DOCSLIB.ORG

Unification of Active Galactic Nuclei at X-Rays and Soft Gamma-Rays

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Unification of Active Galactic Nuclei at X-Rays and Soft Gamma-Rays Unification of Active Galactic Nuclei at X-rays and soft gamma-rays Volker Beckmann Laboratoire AstroParticule et Cosmologie (APC) - Paris, France Habilitation à diriger des recherches présentée à l’Université Paris 7 - Denis Diderot tel-00601042, version 1 - 16 Jun 2011 Soutenue le 10 septembre 2010 devant le jury composé de: Pierre Binétruy President Peter von Ballmoos Rapporteur Chris Done Rapporteur Catherine Boisson Rapporteur (interne) Jérôme Rodriguez Examinateur Etienne Parizot Examinateur . tel-00601042, version 1 - 16 Jun 2011 3 tel-00601042, version 1 - 16 Jun 2011 4 tel-00601042, version 1 - 16 Jun 2011 Figure 1: The 12 meter dome at the Observatoire de Paris, constructed 1845-1847 on the northern tower of the institute when François Arago was its director. Figure from Arago & Barral (1854) Contents 1 CURRICULUM VITAE 7 1.1 PersonalInformation .... ...... ..... ...... ...... .. ..... 7 1.2 Education ....................................... 7 1.3 Workhistory ..................................... 8 1.4 Experience and achievements . ....... 8 2 TEACHING AND PUBLIC OUTREACH 11 2.1 Teaching........................................ 11 2.1.1 Stellar Astrophysics . 11 2.1.2 Extragalactic Astronomy and Cosmology . ....... 11 2.2 Supervision of students . ...... 12 2.2.1 HamburgUniversity ...... ..... ...... ...... ..... 12 2.2.2 ISDC Data Centre for Astrophysics . ..... 12 2.2.3 FrançoisAragoCentre . 12 2.3 Refereeing...................................... 13 2.4 Conference and meeting organisation . .......... 13 2.5 PublicOutreach.................................. 14 2.6 Pressreleases ................................... 14 3 SUMMARY,RELEVANCEANDORIGINALITYOFRESEARCH 17 tel-00601042, version 1 - 16 Jun 2011 4 RESEARCH 19 4.1 From Welteninseln toAGN............................... 19 4.2 From optical to X-ray observations of AGN . ......... 21 4.3 The AGN phenomenon and the Unified Model . ...... 23 4.4 Verifying the unified model through evolutionary tests . ................ 28 4.4.1 Numbercounts ................................. 29 4.4.2 The V/Vmax test................................. 30 4.4.3 The luminosity function . 31 4.4.4 Local luminosity function of optically selected AGN . ............ 32 4.5 Testing Unification on X-ray selected BL Lac Objects . ............. 37 4.6 Early INTEGRAL AGNObservations ......................... 45 4.6.1 The INTEGRAL Mission............................ 45 4.6.2 The hard X-ray spectrum of AGN . 50 4.6.3 The quasars MR 2251-178 and 3C 273 . 53 4.6.4 TheSeyfert2NGC4388.... ..... ...... ...... ..... .. 54 5 6 CONTENTS 4.6.5 The Seyfert 1.5 galaxy NGC 4151 . 58 4.6.6 The First INTEGRAL AGNCatalogue ..................... 60 4.7 AGN Population Studies at Hard X-rays . ........ 62 4.7.1 The Hard X-ray 20–40 keV Luminosity Function . ....... 62 4.7.2 Hard X-ray variability of AGN . 66 4.7.3 The Second INTEGRAL AGNCatalogue ................... 74 4.7.4 The special case of MCG–05–23–016 . 78 4.8 ConnectiontoGamma-rays. ..... 82 4.8.1 ROSAT selected Gamma-ray Blazars . 82 4.8.2 The Fermi view on hard X-ray blazars . ..... 87 4.8.3 The non-blazar population seen by Fermi . ....... 90 5 CONCLUSION & OUTLOOK 93 5.1 Conclusions..................................... 93 5.1.1 Progress concerning the unified scheme . ....... 93 5.1.2 Impact on studies of the cosmic X-ray background . ......... 94 5.1.3 Outlining the connection to the gamma-rays . ......... 94 5.2 Openquestions ................................... 94 5.3 Futureprojects .................................. 96 5.3.1 Research .................................... 96 5.3.2 Enabling science: the François Arago Centre . ......... 98 6 LISTOFPUBLICATIONSANDCONFERENCECONTRIBUTIONS 101 6.1 Articles in refereed international journals . .............. 101 6.2 Invited talks at international conferences . .............. 105 6.3 Refereed conference proceedings . ......... 105 6.4 Non-refereed conference proceedings . .......... 107 6.5 Other non-refereed publications . ......... 108 6.6 Communications in conferences . ....... 114 6.6.1 Talks in international conferences . ........ 114 6.6.2 Posters in international conferences . ......... 116 tel-00601042, version 1 - 16 Jun 2011 6.7 Seminars (only after 2005) . 117 6.8 Thesis and dissertation . 118 6.9 Five significant publications . ........ 118 6.9.1 The HRX-BL Lac sample - Evolution of BL Lac objects . ....... 119 6.9.2 TheFirstINTEGRALAGNCatalog. 132 6.9.3 The Hard X-ray 20-40 keV AGN Luminosity Function . ....... 144 6.9.4 Hard X-ray variability of active galactic nuclei . ............ 155 6.9.5 TheSecondINTEGRALAGNCatalogue . 165 BIBLIOGRAPHY 189 ACKNOWLEDGMENTS 207 Chapter 1 CURRICULUM VITAE 1.1 Personal Information Name: Volker BECKMANN Citizenship: German Date of Birth: March 7, 1968 in Hamburg (Germany) Present Position: Chercheur au CNRS based at the APC (UMR 7164) Address: APC, François Arago Centre, Université Paris Diderot, 10 rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France Telephone: +33 (0)157 27 60 81 Fax: +33 (0)157 27 60 71 E-mail: [email protected] 1.2 Education tel-00601042, version 1 - 16 Jun 2011 1996/2001 PhD at University of Hamburg, Hamburger Sternwarte in Astrophysics. Title: Evolutionary behaviour of AGN - in- vestigations on BL Lac objects and Seyfert II galaxies. Referees: Prof. Dr. Dieter Reimers (Hamburger Stern- warte), and Prof. Dr. Laura Maraschi (Osservatorio Astro- nomico di Brera). PhD defended on January 12, 2001. Grade: magna cum laude 1993/96 Diplom (Master) in Physics at the University of Hamburg. Thesis: X-ray spectral index of RASS-AGN. Referees: Prof. Dr. Sjur Refsdal and Prof. Dr. Dieter Reimers (Hamburger Sternwarte). Grade: cum laude 1989/93 Vordiplom (Bachelor) in Physics at the University of Hamburg 7 8 CHAPTER 1. CURRICULUM VITAE 1.3 Work history since September 2009 Chercheur CNRS, working for the APC laboratory (Uni- versité Paris 7 - Denis Diderot). In charge of the François Arago Centre, a data and computing centre for space- and ground-based astroparticle physics. April 2007 - Aug. 2009 Collaborateur Scientifique of the University of Geneva, working at the ISDC Data Centre for Astrophysics. Op- erations coordinator and instrument specialist for the spec- trograph SPI of the INTEGRAL mission at the ISDC. July 2007 until August 2009 also INTEGRAL responsible sci- entist. since April 2007 Adjunct Assistant Professor at the University of Maryland Baltimore County (UMBC). Oct. 2003 - March 2007 Working as a Research Associate for UMBC at NASA/Goddard Space Flight Center. Since July 2006 head of the INTEGRAL guest observer facility at NASA. Support of guest investigators, preparation and administra- tion of INTEGRAL budget, analysis and interpretation of INTEGRAL data, maintaining the INTEGRAL/HEASARC archive. Since August 2006 Assistant Research Professor at UMBC. Feb. 2001 – Sep. 2003 Working for the IAAT (University of Tübingen) at the ISDC. Developing and integrating analysis software for INTEGRAL, support of operations of the INTEGRAL satel- lite. May – July 2000 Working at the Osservatorio Astronomico di Brera in Mi- lan, financed by an Italian grant (CNR). Apr.-Sep. 1999 Working at the Osservatorio Astronomico di Brera, fi- tel-00601042, version 1 - 16 Jun 2011 nanced by the Deutsche Akademische Austauschdienst (DAAD). 1996 – 2000 Scientific assistant researcher at the Hamburger Stern- warte, financed by the Deutsche Forschungsgemeinschaft (DFG). 1.4 Experience and achievements Teaching experience Two full courses as assistant research professor at the physics department of the the University of Maryland for physics master students. In addition, teaching (as replacement) at the University of Geneva. See Section 2.1. 1.4. EXPERIENCE AND ACHIEVEMENTS 9 Supervising experience Supervision or co-supervision of 8 students (among which 2 PhD students). See Section 2.2. Publications 60 publications in international refereed journals, including 17 as lead author. 22 publications in international refereed conference proceedings including 7 as lead author. 28 publications in non-refereed conference proceedings including 12 as lead author. 55 Astronomer’s Telegrams including 3 as lead author. 19 GRB Circular Network (GCN) reports including 7 as lead author. Conferences, seminars, and oral communications 25 talks in international conferences of which 3 were invited review talks. 17 poster presentations at international conferences. ca. 30 seminars given in various institutions around the world. Collaborations Working in several institutes in Europe and in the U.S. I had the opportunity to get involved in many scientific collaborations. Here the most productive collaborations are the ones with colleagues at those institutes where I worked, i.e. Hamburg Observatory, ISDC Data Centre for Astrophysics, Osservato- rio Astronomico di Brera, and NASA’s Goddard Space Flight Center. My main collaborators over the tel-00601042, version 1 - 16 Jun 2011 years were and are still: Thierry J.-L. Courvoisier (ISDC, Versoix) Roberto Della Ceca (Osservatorio Astronomico di Brera, Milan) Dieter Engels (Hamburger Sternwarte, Hamburg) Neil Gehrels (NASA/GSFC, Washington D.C.) Julien Malzac (CESR, Toulouse) Ada Paizis (INAF/IASF-Milan) Dieter Reimers (Hamburger Sternwarte, Hamburg) Claudio Ricci (ISDC, Versoix) Jérôme Rodriguez (CEA/SAp, Saclay) Chris R. Shrader (NASA/GSFC, Washington D.C.) Simona Soldi (CEA/SAp, Saclay) Jack Tueller (NASA/GSFC, Washington D.C.) Marc Türler (ISDC, Versoix) Anna Wolter (Osservatorio Astronomico di Brera, Milan) Olaf Wucknitz (Argelander-Institut
Load more

Recommended publications
  • Beyond Einstein... Are We All Afraid of the Truth?
    smw-genart-02-06 Beyond Einstein ... Are we all afraid of the Truth? Sanjay M Wagh Central India Research Institute, Post Box 606, Laxminagar, Nagpur 440 022, India ∗ (Dated: March 20, 2006) Abstract The power-point presentation [1] provided herein shows exactly why Einstein’s field equations of his general relativity are based on an illogical approach to representing the observable world. Einstein had, in fact, discarded these equations way back in 1928 when he had began his solitary search for a unified field theory. However, the rest of us learned, taught, and also put too much faith for too long (for more than seventy years) in an illogical approach to representing the observable world. Consequently, we have developed great reluctance, resulting from dogmatic perceptions, prestige, reputation, ..., that is holding us back from orienting ourselves in the “right” direction to the understanding of the observable phenomena. This raises the question mentioned in the title: Are we all afraid of the Truth? Rhetorically speaking, we could then also ask: are we all afraid of Virginia Woolf? In the sequel, I also illustrate my approach to going Beyond Einstein for developing an appropriate mathematical framework for the fundamental physical ideas behind the General Principle of Relativity, for the unification of fundamental arXiv:physics/0603149v1 [physics.gen-ph] 20 Mar 2006 physical interactions and, hence, for a theory of everything. ∗Electronic address: cirinag˙[email protected] 1 The title of this article may appear only as an eye-catching one to some, repelling one to some others, a thought provoking one to few others ..
    [Show full text]
  • Polarimetric Properties of Blazars Caught by the WEBT
    galaxies Review Polarimetric Properties of Blazars Caught by the WEBT Claudia M. Raiteri * and Massimo Villata INAF, Osservatorio Astrofisico di Torino, via Osservatorio 20, I-10025 Pino Torinese, Italy; [email protected] * Correspondence: [email protected] Abstract: Active galactic nuclei come in many varieties. A minority of them are radio-loud, and exhibit two opposite prominent plasma jets extending from the proximity of the supermassive black hole up to megaparsec distances. When one of the relativistic jets is oriented closely to the line of sight, its emission is Doppler beamed and these objects show extreme variability properties at all wavelengths. These are called “blazars”. The unpredictable blazar variability, occurring on a continuous range of time-scales, from minutes to years, is most effectively investigated in a multi-wavelength context. Ground-based and space observations together contribute to give us a comprehensive picture of the blazar emission properties from the radio to the g-ray band. Moreover, in recent years, a lot of effort has been devoted to the observation and analysis of the blazar polarimetric radio and optical behaviour, showing strong variability of both the polarisation degree and angle. The Whole Earth Blazar Telescope (WEBT) Collaboration, involving many tens of astronomers all around the globe, has been monitoring several blazars since 1997. The results of the corresponding data analysis have contributed to the understanding of the blazar phenomenon, particularly stressing the viability of a geometrical interpretation of the blazar variability. We review here the most significant polarimetric results achieved in the WEBT studies. Keywords: active galactic nuclei; blazars; jets; polarimetry Citation: Raiteri, C.M.; Villata, M.
    [Show full text]
  • 1 Introduction
    Iranian Journal of Astronomy and Astrophysics Iranian Journal of Vol. 1, No. 1, 2013 Astronomy and © Available online at http://journals.du.ac.ir Astrophysics Evaluation of New MOND Interpolating Function with Rotation Curves of Galaxies Hosein Haghi1 ·Hamed Ghasemi2 ·HongSheng Zhao3 1 Department of Physics, Institute for Advanced Studies in Basic Sciences (IASBS), P.O. Box 11365-9161, Zanjan, Iran; email: [email protected] 2 Department of Physics, Zanjan University, Zanjan, Iran 3 SUPA, School of Physics and Astronomy, University of St. Andrews, KY16 9SS, UK Abstract. The rotation curves of a sample of 46 low- and high-surface brightness galaxies are considered in the context of Milgrom's modified dynamics (MOND) to test a new interpolating function proposed by Zhao et al. (2010) [1] and compare with the results of simple interpolating function. The predicted rotation curves are calculated from the total baryonic matter based on the B-band surface photometry, and the observed distribution of neutral hydrogen, in which the one adjustable parameter is the stellar mass-to-light ratio. The predicted rotation curves generally agree with the observed curves for both interpolating functions. We show that the fitted M=L in the B-band correlates with B-V color in the sense expected from what we know about stellar population synthesis models. Moreover, the mass-to-light ratios of MOND with new interpolating function is in consistent with scaled Salpeter's initial mass function of the SPS scheme, while those of MOND with simple interpolating function favor Kroupa IMF. Keywords: ISM: molecules, ISM: structure, instabilities 1 Introduction The rotation curves of spiral galaxies provide an accurate determination of the radial force distribution in spiral galaxies.
    [Show full text]
  • Unification of the Maxwell- Einstein-Dirac Correspondence
    Unification of the Maxwell- Einstein-Dirac Correspondence The Origin of Mass, Electric Charge and Magnetic Spin Author: Wim Vegt Country: The Netherlands Website: http://wimvegt.topworld.center Email: [email protected] Calculations: All Calculations in Mathematica 11.0 have been printed in a PDF File Index 1 “Unified 4-Dimensional Hyperspace 5 Equilibrium” beyond Einstein 4-Dimensional, Kaluza-Klein 5-Dimensional and Superstring 10- and 11 Dimensional Curved Hyperspaces 1.2 The 4th term in the Unified 4-Dimensional 12 Hyperspace Equilibrium Equation 1.3 The Impact of Gravity on Light 15 2.1 EM Radiation within a Cartesian Coordinate 23 System in the absence of Gravity 2.1.1 Laser Beam with a Gaussian division in the x-y 25 plane within a Cartesian Coordinate System in the absence of Gravity 2.2 EM Radiation within a Cartesian Coordinate 27 System under the influence of a Longitudinal Gravitational Field g 2.3 The Real Light Intensity of the Sun, measured in 31 our Solar System, including Electromagnetic Gravitational Conversion (EMGC) 2.4 The Boundaries of our Universe 35 2.5 The Origin of Dark Matter 37 3 Electromagnetic Radiation within a Spherical 40 Coordinate System 4 Confined Electromagnetic Radiation within a 42 Spherical Coordinate System through Electromagnetic-Gravitational Interaction 5 The fundamental conflict between Causality and 48 Probability 6 Confined Electromagnetic Radiation within a 51 Toroidal Coordinate System 7 Confined Electromagnetic Radiation within a 54 Toroidal Coordinate System through Electromagnetic-Gravitational
    [Show full text]
  • Southern Arp - AM # Order
    Southern Arp - AM # Order A B C D E F G H I J 1 AM # Constellation Object Name RA DEC Mag. Size Uranom. Uranom. Millenium 2 1st Ed. 2nd Ed. 3 AM 0003-414 Phoenix ESO 293-G034 00h06m19.9s -41d30m00s 13.7 3.2 x 1.0 386 177 430 Vol I 4 AM 0006-340 Sculptor NGC 10 00h08m34.5s -33d51m30s 13.3 2.4 x 1.2 350 159 410 Vol I 5 AM 0007-251 Sculptor NGC 24 00h09m56.5s -24d57m47s 12.4 5.8 x 1.3 305 141 366 Vol I 6 AM 0011-232 Cetus NGC 45 00h14m04.0s -23d10m55s 11.6 8.5 x 5.9 305 141 366 Vol I 7 AM 0027-333 Sculptor NGC 134 00h30m22.0s -33d14m39s 11.4 8.5 x 2.0 351 159 409 Vol I 8 AM 0029-643 Tucana ESO 079- G003 00h32m02.2s -64d15m12s 12.6 2.7 x 0.4 440 204 409 Vol I 9 AM 0031-280B Sculptor NGC 150 00h34m15.5s -27d48m13s 12 3.9 x 1.9 306 141 387 Vol I 10 AM 0031-320 Sculptor NGC 148 00h34m15.5s -31d47m10s 13.3 2 x 0.8 351 159 387 Vol I 11 AM 0033-253 Sculptor IC 1558 00h35m47.1s -25d22m28s 12.6 3.4 x 2.5 306 141 365 Vol I 12 AM 0041-502 Phoenix NGC 238 00h43m25.7s -50d10m58s 13.1 1.9 x 1.6 417 177 449 Vol I 13 AM 0045-314 Sculptor NGC 254 00h47m27.6s -31d25m18s 12.6 2.5 x 1.5 351 176 386 Vol I 14 AM 0050-312 Sculptor NGC 289 00h52m42.3s -31d12m21s 11.7 5.1 x 3.6 351 176 386 Vol I 15 AM 0052-375 Sculptor NGC 300 00h54m53.5s -37d41m04s 9 22 x 16 351 176 408 Vol I 16 AM 0106-803 Hydrus ESO 013- G012 01h07m02.2s -80d18m28s 13.6 2.8 x 0.9 460 214 509 Vol I 17 AM 0105-471 Phoenix IC 1625 01h07m42.6s -46d54m27s 12.9 1.7 x 1.2 387 191 448 Vol I 18 AM 0108-302 Sculptor NGC 418 01h10m35.6s -30d13m17s 13.1 2 x 1.7 352 176 385 Vol I 19 AM 0110-583 Hydrus NGC
    [Show full text]
  • Arxiv:0808.0461V1 [Astro-Ph] 4 Aug 2008
    Draft version November 25, 2018 A Preprint typeset using LTEX style emulateapj v. 08/22/09 X-RAY SPECTRAL PROPERTIES OF THE BAT AGN SAMPLE Lisa M. Winter1, Richard F. Mushotzky2, Christopher S. Reynolds1, Jack Tueller2 Draft version November 25, 2018 ABSTRACT The 9-month SWIFT Burst Alert Telescope (BAT) catalog provides the first unbiased (NH < 1024 cm−2) look at local (<z>=0.03) AGN. In this paper, we present the collected X-ray properties (0.3 – 12 keV) for the 153 AGN detected. In addition, we examine the X-ray properties for a complete sample of non-beamed sources, above the Galactic plane (b 15◦). Of these, 45% are best fit by simple power law models while 55% require the more complex partial≥ covering model. One of our goals was to determine the fraction of “hidden” AGN, which we define as sources with scattering fractions 0.03 and ratios of soft to hard X-ray flux 0.04. We found that “hidden” AGN constitute a high percentage≤ of the sample (24%), proving that they≤ are a very significant portion of local AGN. Further, we find that the fraction of absorbed sources does increase at lower unabsorbed 2–10 keV luminosities, as well as accretion rates. This suggests that the unified model requires modification to include luminosity dependence, as suggested by models such as the ’receding torus’ model (Lawrence 1991). Some of the most interesting results for the BAT AGN sample involve the host galaxy properties. We found that 33% are hosted in peculiar/irregular galaxies and only 5/74 hosted in ellipticals.
    [Show full text]
  • Early-Type Galaxies in the Antlia Cluster: Catalogue and Isophotal Analysis
    MNRAS 477, 1760–1771 (2018) doi:10.1093/mnras/sty611 Advance Access publication 2018 March 7 Early-type galaxies in the Antlia cluster: catalogue and isophotal analysis Juan P. Calderon,´ 1,2,3‹ Lilia P. Bassino,1,2,3 Sergio A. Cellone1,3,4 and Mat´ıas Gomez´ 5 1Consejo Nacional de Investigaciones Cient´ıficas y Tecnicas,´ Rivadavia 1917, Buenos Aires, Argentina 2Instituto de Astrof´ısica de La Plata (CCT La Plata - CONICET - UNLP), La Plata, Argentina 3Facultad de Ciencias Astronomicas´ y Geof´ısicas, Universidad Nacional de La Plata, Paseo del Bosque, B1900FWA La Plata, Argentina Downloaded from https://academic.oup.com/mnras/article-abstract/477/2/1760/4924514 by Universidad Andres Bello user on 28 May 2019 4Complejo Astronomico´ El Leoncito (CONICET - UNLP - UNC - UNSJ), San Juan, Argentina 5Departamento de Ciencias F´ısicas, Facultad de Ciencias Exactas, Universidad Andres Bello, Santiago, Chile Accepted 2018 February 26. Received 2018 February 26; in original form 2017 December 14 ABSTRACT We present a statistical isophotal analysis of 138 early-type galaxies in the Antlia cluster, located at a distance of ∼ 35 Mpc. The observational material consists of CCD images of four 36 × 36 arcmin2 fields obtained with the MOSAIC II camera at the Blanco 4-m telescope at Cerro Tololo Interamerican Observatory. Our present work supersedes previous Antlia studies in the sense that the covered area is four times larger, the limiting magnitude is MB ∼−9.6 mag, and the surface photometry parameters of each galaxy are derived from Sersic´ model fits extrapolated to infinity. In a companion previous study we focused on the scaling relations obtained by means of surface photometry, and now we present the data, on which the previous paper is based, the parameters of the isophotal fits as well as an isophotal analysis.
    [Show full text]
  • X-Ray Spectral Parameters for a Sample of 95 Active Galactic Nuclei
    Accepted for publication in Astrophysics and Space Science X-Ray Spectral Parameters for a Sample of 95 Active Galactic Nuclei A.A. Vasylenko1, V.I. Zhdanov2, E.V. Fedorova2 1Main Astronomical Observatory NAS of Ukraine, Kyiv, Ukraine e-mail: [email protected] 2Taras Shevchenko National University of Kyiv, Ukraine We present a broadband X-ray analysis of a new homogeneous sample of 95 active galactic nuclei (AGN) from the 22-month Swift/BAT all-sky survey. For this sample we treated jointly the X-ray spectra observed by XMM-Newton and INTEGRAL missions for the total spectral range of 0.5-250 keV. Photon index Г, relative reflection R, equivalent width of Fe Kα line EWFeK, hydrogen column density NH, exponential cut-off energy Ec and intrinsic luminosity Lcorr are determined for all objects of the sample. We investigated correlations Г–R, EWFeK– Lcorr, Г–Ec, EWFeK–NH. Dependence "Г – R" for Seyfert ½ galaxies has been investigated separately. We found that the relative reflection parameter at low power-law indexes for Seyfert 2 galaxies is systematically higher than for Seyfert 1 ones. This can be related to an increasing contribution of the reflected radiation from the gas-dust torus. Our data show that there exists some anticorrelation between EWFeK and Lcorr, but it is not strong. We have not found statistically significant deviations from the AGN Unified Model. Key words: galaxies: Seyfert – X-rays: galaxies: active – galaxies 1. INTRODUCTION It is widely accepted today that the variety of observational appearances of AGNs can be divided in two big groups: those caused by physical conditions in particular AGN, and those due to geometrical effects of the AGN orientation with respect to the line-of-sight.
    [Show full text]
  • Fermi Large Area Telescope Second Source Catalog the Fermi LAT Collaboration
    Revision: 3455: Last update: 2011-07-09 23:47:14 - 0700 Fermi Large Area Telescope Second Source Catalog The Fermi LAT Collaboration ABSTRACT This is a pre-submission draft of the paper provided to document the public release of the 2FGL catalog through the FSSC. The draft will be replaced soon by the version that is submitted to ApJS and posted on the arXiv. We present the second catalog of high-energy γ-ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi),derivedfromdatatakenduringthefirst 24 months of the science phase of the mission, which began on 2008 August 4. Source detection is based on the average flux over the 24-monthperiod.The Second Fermi-LAT catalog (2FGL) includes source location regions, defined in terms of elliptical fits to the 95% confidence regions and spectral fits in terms of power-law, power-law-with-exponential-cutoff, or log-normal forms. Also in- cluded are flux measurements in 5 energy bands for each source and monthly light curves. Twelve sources in the catalog are modeled as spatially extended. We provide a detailed comparison of the results from this catalog with those from the first Fermi-LAT catalog (1FGL). Although the diffuse Galactic and isotropic models used in the 2FGL analysis are improved compared to the 1FGL catalog, we attach caution flags to 162 of the sources to indicate possible confusion with residual imperfections in the diffuse model. The 2FGL catalogcontains1873 sources detected and characterized in the 100 MeV to 100 GeV range of which we consider 127 as being firmly identified and 1174 as being reliably associated with counterparts of known or likely γ-ray-producing source classes.
    [Show full text]
  • A New Sample of Buried Active Galactic Nuclei Selected from The
    TO APPEAR IN The Astrophysical Journal. Preprint typeset using LATEX style emulateapj v. 08/22/09 A NEW SAMPLE OF BURIED ACTIVE GALACTIC NUCLEI SELECTED FROM THE SECOND XMM-NEWTON SERENDIPITOUS SOURCE CATALOGUE KAZUHISA NOGUCHI,YUICHI TERASHIMA, AND HISAMITSU AWAKI Department of Physics, Ehime University, Matsuyama, Ehime 790-8577, Japan To appear in The Astrophysical Journal. ABSTRACT We present the results of X-ray spectral analysis of 22 active galactic nuclei (AGNs) with a small scattering fraction selected from the Second XMM-Newton Serendipitous Source Catalogue using hardness ratios. They are candidates of buried AGNs, since a scattering fraction, which is a fraction of scattered emission by the circumnuclear photoionized gas with respect to direct emission, can be used to estimate the size of the opening part of an obscuring torus. Their X-ray spectra are modeled by a combination of a power law with a photon index of 1.5−2 absorbed by a column density of ∼ 1023−24 cm−2, an unabsorbed power law, narrow Gaussian lines, and some additional soft components. We find that scattering fractions of 20 among 22 objects are less than a typical value (∼ 3%) for Seyfert2s observed so far. In particular, those of eight objects are smaller than 0.5%, which are in the range for buried AGNs found in recent hard X-ray surveys. Moreover, [O III] λ5007 luminosities at given X-ray luminosities for some objects are smaller than those for Seyfert2s previouslyknown. This fact could be interpreted as a smaller size of optical narrow emission line regions produced in the opening direction of the obscuring torus.
    [Show full text]
  • The Third Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope M
    The Astrophysical Journal, 810:14 (34pp), 2015 September 1 doi:10.1088/0004-637X/810/1/14 © 2015. The American Astronomical Society. All rights reserved. THE THIRD CATALOG OF ACTIVE GALACTIC NUCLEI DETECTED BY THE FERMI LARGE AREA TELESCOPE M. Ackermann1, M. Ajello2, W. B. Atwood3, L. Baldini4, J. Ballet5, G. Barbiellini6,7, D. Bastieri8,9, J. Becerra Gonzalez10,11, R. Bellazzini12, E. Bissaldi13, R. D. Blandford14, E. D. Bloom14, R. Bonino15,16, E. Bottacini14, T. J. Brandt10, J. Bregeon17, R. J. Britto18, P. Bruel19, R. Buehler1, S. Buson8,9, G. A. Caliandro14,20, R. A. Cameron14, M. Caragiulo13, P. A. Caraveo21, B. Carpenter10,22, J. M. Casandjian5, E. Cavazzuti23, C. Cecchi24,25, E. Charles14, A. Chekhtman26, C. C. Cheung27, J. Chiang14, G. Chiaro9, S. Ciprini23,24,28, R. Claus14, J. Cohen-Tanugi17, L. R. Cominsky29, J. Conrad30,31,32,70, S. Cutini23,24,28,R.D’Abrusco33,F.D’Ammando34,35, A. de Angelis36, R. Desiante6,37, S. W. Digel14, L. Di Venere38, P. S. Drell14, C. Favuzzi13,38, S. J. Fegan19, E. C. Ferrara10, J. Finke27, W. B. Focke14, A. Franckowiak14, L. Fuhrmann39, Y. Fukazawa40, A. K. Furniss14, P. Fusco13,38, F. Gargano13, D. Gasparrini23,24,28, N. Giglietto13,38, P. Giommi23, F. Giordano13,38, M. Giroletti34, T. Glanzman14, G. Godfrey14, I. A. Grenier5, J. E. Grove27, S. Guiriec10,2,71, J. W. Hewitt41,42, A. B. Hill14,43,68, D. Horan19, R. Itoh40, G. Jóhannesson44, A. S. Johnson14, W. N. Johnson27, J. Kataoka45,T.Kawano40, F. Krauss46, M. Kuss12, G. La Mura9,47, S. Larsson30,31,48, L.
    [Show full text]
  • Bright Star Double Variable Globular Open Cluster Planetary Bright Neb Dark Neb Reflection Neb Galaxy Int:Pec Compact Galaxy Gr
    bright star double variable globular open cluster planetary bright neb dark neb reflection neb galaxy int:pec compact galaxy group quasar ALL AND ANT APS AQL AQR ARA ARI AUR BOO CAE CAM CAP CAR CAS CEN CEP CET CHA CIR CMA CMI CNC COL COM CRA CRB CRT CRU CRV CVN CYG DEL DOR DRA EQU ERI FOR GEM GRU HER HOR HYA HYI IND LAC LEO LEP LIB LMI LUP LYN LYR MEN MIC MON MUS NOR OCT OPH ORI PAV PEG PER PHE PIC PSA PSC PUP PYX RET SCL SCO SCT SER1 SER2 SEX SGE SGR TAU TEL TRA TRI TUC UMA UMI VEL VIR VOL VUL Object ConRA Dec Mag z AbsMag Type Spect Filter Other names CFHQS J23291-0301 PSC 23h 29 8.3 - 3° 1 59.2 21.6 6.430 -29.5 Q ULAS J1319+0950 VIR 13h 19 11.3 + 9° 50 51.0 22.8 6.127 -24.4 Q I CFHQS J15096-1749 LIB 15h 9 41.8 -17° 49 27.1 23.1 6.120 -24.1 Q I FIRST J14276+3312 BOO 14h 27 38.5 +33° 12 41.0 22.1 6.120 -25.1 Q I SDSS J03035-0019 CET 3h 3 31.4 - 0° 19 12.0 23.9 6.070 -23.3 Q I SDSS J20541-0005 AQR 20h 54 6.4 - 0° 5 13.9 23.3 6.062 -23.9 Q I CFHQS J16413+3755 HER 16h 41 21.7 +37° 55 19.9 23.7 6.040 -23.3 Q I SDSS J11309+1824 LEO 11h 30 56.5 +18° 24 13.0 21.6 5.995 -28.2 Q SDSS J20567-0059 AQR 20h 56 44.5 - 0° 59 3.8 21.7 5.989 -27.9 Q SDSS J14102+1019 CET 14h 10 15.5 +10° 19 27.1 19.9 5.971 -30.6 Q SDSS J12497+0806 VIR 12h 49 42.9 + 8° 6 13.0 19.3 5.959 -31.3 Q SDSS J14111+1217 BOO 14h 11 11.3 +12° 17 37.0 23.8 5.930 -26.1 Q SDSS J13358+3533 CVN 13h 35 50.8 +35° 33 15.8 22.2 5.930 -27.6 Q SDSS J12485+2846 COM 12h 48 33.6 +28° 46 8.0 19.6 5.906 -30.7 Q SDSS J13199+1922 COM 13h 19 57.8 +19° 22 37.9 21.8 5.903 -27.5 Q SDSS J14484+1031 BOO
    [Show full text]