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Title:
Evidence for a Supernova Associated with the X-Ray Flash 020903
Authors:
Bersier, D.; Fruchter, A. S.; Strolger, L.-G.; Gorosabel, J.; Levan, A.; Burud, I.; Rhoads, J. E.; Becker, A. C.; Cassan, A.; Chornock, R.; Covino, S.; de Jong, R. S.; Dominis, D.; Filippenko, A. V.; Hjorth, J.; Holmberg, J.; Malesani, D.; Mobasher, B.; Olsen, K. A. G.; Stefanon, M.; Castro Cerón, J. M.; Fynbo, J. P. U.; Holland, S. T.; Kouveliotou, C.; Pedersen, H.; Tanvir, N. R.; Woosley, S. E.
Affiliation:
AA(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AB(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AC(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AD(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.; Instituto de Astrofísica de Andalucía (IAA-CSIC), P.O. Box 03004, E-18080 Granada, Spain.), AE(Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK.), AF(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AG(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AH(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195.), AI(Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F-75014 Paris, France.), AJ(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AK(INAF-Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate (LC), Italy.), AL(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AM(Universität Potsdam, Am Neues Palais 10, D-14469 Potsdam, Germany.; Astrophysikalische Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany.), AN(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AO(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100, Copenhagen, Denmark.), AP(Tuorla Observatory, Väisäläntie 20, FI-21500, Piikkiö, Finland.), AQ(International School for Advanced Studies (SISSA-ISAS), via Beirut 2-4, I-34014 Trieste, Italy.), AR(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AS(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), AT(INAF-Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate (LC), Italy.), AU(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.; Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100, Copenhagen, Denmark.), AV(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100, Copenhagen, Denmark.), AW(Swift Science Center, NASA Goddard Space Flight Center, Code 660.1, Greenbelt, MD 20771-0003.; Universities Space Research Association, 620-10211 Winicopin Circle, Columbia, MD 21044-3431.), AX(NASA Marshall Space Flight Center, NSSTC, SD-50, 320 Sparkman Drive, Huntsville, AL 35805.), AY(Astrophysikalische Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany.), AZ(Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK.), BA(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064.)
Publication:
The Astrophysical Journal, Volume 643, Issue 1, pp. 284-291. (ApJ Homepage)
Publication Date:
05/2006
Origin:
UCP
ApJ Keywords:
Gamma Rays: Bursts, Stars: Supernovae: General
DOI:
10.1086/502640
Bibliographic Code:
2006ApJ...643..284B

Abstract

We present ground-based and Hubble Space Telescope optical observations of the X-ray flash (XRF) 020903, covering 300 days. The afterglow showed a very rapid rise in the first day, followed by a relatively slow decay in the next few days. There was a clear bump in the light curve after ~25 days, accompanied by a drastic change in the spectral energy distribution. The light curve and the spectral energy distribution are naturally interpreted as describing the emergence and subsequent decay of a supernova (SN), similar to SN 1998bw. At peak luminosity, the SN is estimated to be 0.8+/-0.1 mag fainter than SN 1998bw. This argues in favor of the existence of a SN associated with this XRF. A spectrum obtained 35 days after the burst shows emission lines from the host galaxy. We use this spectrum to put an upper limit on the oxygen abundance of the host at [O/H]<=-0.6 dex. We also discuss a possible trend between the softness of several bursts and the early behavior of the optical afterglow, in the sense that XRFs and X-ray-rich gamma-ray bursts (GRBs) seem to have a plateau phase or even a rising light curve. This can be naturally explained in models in which XRFs are similar to GRBs but are seen off the jet axis.

Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These observations are associated with program GO-9405 (PI A. Fruchter).


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