of optical knots extending ,-~ 20" from the nucleus of M87; the knots resemble a fluid jet breaking into droplets. -
Near Infrared Observations of Quasars with Extended Ionized Envelopes
A&A manuscript no. ASTRONOMY (will be inserted by hand later) AND Your thesaurus codes are: 11.01.2; 11.06.2; 11.09.2; 11.16.1; 11.17.3; 13.09.1 ASTROPHYSICS Near infrared observations of quasars with extended ionized envelopes ⋆ I. M´arquez1,2, F. Durret2,3, and P. Petitjean2,3 1 Instituto de Astrof´ısica de Andaluc´ıa (C.S.I.C.), Apartado 3004 , E-18080 Granada, Spain 2 Institut d’Astrophysique de Paris, CNRS, 98bis Bd Arago, F-75014 Paris, France 3 DAEC, Observatoire de Paris, Universit´eParis VII, CNRS (UA 173), F-92195 Meudon Cedex, France Received, ; accepted, Abstract. We have observed a sample of 15 and 8 1. Introduction quasars with redshifts between 0.11 and 0.87 (mean value 0.38) in the J and K’ bands respectively. Eleven of the Attempts to understand properties of active galactic nu- quasars were previously known to be associated with ex- clei (AGN) and their cosmological evolution has led to the tended emission line regions. After deconvolution of the conclusion that the AGN activity as a whole is most likely image, substraction of the PSF when possible, and identi- to be described as a succession of episodic and time lim- fication of companions with the help of HST archive im- ited events happening in most if not all galaxies (Cavaliere ages when available, extensions are seen for at least eleven & Padovani 1989, Collin-Souffrin 1991). The most plausi- quasars. However, average profiles are different from that ble explanation for the onset of activity is fuelling of the of the PSF in only four objects, for which a good fit is nucleus by gas streaming towards the center of the galaxy obtained with an r1/4 law, suggesting that the underlying as a result of interaction, accretion or merging events. -
JRP Angel and HS Stockman.“Optical and Infrared Polarization of Active
Bibliography J.R.P. Angel and H.S. Stockman. \Optical and infrared polarization of active extragalactic objects.". Ann. Rev. Astron. Astrophys., 8:321{361, 1980. S. Ant¶on and I. Browne. \Host galaxies of Flat Radio Spectrum Sources.". In L.O. Takalo and A. SillanpÄaÄa, editors, BL Lac Phenomenon, volume 159 of A.S.P. Conference Series, pages 377{380, 1999. R.R.J. Antonucci. \Polarization of active galactic nuclei and quasars". In M. Kafatos, editor, Supermassive Black Holes, Proceedings of the 3rd George Mason Astrophysics Workshop, pages 26{38. Cambridge Univer- sity Press, Cambridge, 1988. R.R.J. Antonucci and J.S. Ulvestad. \Extended radio emission and the nature of blazars.". Astrophys. J., 294:158{182, 1985. W. Baade. \Polarization in the jet of Messier 87.". Astrophys. J., 123: 550{551, 1956. J. N. Bahcall, S. Kirhakos, D. H. Saxe, and D. P. Schneider. \Hubble Space Telescope Images of a Sample of 20 Nearby Luminous Quasars". Astro- phys. J., 479:642{658, 1997. J.N. Bahcall, S. Kirhakos, D.P. Schneider, R.J. Davis, T.W.B. Muxlow, S.T. Garrington, R.G. Conway, and S.C. Unwin. \HST and MERLIN observations of the jet in 3C 273.". Astrophys. J., Lett., 452:L91{L93, 1995. R. Barvainis. \Free-free emission and the big blue bump in Active Galactic Nuclei.". Astrophys. J., 412:513{523, 1993. 152 BIBLIOGRAPHY S. A. Baum, C. P. O'Dea, G. Giovannini, J. Biretta, W. B. Cotton, S. de Ko®, L. Feretti, D. Golombek, L. Lara, F. D. Macchetto, G. K. Miley, W. B. Sparks, T. -
The Astrology of Space
The Astrology of Space 1 The Astrology of Space The Astrology Of Space By Michael Erlewine 2 The Astrology of Space An ebook from Startypes.com 315 Marion Avenue Big Rapids, Michigan 49307 Fist published 2006 © 2006 Michael Erlewine/StarTypes.com ISBN 978-0-9794970-8-7 All rights reserved. No part of the publication may be reproduced, stored in a retrieval system, or transmitted, in any form or by any means, electronic, mechanical, photocopying, recording, or otherwise, without the prior permission of the publisher. Graphics designed by Michael Erlewine Some graphic elements © 2007JupiterImages Corp. Some Photos Courtesy of NASA/JPL-Caltech 3 The Astrology of Space This book is dedicated to Charles A. Jayne And also to: Dr. Theodor Landscheidt John D. Kraus 4 The Astrology of Space Table of Contents Table of Contents ..................................................... 5 Chapter 1: Introduction .......................................... 15 Astrophysics for Astrologers .................................. 17 Astrophysics for Astrologers .................................. 22 Interpreting Deep Space Points ............................. 25 Part II: The Radio Sky ............................................ 34 The Earth's Aura .................................................... 38 The Kinds of Celestial Light ................................... 39 The Types of Light ................................................. 41 Radio Frequencies ................................................. 43 Higher Frequencies ............................................... -
Not Yet Imagined: a Study of Hubble Space Telescope Operations
NOT YET IMAGINED A STUDY OF HUBBLE SPACE TELESCOPE OPERATIONS CHRISTOPHER GAINOR NOT YET IMAGINED NOT YET IMAGINED A STUDY OF HUBBLE SPACE TELESCOPE OPERATIONS CHRISTOPHER GAINOR National Aeronautics and Space Administration Office of Communications NASA History Division Washington, DC 20546 NASA SP-2020-4237 Library of Congress Cataloging-in-Publication Data Names: Gainor, Christopher, author. | United States. NASA History Program Office, publisher. Title: Not Yet Imagined : A study of Hubble Space Telescope Operations / Christopher Gainor. Description: Washington, DC: National Aeronautics and Space Administration, Office of Communications, NASA History Division, [2020] | Series: NASA history series ; sp-2020-4237 | Includes bibliographical references and index. | Summary: “Dr. Christopher Gainor’s Not Yet Imagined documents the history of NASA’s Hubble Space Telescope (HST) from launch in 1990 through 2020. This is considered a follow-on book to Robert W. Smith’s The Space Telescope: A Study of NASA, Science, Technology, and Politics, which recorded the development history of HST. Dr. Gainor’s book will be suitable for a general audience, while also being scholarly. Highly visible interactions among the general public, astronomers, engineers, govern- ment officials, and members of Congress about HST’s servicing missions by Space Shuttle crews is a central theme of this history book. Beyond the glare of public attention, the evolution of HST becoming a model of supranational cooperation amongst scientists is a second central theme. Third, the decision-making behind the changes in Hubble’s instrument packages on servicing missions is chronicled, along with HST’s contributions to our knowledge about our solar system, our galaxy, and our universe. -
Arxiv:1804.09969V1
Research in Astron. Astrophys. Vol.0 (20xx) No.0, 000–000 Research in http://www.raa-journal.org http://www.iop.org/journals/raa Astronomy and (LATEX: sample.tex; printed on November 9, 2018; 22:51) Astrophysics The pc-scale radio structure of MIR-observed radio galaxies Ye Yuan1,2,3, Minfeng Gu1,2 and Yongjun Chen1,4 1 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China; [email protected] 2 Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, 200030, China 3 Uinversity of Chinese Academy of Sciences,19A Yuquan Road, Beijing 10049, China 4 Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing, JiangSu 210008, China Abstract We investigated the relationship between the accretion process and jet proper- ties by ultilizing the VLBA and mid-infrared (MIR) data for a sample of 45 3CRR radio galaxies selected with a flux density at 178 MHz > 16.4 Jy, 5 GHz VLA core flux den- sity 7 mJy, and MIR observations. The pc-scale radio structure at 5 GHz are presented by using≥ our VLBA observations for 21 sources in February, 2016, the analysis on the archival data for 16 objects, and directly taking the measurements for 8 radio galaxies available in literatures. The accretion mode is constrained from the Eddington ratio with a dividing value of 0.01, which is estimated from the MIR-based bolometric luminosity and the black hole masses. While most FRII radio galaxies have higher Eddington ratio than FRIs, we found that there is indeed no single correspondence between the FR morphol- ogy and accretion mode with eight FRIIs at low accretion and two FRIs at high accretion rate. -
A CHANDRA OBSERVATION of 3C 288— REHEATING the COOL CORE of a 3 Kev CLUSTER from a NUCLEAR OUTBURST at Z = 0.246
A CHANDRA OBSERVATION OF 3C 288— REHEATING THE COOL CORE OF A 3 keV CLUSTER FROM A NUCLEAR OUTBURST at z = 0.246 The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Lal, D. V., R. P. Kraft, W. R. Forman, M. J. Hardcastle, C. Jones, P. E. J. Nulsen, D. A. Evans, J. H. Croston, and J. C. Lee. “ A CHANDRA OBSERVATION OF 3C 288—REHEATING THE COOL CORE OF A 3 keV CLUSTER FROM A NUCLEAR OUTBURST at z = 0.246 .” The Astrophysical Journal 722, no. 2 (October 4, 2010): 1735–1743. © 2010 The American Astronomical Society As Published http://dx.doi.org/10.1088/0004-637x/722/2/1735 Publisher IOP Publishing Version Final published version Citable link http://hdl.handle.net/1721.1/95820 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal, 722:1735–1743, 2010 October 20 doi:10.1088/0004-637X/722/2/1735 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A CHANDRA OBSERVATION OF 3C 288—REHEATING THE COOL CORE OF A 3 keV CLUSTER FROM A NUCLEAR OUTBURST at z = 0.246 D. V. Lal1, R. P. Kraft1, W. R. Forman1, M. J. Hardcastle2, C. Jones1,P.E.J.Nulsen1,D.A.Evans1,3, J. H. Croston4, and J. C. Lee1 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 2 School of Physics, Astronomy, and Mathematics, University of Hertfordshire, Hatfield, AL 10 9AB, UK 3 MIT Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 4 School of Physics and Astronomy, University of Southampton, Southampton, SO17 1SJ, UK Received 2010 April 27; accepted 2010 August 25; published 2010 October 4 ABSTRACT We present results from a 42 ks Chandra/ACIS-S observation of the transitional FR I/FR II radio galaxy 3C 288 at z = 0.246. -
National Radio Astronomy Observatory Observing
NATIONAL RADIO ASTRONOMY OBSERVATORY OBSERVING SUMMARY-1989 STATISTICS February 1990 Cover The Radio Galaxy Fornax A The cover photograph is a superposition of the VLA radio emission (shown as red) from the radio galaxy Fornax A and the visible light in the vicinity of NGC 1316 (shown as blue-white). The two main radio emitting lobes are produced by relativistic electrons in magnetic fields which have been transported hundreds of thousands of light years outward from the elliptical galaxy NGC 1316 which lies between the two regions. The energy for the relativistic flow apparently was provided by the gravitational capture of small galaxies by NGC 1316. The shock waves and trails of the infallen galaxies produce the features in the radio lobes seen as filaments and rings. The small galaxy near NGC 1316 may soon be captured. Observation details: Observers: E. Fomalont (NRAO), R. Ekers (Australia Telescope), K. Ebneter and W. Van Breugel (U. California) Frequency of 1.384 GHz; five hours of D-configuration and five hours of C-configuration Resolution of 15"; field of view is 60' x 40' NATIONAL RADIO ASTRONOMY OBSERVATORY OBSERVING SUMMARY 1989 STATISTICS FEBRUARY 1990 SOME HIGHLIGHTS OF THE 1989 RESEARCH PROGRAM A second Einstein Ring has been identified from new A-configuration VLA observations of MG1652+138, the second candidate for an Einstein ring gravitational lens system to be selected from the MIT-Green Bank 5 GHz survey. Optical images and spectra established the redshift of a faint blue quasar between the two radio sources, while the VLA results have both detected the quasar core at its optical location and improved the ring image quality. -
B Gg Revisited: the Environments of Low-Excitation Radio Galaxies And
Astronomy & Astrophysics manuscript no. 0605 December 17, 2018 (DOI: will be inserted by hand later) Research Note Bgg revisited: The environments of low-excitation radio galaxies and unified models Martin J. Hardcastle Department of Physics, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK ([email protected]) Version of December 17, 2018 Abstract. Recent measurements of the galaxy clustering environments around intermediate-redshift radio sources have suggested a systematic environmental difference between radio galaxies and radio-loud quasars, in contradic- tion to the predictions of simple unified models for the two classes of object. I show that the apparent difference arises mainly as a result of the properties of low-excitation radio galaxies included in the radio-galaxy sam- ple, which tend to lie in significantly richer environments. The environmental properties of high-excitation radio galaxies and quasars are statistically consistent in the redshift range 0.15 <z< 0.4, as unified models would predict. Key words. galaxies: active – galaxies: quasars: general – galaxies: clusters: general – radio continuum: galaxies 1. Introduction achive good statistics at high redshifts (Barr et al. 2003), at lower redshifts simple Bgg determinations seem likely In unified models for powerful radio galaxies and radio- to be able to provide a statistical measure of the environ- loud quasars (Scheuer 1987, Barthel 1987, 1989) isotropic ments of different classes of source. properties of the two classes of objects, such as their Recently Harvanek et al. (2001: hereafter HESR) have clustering environments, should be statistically identical. carried out a large systematic study of the clustering However, the classical unified models work best at high properties of 3CR (Spinrad et al. -
II Cluster Catalog Donald J
Dartmouth College Dartmouth Digital Commons Open Dartmouth: Faculty Open Access Articles 2008 The ARPSW Survey. VII. The ARPSW ‐II Cluster Catalog Donald J. Horner NASA Goddard Space Flight Center Eric S. Perlman University of Maryland-Baltimore County Harald Ebeling Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI Laurence Jones University of Birmingham Caleb A. Scharf Columbia University See next page for additional authors Follow this and additional works at: https://digitalcommons.dartmouth.edu/facoa Part of the Astrophysics and Astronomy Commons Recommended Citation Horner, Donald J.; Perlman, Eric S.; Ebeling, Harald; Jones, Laurence; Scharf, Caleb A.; Wegner, Gary; Malkan, Matthew; and Maughan, Ben, "The AW RPS Survey. VII. The AW RPS‐II Cluster Catalog" (2008). Open Dartmouth: Faculty Open Access Articles. 3497. https://digitalcommons.dartmouth.edu/facoa/3497 This Article is brought to you for free and open access by Dartmouth Digital Commons. It has been accepted for inclusion in Open Dartmouth: Faculty Open Access Articles by an authorized administrator of Dartmouth Digital Commons. For more information, please contact [email protected]. Authors Donald J. Horner, Eric S. Perlman, Harald Ebeling, Laurence Jones, Caleb A. Scharf, Gary Wegner, Matthew Malkan, and Ben Maughan This article is available at Dartmouth Digital Commons: https://digitalcommons.dartmouth.edu/facoa/3497 The Astrophysical Journal Supplement Series, 176:374Y413, 2008 June # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE WARPS SURVEY. VII. THE WARPS-II CLUSTER CATALOG Donald J. Horner,1 Eric S. Perlman,2,3 Harald Ebeling,4 Laurence R. Jones,5 Caleb A. Scharf,6 Gary Wegner,7 Matthew Malkan,8 and Ben Maughan9 Received 2007 November 19; accepted 2007 December 26 ABSTRACT We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters.