TY - JOUR
T1 - The Swift short gamma-ray burst rate density
T2 - 2012 Gamma-Ray Bursts Conference, GRB 2012
AU - Coward, David M.
AU - Howell, Eric
AU - Piran, Tsvi
AU - Stratta, Giulia
AU - Branchesi, Marica
AU - Bromberg, Omer
AU - Gendre, Bruce
AU - Burman, Ronald
AU - Guetta, Dafne
N1 - Publisher Copyright:
© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence.
PY - 2012
Y1 - 2012
N2 - Presently only 30% of short gamma ray bursts (SGRBs) have accurate redshifts, and this sample is highly biased by the limited sensitivity of Swift to detect SGRBs. We account for the dominant biases to calculate a realistic SGRB rate density out to z = 0.5 using the Swift sample of peak fluxes, redshifts, and those SGRBs with a beaming angle constraint from X-ray/optical observations. Assuming a significant fraction of binary neutron star mergers produce SGRBs, we calculate lower and upper detection rate limits of (1-180) per Yr by an advanced LIGO and Virgo coincidence search. Our detection rate is compatible with extrapolations using Galactic pulsar observations and population synthesis.
AB - Presently only 30% of short gamma ray bursts (SGRBs) have accurate redshifts, and this sample is highly biased by the limited sensitivity of Swift to detect SGRBs. We account for the dominant biases to calculate a realistic SGRB rate density out to z = 0.5 using the Swift sample of peak fluxes, redshifts, and those SGRBs with a beaming angle constraint from X-ray/optical observations. Assuming a significant fraction of binary neutron star mergers produce SGRBs, we calculate lower and upper detection rate limits of (1-180) per Yr by an advanced LIGO and Virgo coincidence search. Our detection rate is compatible with extrapolations using Galactic pulsar observations and population synthesis.
UR - http://www.scopus.com/inward/record.url?scp=85052373717&partnerID=8YFLogxK
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AN - SCOPUS:85052373717
SN - 1824-8039
VL - 2012-May
JO - Proceedings of Science
JF - Proceedings of Science
Y2 - 7 May 2012 through 11 May 2012
ER -