Measuring ΩM, ΩΛ and the SFR with class III GRBs

Details Measuring ΩM, ΩΛ and the SFR with class III GRBs Measuring ΩM, ΩΛ and the SFR with class III GRBs

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..662..438b&link_type=abstract

GAMMA-RAY BURST AND AFTERGLOW ASTRONOMY 2001: A Workshop Celebrating the First Year of the HETE Mission. AIP Conference Proceed

Astronomy and Astrophysics

Astronomy

Gamma-Ray Sources, Gamma-Ray Bursts, Star Formation, Observational Cosmology

Scientific paper

New evidences of the existence of three classes of GRBs are presented. In addition, it is shown the potential of class III GRBs for measuring the cosmological parameters ΩM and ΩΛ by comparing observed log N-log P distributions with the theoretical ones via a χ2 test. The result is that all three classes obtained from a neural network classification algorithm by Balastegui, Ruiz-Lapuente & Canal [1] (2001 BRC hereafter) do fit the cosmological distributions, whereas the cluster analysis classification deviates from them. To derive the theoretical distributions of GRBs, rates proportional to various proposed star formation rates (SFR) are used, and three different SFRs [2] [3] [4] are compared. We also show that in order to obtain acceptable values of ΩM and ΩΛ for class III GRBs, some evolution in luminosity has to be assumed. The fact that class III GRBs fit a rate proportional to the SFR makes them good candidates to come from collapsars, while the shallower distribution of classes I and II (with z < 2) rather suggests that they result from NS-NS or NS-BH mergings, the difference from the distribution of class III arising for the time-delay of the merging with respect to the SFR.

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