On the possible association of
SN 1998bw and GRB 980425

Galama, T.J.; Vreeswijk, P.M.; Paradijs, J.A. van; Kouveliotou, C.; Augusteijn, T.; Patat, F.; Heise, J.; Zand, J. J. M. in ’t; Groot, P.; Wijers, R. A. M. J.; Pian, E.; Palazzi, E.; Frontera, F.; Masetti, N.

doi:10.1051/aas:1999311

Cited by 60 publications

(53 citation statements)

References 3 publications

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“…The light curves (LCs) of SE SNe are powered by the radioactive decay of 56 Ni, so the absolute magnitudes are closely related to the ejected 56 Ni masses, and in turn to the stellar progenitors and explosion mechanisms. Since the discovery of the apparent association of GRB 980425 with the peculiar Type Ic SN 1998bw (Galama et al 1999), and the confirmation by spectra of a SN 1998bw-like event associated with GRB 030329 (Garnavich et al 2003), SE SNe have become of intense interest in connection with gamma-ray bursts (GRBs). Contamination of high-redshift samples of SNe Ia by SE SNe is also an important issue (Homeier 2005).…”

Section: Introductionmentioning

confidence: 99%

Absolute Magnitude Distributions and Light Curves of Stripped-Envelope Supernovae

2006

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The absolute visual magnitudes of three Type IIb, 11 Type Ib, and 13 Type Ic supernovae (collectively known as stripped-envelope supernovae) are studied by collecting data on the apparent magnitude, distance, and interstellar extinction of each event. Weighted and unweighted mean absolute magnitudes of the combined sample, as well as various subsets of the sample, are reported. The limited sample size and the considerable uncertainties, especially those associated with extinction in the host galaxies, prevent firm conclusions regarding differences between the absolute magnitudes of supernovae of Types Ib and Ic, and regarding the existence of separate groups of overluminous and normal-luminosity stripped-envelope supernovae. The spectroscopic characteristics of the events of the sample are considered. Three of the four overluminous events are known to have had unusual spectra. Most but not all of the normal-luminosity events have had typical spectra. The light curves of stripped-envelope supernovae are collected and compared. Because SN 1994I in M51 was very well observed, it often is regarded as the prototypical Type Ic supernova, but it has the fastest light curve in the sample. Light curves are modeled by means of a simple analytical technique that, combined with a constraint on E/M from spectroscopy, yields internally consistent values of ejected mass, kinetic energy, and nickel mass.

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Section: Introductionmentioning

confidence: 99%

Absolute Magnitude Distributions and Light Curves of Stripped-Envelope Supernovae

2006

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“…Supernova (SN) 1998bw was discovered in April 1998 in a spiral arm of the face-on SB galaxy ESO 184-G82 at a redshift of z = 0.0085 (Galama et al 1998a). This exceptional type Ic supernova was born famous because of its positional and temporal coincidence with the gamma-ray burst GRB 980425 (Galama et al 1998b).…”

Section: Introductionmentioning

confidence: 99%

Supernova 1998bw – the final phases

Sollerman

Holland

Challis

et al. 2002

A&A

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114

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Abstract. The probable association with GRB 980425 immediately put SN 1998bw at the forefront of supernova research. Here, we present revised late-time BV RI light curves of the supernova, based on template images taken at the VLT. To follow the supernova to the very last observable phases we have used HST /STIS. Deep images taken in June and November 2000 are compared to images taken in August 2001. The identification of the supernova is firmly established. This allows us to measure the light curve to ∼1000 days past explosion. The main features are a rapid decline up to more than 500 days after explosion, with no sign of complete positron trapping from the 56 Co decay. Thereafter, the light curve flattens out significantly. One possible explanation is powering by more long lived radioactive isotopes, if they are abundantly formed in this energetic supernova.

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“…being an X-ray flash (XRF), with the fluences satisfying (Frontera et al 2000). Despite intense optical and near-S 1 S X g infrared (IR) follow-up observations initiated 6.5 and 8.4 hr after the burst, respectively (Klose 1998;Castro-Tirado et al 1998), no optical counterpart was found (Galama et al 1998;Wozniak 1998;Rhoads et al 1998;Bloom et al 1998;Schaefer et al 1998). The deep R-band observations carried out by Lindgren et al (1999) showed mag at 9.9 hr after the GRB.…”

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confidence: 99%

Photometric Redshift of the GRB 981226 Host Galaxy

Christensen

Hjorth

Gorosabel³

2005

ApJ

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No optical afterglow was found for the dark burst GRB 981226, and hence no absorption redshift has been obtained. We here use ground-based and space imaging observations to analyze the spectral energy distribution (SED) of the host galaxy. By comparison with synthetic template spectra, we determine the photometric redshift of the GRB 981226 host to be (68% confidence level). While the age-metallicity degeneracy z p 1.11 ‫ע‬ 0.06 phot for the host SED complicates the determination of accurate age, metallicity, and extinction, the photometric redshift is robust. The inferred z phot value is also robust compared to a Bayesian redshift estimator, which gives . The characteristics for this host are similar to other gamma-ray burst (GRB) hosts previously z p 0.94 ‫ע‬ 0.13 phot examined. Available low-resolution spectra show no emission lines at the expected wavelengths. The photometric redshift estimate indicates an isotropic energy release consistent with the Amati relation for this GRB, which had a spectrum characteristic of an X-ray flash.

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On the possible association of SN 1998bw and GRB 980425

Cited by 60 publications

References 3 publications

Absolute Magnitude Distributions and Light Curves of Stripped-Envelope Supernovae

Absolute Magnitude Distributions and Light Curves of Stripped-Envelope Supernovae

Supernova 1998bw – the final phases

Photometric Redshift of the GRB 981226 Host Galaxy

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