The optical luminosity function of gamma-ray bursts deduced from ROTSE-III observations

Cui, X. H. and Wu, X. F. and Wei, J. J. and Yuan, F. and Zheng, W. K. and Liang, E. W. and Akerlof, C. W. and Ashley, M. C. B. and Flewelling, H. A. and Göğüş, Ersin and Güver, T. and Kızıloğlu, U. and Mckay, T. A. and Pandey, S. B. and Rykoff, E. S. and Rujopakarn, W. and Schaefer, B. E. and Wheeler, J. C. and Yost, S. A. (2014) The optical luminosity function of gamma-ray bursts deduced from ROTSE-III observations. Astrophysical Journal, 795 (2). ISSN 0004-637X (Print) 1538-4357 (Online)

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Official URL: http://dx.doi.org/10.1088/0004-637X/795/2/103


We present the optical luminosity function (LF) of gamma-ray bursts (GRBs) estimated from a uniform sample of 58 GRBs from observations with the Robotic Optical Transient Search Experiment III (ROTSE-III). Our GRB sample is divided into two sub-samples: detected afterglows (18 GRBs) and those with upper limits (40 GRBs). We derive R-band fluxes for these two sub-samples 100 s after the onset of the burst. The optical LFs at 100 s are fitted by assuming that the co-moving GRB rate traces the star formation rate. While fitting the optical LFs using Monte Carlo simulations, we take into account the detection function of ROTSE-III. We find that the cumulative distribution of optical emission at 100 s is well described by an exponential rise and power-law decay, a broken power law, and Schechter LFs. A single power-law (SPL) LF, on the other hand, is ruled out with high confidence.

Item Type:Article
Additional Information:Article Number: 103
Uncontrolled Keywords:gamma-ray burst: general; methods: statistical
Subjects:Q Science > QB Astronomy > QB460-466 Astrophysics
ID Code:25344
Deposited By:Ersin Göğüş
Deposited On:21 Dec 2014 20:26
Last Modified:02 Aug 2019 12:10

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