2006) leading to the suggestion that young massive stars are the most likely progenitors (collapsars summarized in Woosley & Bloom 2006). Bloom, Kulkarni & Djorgovski 2002 Fruchter et al. LGRBs have been identified with star-forming galaxies with moderately low metallicity (e.g. ![]() GRBs can be categorized, largely according to their duration, as LGRBs and SGRBs, with the dividing line being at roughly 2 s ( Kouveliotou et al. This in turn provides luminosities and space densities for the bursts, allows possible means of measuring their collimation and ultimately may enable ‘smoking’ gun signatures of their progenitors to be uncovered, as was the case for LGRBs ( Hjorth et al. Afterglows provide precise positions, and hence a route to redshifts and identifying the host galaxies. Similarly, the first identifications of short GRB (SGRB) afterglows in 2005 opened a new window on this still enigmatic class of transient ( Gehrels et al. ![]() 1997) proved to be a pivotal moment in their study. The detection of the first fading afterglow from long gamma-ray bursts (LGRBs) ( Costa et al. Gamma-ray burst: individual: GRB 080905A 1 INTRODUCTION
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