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A Clash of Clusters Provides New Clue to Dark Matter
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The metallicity of GRB host galaxies
Do long-duration GRBs (LGRBs) come from low-metallicity progenitors? Such a scenario is favored by the collapsar model, but is there supporting observational evidence? We will focus on the properties of the host galaxies of LGRBs, and how they are similar or different than comparable samples. Are observational signatures that LGRBs come from special environments believable and robust? What are the progenitor implications?
- Recommended Reading:
- (Fruchter et al. 2006): presents HST data comparing high-redshift LGRB hosts with hosts of core-collapse supernovae
- (Stanek et al. 2007): compares the metallicity distribution of the hosts of nearby LGRB (with SN) to comparable field galaxies from SDSS
- (Wolf & Podsiadlowski 2007): refines the Fruchter et al. analysis and connects their findings to metallicity
- Additional Reading (not required):
- (Woosley & Heger 2006): argues for rapid rotation, low mass loss and low metallicity for LGRB progenitors in the collapsar model
- (Berger et al. 2006): presents data for the host of LGRB 020127 -- going against the trend found by the other studies?
- (Modjaz et al. 2007): compares hosts of nearby broad-lined SN Ic "hypernovae" with GRB hosts
- (Prochaska 2006): cautions against concluding too much about this issue from absorption line spectroscopy of GRB afterglows themselves
Stanford High Performance Computing Conference IV