Elisa/NGO, Revealing a Hidden Universe Notes & News for GW

Total Page:16

File Type:pdf, Size:1020Kb

Elisa/NGO, Revealing a Hidden Universe Notes & News for GW GW Notes Special Issue: eLISA/NGO, revealing a hidden universe Notes & News for GW science Guest editors: David Spergel and Zhang Shuangnan Editors: Pau Amaro-Seoane and Bernard F. Schutz ISSN: 1868-1921 GW Notes was born from the need for a journal where the distinct communities in- volved in gravitational wave research might gather. While these three communities - Astrophysics, General Relativity and Data Analysis - have made significant collabora- tive progress over recent years, we believe that it is indispensable to future advancement that they draw closer, and that they speak a common idiom. Notes & News for GW science 1 Publisher: Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) Am Mühlenberg 1 14476 Potsdam Germany Editors: P. Amaro Seoane and B.F. Schutz ISSN: 1868-1921 URL: http://brownbag.lisascience.org/lisa-gw-notes/ Notes & News for GW science #6 May 28, 2013 GW Notes 1 Notes & News for GW science eLISA/NGO: Revealing a hidden universe Editorial Prof. A. Lobo As you proably know, Prof. José Alberto Lobo Gutiérrez passed away last September 30 2012. He left behind a wife (Rosa Maria), a son (Albert), and a daughter (Montser- rat). Prof. Lobo has been a pioneer of the field of Gravitational Wave Astronomy in Spain, devoting his life to resonant ground-based detectors and to space-based ones. His contributions range from theoretical studies to the development of instrumen- tation, including data analysis methods. Even in the final stages of his cancer, he was mainly concerned and actively planning towards maintaining and promoting Notes & News for GW science the Spanish team activities and involvement into LISA PathFinder and its successor mission LISA. José Alberto Lobo Gutiérrez obtained his PhD from the University of Barcelona (UB) in 1980, doing research under the supervision of Prof. Joaquim Gomis and writing a thesis in “Dynamics of Relativistic Particles”. Afterwards, he worked at the UB for about 25 years where he taught a variety of topics, many of them theoretical, like mathematical methods of physics or General Relativity, but also experimental. During all this time he had the opportunity to interact with many students. His very personal way of teaching has left an imprint on most of his students. He also supervised eight PhD thesis on gravitational wave astronomy. His research path started in the area of theoretical physics but his research interests evolved towards the area of gravitational physics and of gravitational wave astron- omy, where he has been a pioneer of the field in Spain. His contributions to this field cover a wide range of topics, from theoretical studies to the design and development of instrumentation, including data analysis techniques. After more than a decade of working on science related to ground-based gravitational-wave observatories, mainly on resonant detectors, he got involved in the endeavor of designing and building a space-based gravitational-wave detector, the Laser Interferometer Space Antenna (LISA). To that end he formed a new group from scratch at the Institut de Ciències de l’Espai (ICE; CSIC-IEEC). With this group he led the Spanish contribution to the LISA PathFinder mission and also research towards a future LISA mission. In 2005 he moved to the ICE as a CSIC Research Professor, where he remained. During these years, the ICE group has contributed the Data and Diagnostic Subsystem of the LISA Technology Package (LTP), the pay- load of LISA PathFinder. This consists of highly stable temperature sensors, magne- tometers and a particle counter to monitor the experiment environment, plus heaters and magnetic coils. These instruments will monitor and characterize the experiment 2 GW Notes May 28, 2013 Notes & News for GW science eLISA/NGO: Revealing a hidden universe during flight operations. In addition, the Data Management Unit will act as the com- puter of the LTP experiment, processing the measurements and controlling different subsystems. This hardware package, together with the flight software, has been de- livered for its final integration in the satellite. Alberto Lobo was also a member of the LISA International Science Team and of the Science Team for eLISA/NGO. His leadership and human qualities have been fun- damental for the success of the enterprise he initiated at the ICE. Probably, one of his biggest achievements has been to transmit his passion and his joy for science to everybody around him, and to prepare a generation of scientists that will continue the efforts that he pioneered. Since we have been authors on the highlight article of this issue of GW Notes, we have approached David Spergel and Zhang Shuangnan and asked them to be guest editors, so that the refereed process was anonymous. We thank them for their effort with the communication with the referee. Notes & News for GW science Due to the length of this article, we have decided to exclude from this issue the ab- stracts of those papers published on the arxiv since the previous GW Notes. Alberto was a valued colleague and friend, and will be sorely missed by the grav- itational wave community. It is our hope that this article will help in keeping his memory alive. Pau Amaro-Seoane & Bernard F. Schutz, editors #6 May 28, 2013 GW Notes 3 Notes & News for GW science eLISA/NGO: Revealing a hidden universe GW Notes highlight article eLISA/NGO eLISA/NGO: Astrophysics and cosmology in the gravitational-wave millihertz regime Pau Amaro-Seoane 1, Sofiane Aoudia 1, Stanislav Babak 1, Pierre Binétruy 2, Emanuele Berti 3; 4, Alejandro Bohé 5, Chiara Caprini 6, Monica Colpi 7, Neil J. Cornish 8, Karsten Danzmann 1, Jean-François Dufaux 2, Jonathan Gair 9, Ian Hinder 1, Oliver Jennrich 10, Philippe Jetzer 11, Antoine Klein 11; 8, Ryan N. Lang 12, Alberto Lobo 13, Tyson Littenberg 14; 15, Sean T. McWilliams 16, Gijs Nelemans 17; 18; 19, Antoine Notes & News for GW science Petiteau 2; 1, Edward K. Porter 2, Bernard F. Schutz 1, Alberto Sesana 1, Robin Stebbins 20, Tim Sumner 21, Michele Vallisneri 22, Stefano Vitale 23, Marta Volonteri 24; 25, Henry Ward 26 and Barry Wardell 1; 27 1Max Planck Institut für Gravitationsphysik (Albert-Einstein-Institut), Germany , 2APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs. de Paris, Sorbonne Paris Cité, France , 3Department of Physics and Astronomy, The University of Mississippi, University, MS 38677, USA , 4Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena CA 91125, USA , 5UPMC- CNRS, UMR7095, Institut d’Astrophysique de Paris, F-75014, Paris, France , 6Institut de Physique Théorique, CEA, IPhT, CNRS, URA 2306, F-91191Gif/Yvette Cedex, France , 7University of Milano Bicocca, Milano, I-20100, Italy , 8Department of Physics, Montana State University, Bozeman, MT 59717, USA , 9Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK , 10ESA, Keplerlaan 1, 2200 AG Noordwijk, The Netherlands , 11Institute of Theoretical Physics University of Zürich, Winterthurerstr. 190, 8057 Zürich Switzerland , 12Washington University in St. Louis, One Brookings Drive, St. Louis, MO 63130, USA , 13Institut de Ciències de l’Espai (CSIC-IEEC), Campus UAB, Torre C-5, parells, 2na planta, ES-08193, Bellaterra, Barcelona, Spain , 14Maryland Center for Fundamental Physics, Department of Physics, University of Maryland, College Park, MD 20742 , 15Gravitational Astrophysics Laboratory, NASA Goddard Spaceflight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA , 16Department of Physics, Princeton University, Princeton, NJ 08544, USA , 17Department of Astrophysics, Radboud University Nijmegen, The Netherlands , 18Institute for Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium , 19Nikhef, Science Park 105, 1098 XG Amsterdam, The Netherlands , 20NASA Liason, NASA GSFC, USA , 21Imperial College, UK , 22Jet Propulsion Laboratory, California Inst. of Technology, Pasadena, CA 91109, USA , 23University of Trento, Department of Physics, I38050 Povo, Trento, Italy , 24Institut d’Astrophysique de Paris, 98bis Boulevard Arago, 75014 Paris, France , 25Astronomy Department, University of Michigan, Ann Arbor, MI 48109, USA , 26Institute for Gravitational Research, Department of Physics & Astronomy Kelvin Building, University of Glasgow, Glasgow , 27School of Mathematical Sciences and Complex & Adaptive Systems Laboratory, University College Dublin, Belfield, Dublin 4, Ireland. 4 GW Notes May 28, 2013 Notes & News for GW science eLISA/NGO: Revealing a hidden universe We acknowledge the LISA Pathfinder Team and the rest of the members of the former joint science team for LISA, whose work constituted a crucial starting point for our ar- ticle: F. Antonucci, M. Armano, H. Audley, G. Auger, M. Benedetti, J. Bogenstahl, D. Bor- toluzzi, N. Brandt, M. Caleno, A. Cavalleria, G. Congedo, M. Cruise, F. De Marchia, M. Diaz-Aguilo, I. Diepholz, G. Dixon, R. Dolesi, N. Dunbar, J. Fauste, L. Ferraioli, V. Ferroni, W. Fichter, E. Fitzsimons, M. Freschi, C. García Marirrodriga, R. Gerndt, L. Gesa, F. Gibert, D. Giardini, C. Grimani, A. Grynagier, F. Guzmán, H. Halloin, I. Harrison, G. Heinzel, M. Hewitson, D. Hollington, D. Hoyland, M. Hueller, J. Huesler, B. Johlander, N. Karnesis, N. Korsakova, C. Killow, X. Llamas, I. Lloro, R. Maarschalkerweerd, S. Madden, D. Mance, V. Martin, I. Mateos, P. McNamara, J. Mendes, E. Mitchells, D. Nicolodi, M. Nofrarias, M. Perreur-Lloyd, E. Plagnol, P. Notes & News for GW science Prat, J. Ramos-Castro, J. Reiche, J.A. Romera Pérez, D. Robertson, H. Rozemeijer, G. Russano, A. Schleicher,
Recommended publications
  • Very High Energy Emission from Blazars Interpreted Through Simultaneous Multiwavelength Observations
    UNIVERSITA` DEGLI STUDI DI SIENA FACOLTA` DI SCIENZE MATEMATICHE, FISICHE E NATURALI Dipartimento di Fisica Very High Energy emission from blazars interpreted through simultaneous multiwavelength observations Relatore/Supervisor: Candidato/Candidate: Dr. Antonio Stamerra Giacomo Bonnoli Tutore/Tutor: Prof. Riccardo Paoletti Ph.D. School in Physics Cycle XXI December 2010 Abstract In the framework of Astroparticle Physics the understanding of the particle acceleration process and related high energy electromagnetic emission within astrophysical sources is an issue of fundamental importance to unravel the structure and evolution of many classes of celestial objects, on different scales from micro{quasars to active galactic nuclei. This has an important role not only for astrophysics itself, but for many related topics of cosmic ray physics and High Energy physics, such as the search for dark matter. Also cosmology is interested, as deepening our knowledge on Active Galactic Nuclei and their interaction with the environment can help to clarify open issues on the formation of cosmic structures and evolution of universe on large scales. The present view on sources emitting high energy radiation is now gaining new insight thanks to multiwavelength observations. This approach allows to explore the spectral energy distribution of the sources all across the electromagnetic spectrum, therefore granting the best achievable understanding of the physical processes that originate the radiation that we see, and their mutual relationships. Our theories model the sources in terms of parameters that can be inferred from the observables quantities measured, and the multiwavelength observations are a key instrument in order to rule out or support some selected models out of the many that compete in the effort of describing the processes at work.
    [Show full text]
  • Active Galactic Nuclei: a Brief Introduction
    Active Galactic Nuclei: a brief introduction Manel Errando Washington University in St. Louis The discovery of quasars 3C 273: The first AGN z=0.158 2 <latexit sha1_base64="4D0JDPO4VKf1BWj0/SwyHGTHSAM=">AAACOXicbVDLSgMxFM34tr6qLt0Ei+BC64wK6kIoPtCNUMU+oNOWTJq2wWRmSO4IZZjfcuNfuBPcuFDErT9g+hC09UC4h3PvJeceLxRcg20/W2PjE5NT0zOzqbn5hcWl9PJKUQeRoqxAAxGoskc0E9xnBeAgWDlUjEhPsJJ3d9rtl+6Z0jzwb6ETsqokLZ83OSVgpHo6754xAQSf111JoK1kTChN8DG+uJI7N6buYRe4ZBo7di129hJ362ew5NJGAFjjfm3V4m0nSerpjJ21e8CjxBmQDBogX08/uY2ARpL5QAXRuuLYIVRjooBTwZKUG2kWEnpHWqxiqE+MmWrcuzzBG0Zp4GagzPMB99TfGzGRWnekZya7rvVwryv+16tE0DysxtwPI2A+7X/UjASGAHdjxA2uGAXRMYRQxY1XTNtEEQom7JQJwRk+eZQUd7POfvboej+TOxnEMYPW0DraRA46QDl0ifKogCh6QC/oDb1bj9ar9WF99kfHrMHOKvoD6+sbuhSrIw==</latexit> <latexit sha1_base64="H7Rv+ZHksM7/70841dw/vasasCQ=">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</latexit> The power source of quasars • The luminosity (L) of quasars, i.e. how bright they are, can be as high as Lquasar ~ 1012 Lsun ~ 1040 W. • The energy source of quasars is accretion power: - Nuclear fusion: 2 11 1 ∆E =0.007 mc =6 10 W s g−
    [Show full text]
  • Dynamics and Evolution of Supermassive Black Holes in Merging Galaxies
    Dynamics and Evolution of Supermassive Black Holes in Merging Galaxies Fazeel Mahmood Khan Astronomisches Rechen-Institut Zentrum f¨urAstronomie der Universit¨atHeidelberg Heidelberg 2011 Cover picture: Gemini image of NGC 5426-27 (Arp 271). Dissertation submitted to the Combined Faculties for the Natural Sciences and for Mathematics of the Ruperto-Carola University of Heidelberg, Germany for the degree of Doctor of Natural Sciences Put forward by Fazeel Mahmood Khan Born in: Azad Kashmir, Pakistan Oral examination: January 25, 2012 Dynamics and Evolution of Supermassive Black Holes in Merging Galaxies Referees: PD Dr. Andreas Just Prof. Dr. Volker Springel Abstract Supermassive black holes (SMBHs) are ubiquitous in galaxy centers and are correlated with their hosts in fundamental ways, suggesting an intimate link between SMBH and galaxy evolution. In the paradigm of hierarchical galaxy formation this correlation demands prompt coalescence of SMBH binaries, presumably due to dynamical friction, interaction of stars and gas with the binary and finally due to gravitational wave emission. If they are able to coalesce in less than a Hubble time, SMBH binaries will be a promising source of gravitational waves for gravitational wave detectors. However, it has been suggested that SMBH binaries may stall at a separation of 1 parsec. This stalling is sometimes referred to as the \Final Parsec Problem (FPP)". This study uses N-body simulations to test an improved formula for the orbital decay of SMBHs due to dynamical friction. Using a large set of N-body simulations, we show that the FPP does not occur in galaxies formed via mergers. The non spherical shape of the merger remnants ensures a constant supply of stars for the binary to interact with.
    [Show full text]
  • Messier Objects
    Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun.
    [Show full text]
  • Asian Nobel Prize' for Mapping the Universe 27 May 2010
    Scientists win 'Asian Nobel Prize' for mapping the universe 27 May 2010 Three US scientists whose work helped map the category. universe are among the recipients of the one- million-US-dollar Shaw Prize, known as the "Asian (c) 2010 AFP Nobel," the competition's organisers said Thursday. Princeton University professors Lyman Page and David Spergel and Charles Bennett of Johns Hopkins University, won the award for an experiment that helped to determine the "geometry, age and composition of the universe to unprecedented precision." The trio will share the Shaw Prize's award for astronomy, with one-million-US-dollar prizes also awarded in the categories for mathematical sciences and life sciences and medicine. The University of California's David Julius won the award for life sciences and medicine for his "seminal discoveries" of how the skin senses pain and temperature, the organisers' statement said. "(Julius's) work has provided insights into fundamental mechanisms underlying the sense of touch as well as knowledge that opens the door to rational drug design for the treatment of chronic pain," the statement said. Princeton's Jean Bourgain won an award for his "profound work" in mathematical sciences, it said. The Shaw Prize, funded by Hong Kong film producer and philanthropist Run Run Shaw and first awarded in 2004, honours exceptional contributions "to the advancement of civilization and the well-being of humankind." The awards will be presented at a ceremony in Hong Kong on September 28. Last year, two scientists whose work challenged the assumption that obesity is caused by a lack of will power won the life sciences and medicine 1 / 2 APA citation: Scientists win 'Asian Nobel Prize' for mapping the universe (2010, May 27) retrieved 27 September 2021 from https://phys.org/news/2010-05-scientists-asian-nobel-prize-universe.html This document is subject to copyright.
    [Show full text]
  • Professor Peter Goldreich Member of the Board of Adjudicators Chairman of the Selection Committee for the Prize in Astronomy
    The Shaw Prize The Shaw Prize is an international award to honour individuals who are currently active in their respective fields and who have recently achieved distinguished and significant advances, who have made outstanding contributions in academic and scientific research or applications, or who in other domains have achieved excellence. The award is dedicated to furthering societal progress, enhancing quality of life, and enriching humanity’s spiritual civilization. Preference is to be given to individuals whose significant work was recently achieved and who are currently active in their respective fields. Founder's Biographical Note The Shaw Prize was established under the auspices of Mr Run Run Shaw. Mr Shaw, born in China in 1907, was a native of Ningbo County, Zhejiang Province. He joined his brother’s film company in China in the 1920s. During the 1950s he founded the film company Shaw Brothers (HK) Limited in Hong Kong. He was one of the founding members of Television Broadcasts Limited launched in Hong Kong in 1967. Mr Shaw also founded two charities, The Shaw Foundation Hong Kong and The Sir Run Run Shaw Charitable Trust, both dedicated to the promotion of education, scientific and technological research, medical and welfare services, and culture and the arts. ~ 1 ~ Message from the Chief Executive I warmly congratulate the six Shaw Laureates of 2014. Established in 2002 under the auspices of Mr Run Run Shaw, the Shaw Prize is a highly prestigious recognition of the role that scientists play in shaping the development of a modern world. Since the first award in 2004, 54 leading international scientists have been honoured for their ground-breaking discoveries which have expanded the frontiers of human knowledge and made significant contributions to humankind.
    [Show full text]
  • David Spergel Is the Director of the Center for Computational Astrophysics and the Charles Young Professor of Astronomy at Princeton University
    David Spergel is the director of the Center for Computational Astrophysics and the Charles Young Professor of Astronomy at Princeton University. He is the former chair of the Space Studies Board. Using microwave background observations from the Wilkinson Microwave Anisotropy Probe (WMAP) and the Atacama Cosmology Telescope, Spergel has measured the age, shape and composition of the universe. These observations have played a significant role in establishing the standard model of cosmology. He is one of the leaders of the Simons Observatory, which will include a planned millimeter-wave telescope that will allow us to take the next step in studying the microwave sky and probing the history of the universe. Spergel is currently co-chair of the Wide Field Infrared Survey Telescope (WFIRST) science team. WFIRST will study the nature of dark energy, complete the demographic survey of extrasolar planets, characterize the atmospheres of nearby planets and survey the universe with more than 100 times the field of view of the Hubble Space Telescope. Spergel has played a significant role in designing the coronagraph and in shaping the overall mission. Since completing my Ph.D. work, Spergel has been interested in using laboratory experiments and astronomical observations to probe the nature of dark matter and look for new physics. Recently, Spergel has been active in the exploration of data from the Gaia satellite and observations made by Subaru’s Hyper Suprime-Cam. Spergel serves as co-chair of the Global Coordination of Ground and Space Astrophysics working group of the International Astronomical Union. At Princeton, Spergel was department chair for a decade.
    [Show full text]
  • Gamma-Ray and Neutrino Signals from Accretion Disk Coronae of Active Galactic Nuclei
    galaxies Review Gamma-ray and Neutrino Signals from Accretion Disk Coronae of Active Galactic Nuclei Yoshiyuki Inoue 1,2,3,* , Dmitry Khangulyan 4 and Akihiro Doi 5,6 1 Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka 560-0043, Japan 2 Interdisciplinary Theoretical & Mathematical Science Program (iTHEMS), RIKEN, 2-1 Hirosawa, Saitama 351-0198, Japan 3 Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa 277-8583, Japan 4 Department of Physics, Rikkyo University, Nishi-Ikebukuro 3-34-1, Toshima-ku, Tokyo 171-8501, Japan; [email protected] 5 Institute of Space and Astronautical Science JAXA, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan; [email protected] 6 Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), 3-1-1 Yoshinodai, Chuou-ku, Sagamihara, Kanagawa 252-5210, Japan * Correspondence: [email protected] Abstract: To explain the X-ray spectra of active galactic nuclei (AGN), non-thermal activity in AGN coronae such as pair cascade models has been extensively discussed in the past literature. Although X-ray and Gamma-ray observations in the 1990s disfavored such pair cascade models, recent millimeter-wave observations of nearby Seyferts have established the existence of weak non-thermal coronal activity. In addition, the IceCube collaboration reported NGC 1068, a nearby Seyfert, as the hottest spot in their 10 year survey. These pieces of evidence are enough to investigate the non-thermal perspective of AGN coronae in depth again. This article summarizes our current Citation: Inoue, Y.; Khangulyan, D.; observational understanding of AGN coronae and describes how AGN coronae generate high-energy Doi, A.
    [Show full text]
  • Positron Annihilation Spectroscopy of Active Galactic Nuclei
    Research Paper J. Astron. Space Sci. 36(1), 21-33 (2019) https://doi.org/10.5140/JASS.2019.36.1.21 Positron Annihilation Spectroscopy of Active Galactic Nuclei Dmytry N. Doikov1, Alexander V. Yushchenko2, Yeuncheol Jeong3† 1Odessa National Maritime University, Department of Mathematics, Physics and Astronomy, Odessa, 65029, Ukraine 2Astrocamp Contents Research Institute, Goyang, 10329, Korea 3Daeyang Humanity College, Sejong University, Seoul, 05006, Korea This paper focuses on the interpretation of radiation fluxes from active galactic nuclei. The advantage of positron annihilation spectroscopy over other methods of spectral diagnostics of active galactic nuclei (therefore AGN) is demonstrated. A relationship between regular and random components in both bolometric and spectral composition of fluxes of quanta and particles generated in AGN is found. We consider their diffuse component separately and also detect radiative feedback after the passage of high-velocity cosmic rays and hard quanta through gas-and-dust aggregates surrounding massive black holes in AGN. The motion of relativistic positrons and electrons in such complex systems produces secondary radiation throughout the whole investigated region of active galactic nuclei in form of cylinder with radius R= 400-1000 pc and height H=200-400 pc, thus causing their visible luminescence across all spectral bands. We obtain radiation and electron energy distribution functions depending on the spatial distribution of the investigated bulk of matter in AGN. Radiation luminescence of the non- central part of AGN is a response to the effects of particles and quanta falling from its center created by atoms, molecules and dust of its diffuse component. The cross-sections for the single-photon annihilation of positrons of different energies with atoms in these active galactic nuclei are determined.
    [Show full text]
  • 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).
    [Show full text]
  • The Physics and Cosmology of Tev Blazars
    Blazars Gamma-ray sky Structure formation The Physics and Cosmology of TeV Blazars Christoph Pfrommer1 in collaboration with Avery E. Broderick, Phil Chang, Ewald Puchwein, Astrid Lamberts, Mohamad Shalaby, Volker Springel 1Heidelberg Institute for Theoretical Studies, Germany Jun 11, 2015 / Nonthermal Processes in Astrophysical Phenomena, Minneapolis Christoph Pfrommer The Physics and Cosmology of TeV Blazars Blazars Gamma-ray sky Structure formation Motivation A new link between high-energy astrophysics and cosmological structure formation Introduction to Blazars active galactic nuclei (AGN) propagating gamma rays plasma physics Cosmological Consequences unifying blazars with AGN gamma-ray background thermal history of the Universe Lyman-α forest formation of dwarf galaxies Christoph Pfrommer The Physics and Cosmology of TeV Blazars AGNs are among the most luminous sources in the universe → discovery of distant objects Blazars Active galactic nuclei Gamma-ray sky Propagating γ rays Structure formation Plasma instabilities Active galactic nucleus (AGN) AGN: compact region at the center of a galaxy, which dominates the luminosity of its electromagnetic spectrum AGN emission is most likely caused by mass accretion onto a supermassive black hole and can also launch relativistic jets Centaurus A Christoph Pfrommer The Physics and Cosmology of TeV Blazars Blazars Active galactic nuclei Gamma-ray sky Propagating γ rays Structure formation Plasma instabilities Active galactic nucleus at a cosmological distance AGN: compact region at the center
    [Show full text]
  • MATTERS of GRAVITY Contents Editor
    MATTERS OF GRAVITY The newsletter of the Topical Group on Gravitation of the American Physical Society Number 17 Spring 2001 Contents APS TGG News: APS Prize on gravitation, by Clifford Will .................. 3 TGG Elections, by David Garfinkle ...................... 3 We hear that, by Jorge Pullin ......................... 3 Research Briefs: Experimental Unruh Radiation?, by Matt Visser ............... 4 Why is the Universe accelerating?, by Beverly Berger ............ 6 The Lazarus Project, by Richard Price .................... 9 LIGO locks its first detector!, by Stan Whitcomb ............... 12 Progress on the nonlinear r-mode problem, by Keith Lockitch ........ 13 Conference Reports Analog Models of General Relativity, by Matt Visser ............. 17 Astrophysical Sources of Gravitational radiation, by Joan Centrella ..... 19 Numerical relativity at the 20th Texas meeting, by Pablo Laguna ...... 21 Editor Jorge Pullin Center for Gravitational Physics and Geometry The Pennsylvania State University University Park, PA 16802-6300 Fax: (814)863-9608 Phone (814)863-9597 Internet: [email protected] WWW: http://www.phys.psu.edu/~pullin ISSN: 1527-3431 1 Editorial Not much to report here. If you are burning to have Matters of Gravity with you all the time, the newsletter is now available for Palm Pilots, Palm PC's and web-enabled cell phones as an Avantgo channel. Check out http://www.avantgo.com under technology science. The next newsletter is due September 1st. If everything goes well this newsletter should! be available in the gr-qc Los Alamos archives (http://xxx.lanl.gov) under number gr-qc/yymmnnn. To retrieve it send email to [email protected] with Subject: get yymmnnn (numbers 2-16 are also available in gr-qc).
    [Show full text]