The nu {cal F}_ν Peak Energy Distributions of Gamma--Ray Bursts Observed by BATSE

Details The nu {cal F}_ν Peak Energy Distributions of Gamma--Ray Bursts Observed by BATSE The nu {cal F}_ν Peak Energy Distributions of Gamma--Ray Bursts Observed by BATSE

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.5302m&link_type=abstract

American Astronomical Society, 186th AAS Meeting, #53.02; Bulletin of the American Astronomical Society, Vol. 27, p.886

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The majority of gamma-ray bursts exhibit a peak in their nu {cal F}_ν photon energy spectra at an energy E_p that is in the range of ~ 20--2000 keV available to the Large Area Detectors of the Burst and Transient Source Experiment (BATSE) on the Compton Gamma--Ray Observatory. If gamma--ray burst sources are at cosmological distances (d ~ 1 Gpc), then the spectra of dim bursts should be redshifted to lower energies relative to those of bright bursts. The magnitude of the shift is a function of the cosmological redshifts z of both the dim and bright burst sources and hence yields the range of redshift available to the bursts; this range is further constrained by considering cosmological model fits to the differential number--intensity distribution. We have produced photon energy spectra for ~ 400 bursts using data from BATSE to investigate if this expected shift in the nu {cal F}_ν peak is observed. We find that the mean peak energies of the burst spectra are correlated with intensity: lower intensity groups of burst spectra exhibit a lower average peak energy, although the distributions of E_p are quite wide. Denoting the redshift of an event with an observed photon flux P (photons cm(-2) s(-1) ) by z_P, we find that the maximicrons range consistent with the bursts of our sample is (1 + z1) / (1 + z100) ~ 2.2.

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