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

X. H. Cui; X. F. Wu; J. J. Wei; F. Yuan; W. K. Zheng; E. W. Liang; C. W. Akerlof; M. C.B. Ashley; H. A. Flewelling; E. Göüş; T. Güver; Kizilolu; T. A. McKay; S. B. Pandey; E. S. Rykoff; W. Rujopakarn; B. E. Schaefer; J. C. Wheeler; S. A. Yost

doi:10.1088/0004-637X/795/2/103

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

X. H. Cui^*, X. F. Wu, J. J. Wei, F. Yuan, W. K. Zheng, E. W. Liang, C. W. Akerlof, M. C.B. Ashley, H. A. Flewelling, E. Göüş, T. Güver, Kizilolu, T. A. McKay, S. B. Pandey, E. S. Rykoff, W. Rujopakarn, B. E. Schaefer, J. C. Wheeler, S. A. Yost

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

3 Citations (Scopus)

Abstract

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.

Original language	English
Article number	103
Journal	Astrophysical Journal
Volume	795
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/795/2/103
Publication status	Published - 10 Nov 2014

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Cui, X. H., Wu, X. F., Wei, J. J., Yuan, F., Zheng, W. K., Liang, E. W., Akerlof, C. W., Ashley, M. C. B., Flewelling, H. A., Göüş, E., Güver, T., Kizilolu, McKay, T. A., Pandey, S. B., Rykoff, E. S., Rujopakarn, W., Schaefer, B. E., Wheeler, J. C., & Yost, S. A. (2014). The optical luminosity function of gamma-ray bursts deduced from rotse-III observations. Astrophysical Journal, 795(2), Article 103. https://doi.org/10.1088/0004-637X/795/2/103

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title = "The optical luminosity function of gamma-ray bursts deduced from rotse-III observations",

abstract = "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.",

keywords = "gamma-ray burst: general, methods: statistical",

author = "Cui, {X. H.} and Wu, {X. F.} and Wei, {J. J.} and F. Yuan and Zheng, {W. K.} and Liang, {E. W.} and Akerlof, {C. W.} and Ashley, {M. C.B.} and Flewelling, {H. A.} and E. G{\"o}{\"u}{\c s} and T. G{\"u}ver and Kizilolu and McKay, {T. A.} and Pandey, {S. B.} and Rykoff, {E. S.} and W. Rujopakarn and Schaefer, {B. E.} and Wheeler, {J. C.} and Yost, {S. A.}",

year = "2014",

month = nov,

day = "10",

doi = "10.1088/0004-637X/795/2/103",

language = "English",

volume = "795",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

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Cui, XH, Wu, XF, Wei, JJ, Yuan, F, Zheng, WK, Liang, EW, Akerlof, CW, Ashley, MCB, Flewelling, HA, Göüş, E, Güver, T, Kizilolu, McKay, TA, Pandey, SB, Rykoff, ES, Rujopakarn, W, Schaefer, BE, Wheeler, JC & Yost, SA 2014, 'The optical luminosity function of gamma-ray bursts deduced from rotse-III observations', Astrophysical Journal, vol. 795, no. 2, 103. https://doi.org/10.1088/0004-637X/795/2/103

TY - JOUR

T1 - The optical luminosity function of gamma-ray bursts deduced from rotse-III observations

AU - Cui, X. H.

AU - Wu, X. F.

AU - Wei, J. J.

AU - Yuan, F.

AU - Zheng, W. K.

AU - Liang, E. W.

AU - Akerlof, C. W.

AU - Ashley, M. C.B.

AU - Flewelling, H. A.

AU - Göüş, E.

AU - Güver, T.

AU - Kizilolu,

AU - McKay, T. A.

AU - Pandey, S. B.

AU - Rykoff, E. S.

AU - Rujopakarn, W.

AU - Schaefer, B. E.

AU - Wheeler, J. C.

AU - Yost, S. A.

PY - 2014/11/10

Y1 - 2014/11/10

N2 - 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.

AB - 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.

KW - gamma-ray burst: general

KW - methods: statistical

UR - http://www.scopus.com/inward/record.url?scp=84908395958&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/795/2/103

DO - 10.1088/0004-637X/795/2/103

M3 - Article

SN - 0004-637X

VL - 795

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 103

ER -

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

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