Abstract
We predict the rate at which gamma-ray burst (GRB) afterglows should be detected in supernova (SN) searches as a function of limiting flux. Although GRB afterglows are rarer than supernovae (SNs), 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 SNs 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. Hence, current and future SN searches can place strong constraints on the afterglow appearance fraction of GRB sources.
Highlights
Since their discovery in the late 1960’s (Klebasadel et al 1973) through early 1997, Gamma-Ray Bursts (GRBs) had defied all attempts to determine their distance scale conclusively
We apply equation (4) to determine the average rate at which GRB afterglows, supernovae Type Ia (SNeIa), and SNeII should be detected in a field of 1 deg2 as a function of limiting flux
We have predicted the rate at which GRB afterglows should be detected in supernova searches as a function of limiting flux
Summary
1997), and radio (Frail et al 1997) counterparts to GRB sources. In particular, FeII and MgII absorption lines were detected at a redshift z = 0.835 in the spectrum of the optical counterpart to GRB970508 (Metzger et al 1997), demonstrating conclusively that this burst occurred at a cosmological distance with a redshift z > 0.835. The isotropy of the burst population and the flattening of their number counts, taken in combination with the fact that the first confirmed redshift for an optical counterpart is high, provides strong evidence that GRB sources are located at cosmological distances. Cosmological GRBs are at least 104 times rarer than Type II supernovae (SNeII) – possibly even ∼ 106 times rarer if GRBs occur primarily at high redshifts following the cosmic star formation history (Wijers et al 1997). In this Letter, we predict the detection frequency of GRB afterglows as a function of limiting flux at various observed wavelengths, and compare this rate with the analogous predictions for SNe Type Ia and Type II at high redshifts.
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
