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The Afterglows of Swift-Era Gamma-Ray Bursts. I. Comparing Pre-Swift and Swift-Era Long/Soft (Type Ii) Grb Optical Afterglows∗

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Roger Williams University DOCS@RWU Feinstein College of Arts & Sciences Faculty Feinstein College of Arts and Sciences Publications 2010 THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE- SWIFT AND SWIFT-ERA ONL G/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS D. A. Kann S. Klose B. Zhang D. Malesani E. Nakar See next page for additional authors Follow this and additional works at: http://docs.rwu.edu/fcas_fp Part of the Astrophysics and Astronomy Commons Recommended Citation Kann, D.A. ....... A. Updike, et al. 2010. "The Afterglows of Swift-Era Gamma-Ray Bursts. I. Comparing Pre-Swift nda Swift-Era Long/ Soft T( ype II) GRB Optical Afterglows." Astrophysical Journal 720: 1513. This Article is brought to you for free and open access by the Feinstein College of Arts and Sciences at DOCS@RWU. It has been accepted for inclusion in Feinstein College of Arts & Sciences Faculty Publications by an authorized administrator of DOCS@RWU. For more information, please contact [email protected]. Authors D. A. Kann, S. Klose, B. Zhang, D. Malesani, E. Nakar, A. Pozanenko, A. C. Wilson, N. R. Butler, P. Jakobsson, S. Schulze, M. Andreev, L. A. Antonelli, I. F. Bikmaev, V. Biryukov, M. B¨ottcher, R. A. Burenin, J. M. Castro Cer´on, A. J. Castro-Tirado, G. Chincarini, B. E. Cobb, S. Covino, P. D’Avanzo, V. D’Elia, M. Della Valle, A. de Ugarte Postigo, Yu Efimov, P. Ferrero, D. Fugazza, D. Fugazza, J. P.U. Fynbo, M. Gålfalk, F. Grundahl, J. Gorosabel, S. Gupta, S. Guziy, B. Hafizov, J. Hjorth, K. Holhjem, M. Ibrahimov, M. Im, G. L. Israel, M. Je´linek, B. L. Jensen, R. Karimov, I. M. Khamitov, U. Kizilogˇlu, E. Klunko, P. Kuba´nek, A. S. Kutyrev, P. Laursen, A. J. Levan, F. Mannucci, C. M. Martin, A. Mescheryakov, N. Mirabal, J. P. Norris, J. -E. Ovaldsen, D. Paraficz, E. Pavlenko, S. Piranomonte, A. Rossi, V. Rumyantsev, R. Salinas, A. Sergeev, D. Sharapov, J. Sollerman, B. Stecklum, L. Stella, G. Tagliaferri, N. R. Tanvir, J. Telting, V. Testa, Adria Updike, A. Volnova, D. Watson, K. Wiersema, and D. Xu This article is available at DOCS@RWU: http://docs.rwu.edu/fcas_fp/242 The Astrophysical Journal, 720:1513–1558, 2010 September 10 doi:10.1088/0004-637X/720/2/1513 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFT AND SWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS∗ D. A. Kann1,S.Klose1, B. Zhang2, D. Malesani3, E. Nakar4,5, A. Pozanenko6,A.C.Wilson7, N. R. Butler8,9,52, P. Jakobsson10,11, S. Schulze1,11, M. Andreev12,13, L. A. Antonelli14,I.F.Bikmaev15, V. Biryukov16,17,M.Bottcher¨ 18, R. A. Burenin6, J. M. Castro Ceron´ 3,19, A. J. Castro-Tirado20, G. Chincarini21,22,B.E.Cobb23,24,S.Covino21, P. D’Avanzo22,25,V.D’Elia14,26, M. Della Valle27,28,29, A. de Ugarte Postigo21, Yu. Efimov16, P. Ferrero1,30, D. Fugazza21,J.P.U.Fynbo3, M. Gålfalk31, F. Grundahl32, J. Gorosabel20, S. Gupta18,S.Guziy20, B. Hafizov33, J. Hjorth3, K. Holhjem34,35, M. Ibrahimov33,M.Im36, G. L. Israel14,M.Jelinek´ 20,B.L.Jensen3, R. Karimov33, I. M. Khamitov37, U.¨ Kizilogluˇ 38, E. Klunko39,P.Kubanek´ 19, A. S. Kutyrev40, P. Laursen3, A. J. Levan41, F. Mannucci42, C. M. Martin43, A. Mescheryakov6, N. Mirabal44,53, J. P. Norris45, J.-E. Ovaldsen46, D. Paraficz3, E. Pavlenko17, S. Piranomonte14,A.Rossi1, V. Rumyantsev17, R. Salinas47, A. Sergeev12,13, D. Sharapov33, J. Sollerman3,31, B. Stecklum1, L. Stella14, G. Tagliaferri21,N.R.Tanvir48, J. Telting33, V. Testa14, A. C. Updike49, A. Volnova50, D. Watson3, K. Wiersema48,51, and D. Xu3 1 Thuringer¨ Landessternwarte Tautenburg, Sternwarte 5, D–07778 Tautenburg, Germany 2 Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA 3 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 København Ø, Denmark 4 Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 5 Raymond and Beverly Sackler School of Physics & Astronomy, Tel Aviv University, Tel Aviv 69978, Israel 6 Space Research Institute (IKI), 84/32 Profsoyuznaya Str, Moscow 117997, Russia 7 Department of Astronomy, University of Texas, Austin, TX 78712, USA 8 Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450, USA 9 Astronomy Department, University of California, 445 Campbell Hall, Berkeley, CA 94720-3411, USA 10 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Herts, AL10 9AB, UK 11 Centre for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, IS 107 Reykjavik, Iceland 12 Terskol Branch of Institute of Astronomy of RAS, Kabardino-Balkaria Republic 361605, Russian Federation 13 International Centre of Astronomical and Medico-Ecological Research of NASU, 27 Akademika Zabolotnoho St. 03680 Kyiv, Ukraine 14 INAF, Osservatorio Astronomico di Roma, via Frascati 33, 00040, Monteporzio Catone (RM), Italy 15 Kazan State University and Academy of Sciences of Tatarstan, Kazan, Russia 16 Crimean Laboratory of the Sternberg Astronomical Institute, Nauchny, Crimea 98409, Ukraine 17 SRI “Crimean Astrophysical Observatory” (CrAO), Nauchny, Crimea 98409, Ukraine 18 Astrophysical Institute, Department of Physics and Astronomy, Clippinger 339, Ohio University, Athens, OH 45701, USA 19 European Space Agency (ESA), European Space Astronomy Centre (ESAC), P.O. Box-Apdo. de correos 78, 28691 Villanueva de la Canada,˜ Madrid, Spain 20 Instituto de Astrof´ısica de Andaluc´ıa (IAA-CSIC), Apartado de Correos, 3004, E-18080 Granada, Spain 21 INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy 22 Dipartimento di Fisica, Universita` degli studi di Milano-Bicocca, piazza delle Scienze 3, 20126 Milano, Italy 23 Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520, USA 24 Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720–3411, USA 25 Dipartimento di Fisica e Matematica, Universita` dell’Insubria, via Valleggio 11, 22100 Como, Italy 26 ASI-Science Data Centre, Via Galileo Galilei, I-00044 Frascati, Italy 27 INAF, Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16 80131, Napoli, Italy 28 European Southern Observatory, Karl Schwarschild Strasse 2, D-85748 Garching bei Munchen,¨ Germany 29 International Centre for Relativistic Astrophysics Network, Piazzale della Republica 2, Pescara, Abruzzo, Italy 30 Instituto de Astrof´ısica de Canarias, C/ V´ıa Lactea,´ s/n E38205-La Laguna (Tenerife), Spain 31 Stockholm Observatory, Department of Astronomy, Stockholm University, AlbaNova University Centre, 106 91 Stockholm, Sweden 32 Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, 8000 Århus C, Denmark 33 Ulugh Beg Astronomical Institute, Tashkent 700052, Uzbekistan 34 Nordic Optical Telescope, Apartado 474, Santa Cruz de La Palma, Spain 35 Argelander-Institut fur¨ Astronomie, Universitat¨ Bonn, Auf dem Hugel¨ 71, D-53121 Bonn, Germany 36 Center for the Exploration of the Origin of the Universe (CEOU), Astronomy Program, Department of Physics & Astronomy, Seoul National University, 56-1 San, Shillim-dong, Kwanak-gu, Seoul, South Korea 37 TUB¨ ITAK˙ National Observatory, Antalya, Turkey 38 Middle East Technical University, Ankara, Turkey 39 Institute of Solar-Terrestrial Physics, Lermontov st., 126a, Irkutsk 664033, Russia 40 Observational Cosmology Laboratory, NASA/GSFC, 8800 Greenbelt Road, Greenbelt, MD 20771-2400, USA 41 Department of Physics, University of Warwick, Coventry, CV4 7AL, UK 42 INAF, Osservatorio Astrofisico di Arcetri, largo E. Fermi 5, I-50125 Firenze, Italy 43 Loyola College, 4501 N. Charles Street, Baltimore, MD 21210, USA 44 Dpto. de F´ısica Atomica,´ Molecular y Nuclear, Universidad Complutense de Madrid, Madrid, Spain 45 Department of Physics and Astronomy, University of Denver, Denver, CO 80208, USA 46 Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029, Blindern, N-0315 Oslo, Norway 47 Grupo de Astronom´ıa, Facultad de Ciencias F´ısicas y Matematicas,´ Universidad de Concepcion,´ Concepcion,´ Chile 48 Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK 49 Department of Physics and Astronomy, Clemson University, 118 Kinard Laboratory, Clemson, SC 29634, USA 50 Sternberg Astronomical Institute, Moscow State University, Universitetsky pr., 13, Moscow 119992, Russia 51 Astronomical Institute “Anton Pannekoek,” University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands Received 2007 December 13; accepted 2010 July 15; published 2010 August 23 1513 1514 KANN ET AL. Vol. 720 ABSTRACT We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to 2009 September, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A, and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host-galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z = 1system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, are weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) is very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at 1 day after the GRB in the z = 1 system.
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    IL NUOVO CIMENTO Vol. 32 C, N. 3-4 Maggio-Agosto 2009 DOI 10.1393/ncc/i2009-10424-6 Colloquia: IFAE 2009 Recent results in High Energy Gamma-ray Astrophysics G. Barbiellini(1)(2)andF. Longo(1)(2) (1) Dipartimento di Fisica, Universit`a di Trieste - Trieste, Italy (2) INFN, Sezione di Trieste - Trieste, Italy (ricevuto il 19 Settembre 2009; pubblicato online il 12 Ottobre 2009) Summary. — Since June 2008 two gamma-ray satellite experiments, AGILE and Fermi -LAT, have been in contemporaneous operation. Their results allow the study of gamma-ray astrophysics from space to enter in a new era. Starting from the heritage of the EGRET experiment, the science objectives of these two experiments are reviewed. The role of the technological improvement in such achievements is also briefly introduced. PACS 95.55.Ka –X-andγ-ray telescopes and instrumentation. 1. – Introduction to High Energy Gamma-ray Astrophysics main questions The study of the sky in the energy band E>10 MeV to E ∼ 100 GeV is commonly called High Energy Gamma-ray Astrophysics. In this energy band, some of the most energetic phenomena of the Universe happen. The processes at play in the high energy sources are characterized by a wide-band non-thermal emission. Observing the sources from radio to gamma-rays helps to clarify their nature and their environments. Moreover fundamental physics questions could be answered using the information provided by distant high energy sources. The two approaches are indeed complementary in the sense the second one needs the first to avoid potential source issues, while the first one needs the second one to address potential implications of the observations.
  • The Afterglows of Swift-Era Short and Long Gamma-Ray Bursts

    The Afterglows of Swift-Era Short and Long Gamma-Ray Bursts

    The Afterglows of Swift-era Short and Long Gamma-Ray Bursts Dissertation zur Erlangung des akademischen Grades Dr. rer. nat. vorgelegt dem Rat der Physikalisch-Astronomischen Fakult¨at der Friedrich-Schiller-Universit¨atJena eingereicht von Dipl.-Phys. David Alexander Kann geboren am 15.02.1977 in Trier Gutachter 1. Prof. Dr. Artie Hatzes, Th¨uringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg 2. Prof. Dr. J¨orn Wilms, Dr. Remeis-Sternwarte, Sternwartstraße 7, 96049 Bamberg 3. PD Dr. Hans-Thomas Janka, Max-Planck-Institut fr Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching Tag der letzten Rigorosumspr¨ufung: 13. 07. 2011 Tag der ¨offentlichen Verteidigung: 13. 07. 2011 Zusammenfassung Das Ph¨anomen der Gammastrahlenausbr¨uche (Englisch: Gamma-Ray Bursts, kurz: GRBs) war auch lange nach ihrer Entdeckung vor ¨uber vier Jahrzehnten ein großes R¨atsel. Selbst heute, ¨uber ein Jahrzehnt seit Beginn der “Ara¨ der Nachgl¨uhen” (engl.: Afterglows) sind noch viele Fragen unbeantwortet. Das akzeptierte Bild, welches einen Großteil der Daten erkl¨aren kann ist, dass GRBs erzeugt werden, wenn ein massereicher Himmelsk¨orper (en- tweder ein Stern, der die Hauptreihe verlassen hat, oder miteinander verschmelzende kom- pakte Objekte) in kosmologischer Distanz zu einem schnell rotierenden Objekt kollabiert (ein Schwarzes Loch oder vielleicht ein kurzlebiger Magnetar), welches ultrarelativistische Materieausw¨urfe (sogenannte “Jets”) entlang der Polachse ausschleudert. Die interne Dissi- pation von Energie in dem Jet f¨uhrt zu kollimierter nicht-thermischer Strahlung bei hohen Energien (der eigentliche GRB), w¨ahrend Schockfronten, die bei der Interaktion des Jets mit der interstellaren Materie erzeugt werden, zu einem langlebigen abklingenden Afterglows f¨uhren. Die gesammelten physikalischen Prozesse, die die GRB-Emission beschreiben, werden als das Standard-Feuerballmodell bezeichnet.