Detection of a Supernova Signature Associated with GRB 011121

By J. Bloom, Shrinivas R. Kulkarni, P. Price, D. Reichart, T. Galama, B. Schmidt, D. Frail, E. Berger, P. McCarthy, R. Chevalier and 13 more. 2002

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Using observations from an extensive monitoring campaign with the Hubble Space Telescope, we present the detection of an intermediate-time flux excess that is redder in color relative to the afterglow of GRB 011121, currently distinguished as the gamma-ray burst with the lowest known redshift. The red "bump," which exhibits a spectral rollover at ~7200 Å, is well described by a redshifted Type Ic supernova that occurred approximately at the same time as the gamma-ray burst event. The inferred luminosity is about half that of the bright supernova SN 1998bw. These results serve as compelling evidence for a massive star origin of long-duration gamma-ray bursts. Models that posit a supernova explosion weeks to months preceding the gamma-ray burst event are excluded by these observations. Finally, we discuss the relationship between spherical core-collapse supernovae and gamma-ray bursts.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b33c99ea3723e20ffa15d864bc2ec2ac4e14bf9b

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Citations in the corpus

The Supernova Gamma-Ray Burst Connection (2006, background): “…with Garnavich et al. (2003b) showing evidence that the brightness and color evolution resembled 1998S (a Type IIn; see also Meurs and Rebelo 2004) and Bloom et al. (2002b) showing consistency with a Ic-like curve interpolated between the faint and fast 1994I and the bright and slow 1998bw.”
Gamma-Ray Burst Energetics and the Gamma-Ray Burst Hubble Diagram: Promises and Limitations (2003, background): “Alternatively, especially in light of the detection of a supernova component with GRB 011121 (Bloom et al. 2002; Garnavich et al. 2003), we favor the hypothesis that all long-duration GRBs also lead to supernovae, with the diversity in GRB energies set by a progenitor-dependent ratio of the energy…”
Short-Duration Gamma-Ray Bursts (2013, background): “…significance (e.g.,Hjorth et al. 2003, Stanek et al. 2003, Pian et al. 2006, Berger et al. 2011), and on photometric re-brightenings on a timescale of∼ 15− 20 d post-burst that match Type Ic SN light curves in both brightness and color (toz∼ 1; e.g.,Bloom et al. 1999, 2002, Woosley & Bloom 2006).”
Gamma-Ray Bursts in the Swift Era (2007, background): “In some other cases, red SNe bumps have been observed in the late optical afterglow light curves (Bloom et al. 1999a, 2002; Reichart 1999; DellaValle et al. 2003; Fynbo et al. 2004; see a comprehensive sample in Zeh et al. 2004 and references therein).”
Photometry and Spectroscopy of GRB 030329 and Its Associated Supernova 2003dh: The First Two Months (2003, methodology): “A bum p in thelightcurvewasobserved both from the ground and with HST (Garnavich et al.2003a;Bloom et al.2002).”
Relativistic Jets in Collapsars (2002, background): “…Type I supernovae have also been seen in the optical afterglows of at least three GRBs (980326, Bloom et al. 1999; 970228, Reichart 1999; and 011121, Bloom et al. 2002, Galama et al. 2000) and GRB 980425 has been associated with an optical supernova, SN 1998bw (e.g., Iwamoto et al. 1998; Woosley,…”
The VLT-FLAMES Survey of Massive Stars: Observations in the Galactic Clusters NGC 3293, NGC 4755 and NGC 6611 ⋆ (2005, background): “…et al. 2004), and following recent discoveries that some of the most spectacular supernovae appear to be related to γ-ray bursts (e.g. Galama et al. 1998; Bloom et al. 2002; Hjorth et al. 2003), understanding the evolution of massive stars will gain even greater importance in the near future.”
The Type Ic Hypernova SN 2003dh/GRB 030329 (2003, background): “After the serendipitous discovery of SN 1998bw in coincidence with GRB 980425 (Galama et al. 1998), several other cases of possible SNe in GRBs have been reported (e.g., Bloom et al. 2002; Garnavich et al. 2003).”
Massive Stars in the Local Group: Implications for Stellar Evolution and Star Formation (2003, background): “Massive stars are believed by many to be the source of the most energetic phenomenon yet found, emitting gamma-ray bursts as they collapse into black holes (Woosley 1993, Bloom et al. 2002, Price et al. 2002).”
The afterglow of GRB 021004: surfing on density waves (2002, background): “Finally, if this interpretation is correct, the OA of GRB 021004 should not have a SN component in its lightcurve (see, e.g., Bloom et al. 2002), even though such a component would be in any case difficult to detect given the large redshift of the event.”
A Systematic Analysis of Supernova Light in Gamma-Ray Burst Afterglows (2003, methodology): “The results of our numerical procedure were compared with corresponding results published by Dado et al. (2002a) and Bloom et al. (2002b), and we found close agreement.”
The Propagation and Eruption of Relativistic Jets from the Stellar Progenitors of Gamma-Ray Bursts (2003, background): “In addition to the observed association with star-forming regions in galaxies (Vreeswijk et al. 2001; Bloom et al. 2002a; Gorosabel et al. 2003), ‘‘bumps’’ observed in the afterglows of many GRBs (Reichart 1999; Galama et al. 2000; Bloom et al. 2002b; Garnavich et al. 2003; Bloom 2004), spectral…”
Spectroscopic Discovery of the Supernova 2003dh Associated with GRB 030329 (2003, background): “At , GRB 011121/SN 2001kez p 0.36 was a relatively nearby burst that showed a late-time bump and color changes consistent with a supernova (Garnavich et al. 2003c; Bloom et al. 2002).”
Low-Luminosity Gamma-Ray Bursts as a Unique Population: Luminosity Function, Local Rate, and Beaming Factor (2006, background): “In some other cases, red SNe bumps were observed in the late optical afterglow light curves (Bloom et al. 1999, 2002; Della Valle et al. 2003; Fynbo 2004; see a comprehensive sample and references in Zeh et al. 2004).”
The physics of gamma-ray bursts & relativistic jets (2014, background): “This is consistent with the compact star merger scenarios, since compact stars born in asymmetric supernovae most likely received a “kick”, so that the binary system drifted away from the star forming regions when mergers occur (Bloom et al., 2002a).”
Events in the life of a cocoon surrounding a light, collapsar jet (2002, background): “…becomes optically thin, as a bright Ib/c supernova (some evidence for supernova-type emission has been found in: GRB 980326, Bloom et al. 1999; GRB 970228, Reichart 1999; GRB 990712, Björnsson et al. 2001; GRB 000911, Lazzati et al. 2001; GRB 011121, Bloom et al. 2002 and Garnavich et al. 2002).”