The Expected Rate of Gamma-Ray Burst Afterglows In Supernova Searches

Abstract

We predict the rate at which Gamma-Ray Burst (GRB) afterglows should be detected in supernova searches as a function of limiting flux. Although GRB afterglows are rarer than supernovae, they are detectable at greater distances because of their higher intrinsic luminosity. Assuming that GRBs trace the cosmic star formation history and that every GRB gives rise to a bright afterglow, we find that the average detection rate of supernovae and afterglows should be comparable at limiting magnitudes brighter than K=18. The actual rate of afterglows is expected to be somewhat lower since only a fraction of all gamma-ray selected GRBs were observed to have associated afterglows. However, the rate could also be higher if the initial gamma-ray emission from GRB sources is more beamed than their late afterglow emission. Hence, current and future supernova searches can place strong constraints on the afterglow appearance fraction and the initial beaming angle of GRB sources.

13 pages, submitted to ApJL

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• Orphan Afterglows of Collimated Gamma-Ray Bursts: Rate Predictions and Prospects for Detection
• Pair-Instability Supernovae at the Epoch of Reionization
• The difficulty in using orphan afterglows to measure gamma-ray burst beaming
• Environment of The Gamma-Ray Burst GRB971214 : A Giant H II Region surrounded by A Galactic Supershell
• Jetted Tidal Disruptions of Stars as a Flag of Intermediate Mass Black Holes at High Redshifts
• Gravitational wave frequencies and energies in hypernovae
• HST Imaging of MEGA Microlensing Candidates in M31