Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 486, Issue 1, Pages 672-690Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz891
Keywords
gravitational waves; nuclear reactions, nucleosynthesis, abundances; gamma-ray burst: general
Categories
Funding
- 2017 Kavli Summer Program in Astrophysics at the Niels Bohr Institute in Copenhagen
- Kavli Foundation
- Danish National Research Foundation (DNRF)
- Niels Bohr International Academy
- UCMEXUS-CONACYT Doctoral Fellowship
- David and Ellen Lee Postdoctoral Fellowship at the California Institute of Technology
- European Union [749145]
- NASA [NNG17PX03C]
- NSF [AST-1518052]
- Gordon & Betty Moore Foundation
- Heising-Simons Foundation
- Alfred P. Sloan Foundation
- David and Lucile Packard Foundation
- Niels Bohr Professorship from the DNRF
- DARK
- Marie Curie Actions (MSCA) [749145] Funding Source: Marie Curie Actions (MSCA)
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The combined detection of a gravitational-wave signal, kilonova, and short gamma-ray burst (sGRB) from GW170817 marked a scientific breakthrough in the field of multimessenger astronomy. But even before GW170817, there have been a number of sGRBs with possible associated kilonova detections. In this work, we re-examine these ` historical' sGRB afterglows with a combination of state-of-the-art afterglow and kilonova models. This allows us to include optical/near-infrared synchrotron emission produced by the sGRB as well as ultraviolet/optical/near-infrared emission powered by the radioactive decay of r-process elements (i.e. the kilonova). Fitting the light curves, we derive the velocity and the mass distribution as well as the composition of the ejected material. The posteriors on kilonova parameters obtained from the fit were turned into distributions for the peak magnitude of the kilonova emission in different bands and the time at which this peak occurs. From the sGRB with an associated kilonova, we found that the peak magnitude in H bands falls in the range [-16.2, -13.1] (95 per cent of confidence) and occurs within 0.8-3.6 d after the sGRB prompt emission. In g band instead we obtain a peak magnitude in range [-16.8, -12.3] occurring within the first 18 h after the sGRB prompt. From the luminosity distributions of GW170817/AT2017gfo, kilonova candidates GRB130603B, GRB050709, and GRB060614 (with the possible inclusion of GRB150101B, GRB050724A, GRB061201, GRB080905A, GRB150424A, and GRB160821B) and the upper limits from all the other sGRBs not associated with any kilonova detection we obtain for the first time a kilonova luminosity distribution in different bands.
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