Photometry and Spectroscopy of GRB 030329 and Its Associated Supernova 2003dh: The First Two Months

By Thomas Matheson, P. Garnavich, Krzysztof Zbigniew Stanek, D. Bersier, S. Holland, K. Krisciunas, N. Caldwell, P. Berlind, J. Bloom, M. Bolte and 49 more. 2003

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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 (2003 March 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.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b59576e32ec47eed739b7ac70528b3516d060bd8

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In Astronomy and Astrophysics

1. A. Filippenko
2. N. Smith
3. Ryan Chornock
4. Weidong Li
5. R. Kirshner
6. S. Smartt
7. Stan Woosley
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In Instrumentation

1. Stan Woosley
2. Weidong Li
3. A. Filippenko
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6. Z. Dai
7. R. Kirshner
8. Ryan Chornock

Citations in the corpus

• Determining the Type, Redshift, and Age of a Supernova Spectrum (2006, background): “…defined by the absence of elements (hydrogen and helium; although see Elmhamdi et al. 2006 for the presence of hydrogen in SNe Ib/c) in their atmospheres and thus form a heterogeneous class— which includes the supernovae associated with gamma-ray bursts (Kulkarni et al. 1998; Matheson et al. 2003).”
• Nearby Supernova Rates from the Lick Observatory Supernova Search. II. The Observed Luminosity Functions and Fractions of Supernovae in a Complete Sample (2010, methodology): “…suggest that they are rare (∼< 2% of the total CC SNe using Poisson statistics).5 Of the subclass of SNe Ibc-pec, the broad-lined SNe Ic deserve special attention because of their link to gammaray bursts (GRBs; e.g., Galama et al. 1998; Matheson et al. 2003; Modjaz et al. 2006; Pian et al. 2006).”
• A Systematic Analysis of Supernova Light in Gamma-Ray Burst Afterglows (2003, background): “The most convincing example is GRB 030329 (Peterson & Price 2003) at z ¼ 0:1685 (Greiner et al. 2003a) with spectral confirmation of supernova light in its afterglow (Hjorth et al. 2003; Kawabata et al. 2003; Matheson et al. 2003; Stanek et al. 2003).”
• Probing the cosmic reionization history and local environment of gamma‐ray bursts through radio dispersion (2003, background): “…the formation and collapse of massive stars (e.g. van Paradijs, Kouveliotou & Wijers 2000, Bloom, Kulkarni & Djorgovski 2002, Hjorth et al. 2003, Matheson et al. 2003) indicates that they can occur in significant numbers at early epochs, perhaps up to the formation era of the very first stars…”
• Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, unknown): “…(Galama et al. 1998; Iwamoto et al. 1998; Woosley et al. 1999; Nakamura et al. 2001a), GRB 030329/SN 2003dh (Stanek et al. 2003; Hjorth et al. 2003; Matheson et al. 2003; Mazzali et al. 2003; Lipkin et al. 2004; Deng et al. 2005), and GRB 031203/SN 2003lw (Thomsen et al. 2004; Gal-Yam et al. 2004;…”
• The Supernova Gamma-Ray Burst Connection (2006, background): “We leave the discussion of the modeling of SN2003dh to §3, but we emphasize here that even what should be the easiest-to-measure “observable” of a SN-GRB can be highly model dependent: the reported peak magnitude of SN2003dh differed by more than 1 magnitude (from 0.6 mag fainter to 0.5 mag brighter”
• Early-Time Photometry and Spectroscopy of the Fast Evolving SN 2006aj Associated with GRB 060218 (2006, background): “The risetime for SN 2006aj is the shortest ever measured for a SN Ic and is significantly shorter than for GRB 980425/SN 1998bw and GRB 030329/SN 2003dh (∼ 14 − 16 days: Galama et al. 1998; Matheson et al. 2003), while SN 2006aj is as almost bright as SN 1998bw.”
• Long γ-Ray Bursts and Type Ic Core-Collapse Supernovae Have Similar Locations in Hosts (2007, background): “They are the only type of supernova observed after the fading of the afterglow from long-duration γray bursts (Galama et al. 1998; Matheson et al. 2003; Stanek et al. 2003; Hjorth et al. 2003; Modjaz et al. 2006).”
• Gamma-Ray Bursts in the Swift Era (2009, background): “5 features identifiable as Hα, [OIII], Hβ and [OII] at z = 0.1687 (Kawabata et al. 2003, Matheson et al. 2003) making GRB 030329 the second nearest burst overall at the time and the nearest classical burst2.”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, background): “Figure 2: (a)The photometric (R-band) evolution of GRB 030329/SN 2003dh, from [6]; (b) the spectral evolution of GRB 030329/SN 2003dh, as compared with that of SN 1998bw, from [4].”