PHOTOMETRY AND SPECTROSCOPY OF GRB 030329 AND ITS ASSOCIATED SUPERNOVA 2003dh: THE FIRST TWO MONTHS

Matheson, Thomas; Garnavich, P. M.; Stanek, k. z.; Bersier, D.; Holland, S. T.; Krisciunas, K.; Caldwell, N.; Berlind, P.; Bloom, J. S.; Bolte, M.; Bonanos, A. Z.; Brown, M. J. I.; Brown, W. R.; Calkins, M. L.; Challis, P.; Chornock, R.; Echevarria, L.; Eisenstein, D. J.; Everett, M. E.; Filippenko, A. V.; Flint, K.; Foley, R. J.; Freedman, D. .L.; Hamuy Wackenhut, Mario; Harding, P.; Hathi, N. P.; Hicken, M.; Hoopes, C.; Impey, C.; Jannuzi, B. T.; Jansen, R. A.; Jha, S.; Kaluzny, J.; Kannappan, S.; Kirshner, R. P.; Latham, D. W.; Lee, J. C.; Leonard, D. .C.; Li, W.; Luhman, K. L.; Martini, P.; Mathis, H.; Maza Sancho, José; Megeath, S. T.; Miller, L. R.; Minniti, D.; Olszewski, E. W.; Papenkova, M.; Phillips, M. M.; Pindor, B.; Sasselov, D. D.; Schild, R.; Schweiker, H.; Spahr, T.; Thomas-Osip, J.; Thompson, I.; Weisz, D.; Windhorst, R.; Zaritsky, D.

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2003-12-10

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PHOTOMETRY AND SPECTROSCOPY OF GRB 030329 AND ITS ASSOCIATED SUPERNOVA 2003dh: THE FIRST TWO MONTHSFormato de cita

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We present extensive optical and infrared photometry of the afterglow of gamma-ray burst (GRB) 030329 and its associated supernova (SN) 2003dh over the first two months after detection (2003March 30–May 29 UT). Optical spectroscopy from a variety of telescopes is shown and, when combined with the photometry, allows an unambiguous separation between the afterglow and SN contributions. The optical afterglow of the GRB is initially a power-law continuum but shows significant color variations during the first week that are unrelated to the presence of an SN. The early afterglow light curve also shows deviations from the typical power-law decay. An SN spectrum is first detectable 7 days after the burst and dominates the light after 11 days. The spectral evolution and the light curve are shown to closely resemble those of SN 1998bw, a peculiar Type Ic SN associated with GRB 980425, and the time of the SN explosion is close to the observed time of the GRB. It is now clear that at least some GRBs arise from core-collapse SNe.

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We also thank all the observers who provided their data and analysis through the GCN. KPNO, a part of the National Optical Astronomy Observatory, is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation. P. M. G. and S. T. H. acknowledge the support of NASA/LTSA grant NAG5-9364. D. J. E. was supported by NSF grant AST 00-98577 and by an Alfred P. Sloan Research Fellowship. D. M., L. I., and J. M. are supported by FONDAP Center for Astrophysics 15010003. J. K. was supported by KBN grant 5P03D004.21. J. C. L. acknowledges financial support from NSF grant AST 99-00789. P. M. was supported by a Carnegie Starr Fellowship. E. W. O. was partially supported by NSF grant AST 00- 98518. B. P. is supported by NASA grant NAG5-9274. R. A. W. and R. A. J. are supported by NASA grant NAG5-12460. D. C. L. acknowledges financial support provided by NASA through grant GO-9155 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The work of A. V. F.’s group at the University of California, Berkeley, is supported by NSF grant AST 03-07894, as well as by the Sylvia and Jim Katzman Foundation. KAIT was made possible by generous donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, and the Katzman Foundation.

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URI: https://repositorio.uchile.cl/handle/2250/126212
DOI: DOI: 10.1086/379228
ISSN: 0004-637X

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The Astrophysical Journal, 599:394–407, 2003 December 10

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