THE LIGHT CURVE OF THE MACRONOVA ASSOCIATED WITH THE LONG–SHORT BURST GRB 060614

By Zhiping Jin, Xiang Li, Z. Cano, S. Covino, Yizhong Fan, D. Wei. 2015

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The Swift-detected GRB 060614 was a unique burst that straddles an imaginary divide between long- and short-duration gamma-ray bursts (GRBs), and its physical origin has been heavily debated over the years. Recently, a distinct, very soft F814W-band excess at t ∼ 13.6 ?> days after the burst was identified in a joint-analysis of VLT and Hubble Space Telescope optical afterglow data of GRB 060614, which has been interpreted as evidence for an accompanying macronova (also called a kilonova). Under the assumption that the afterglow data in the time interval of 1.7–3.0 days after the burst are due to external FS emission, when this assumption is extrapolated to later times it is found that there is an excess of flux in several multi-band photometric observations. This component emerges at ∼4 days after the burst, and it may represent the first time that a multi-epoch/band light curve of a macronova has been obtained. The macronova associated with GRB 060614 peaked at t ≲ 4 ?> days after the burst, which is significantly earlier than that observed for a supernova associated with a long-duration GRB. Due to the limited data, no strong evidence for a temperature evolution is found. We derive a conservative estimate of the macronova rate of ∼ 16.3 − 8.2 + 16.3 Gpc − 3 yr − 1 , ?> implying a promising prospect for detecting the gravitational wave radiation from compact-object mergers by upcoming Advanced LIGO/VIRGO/KAGRA detectors (i.e., the rate is  GW ∼ 0.5 − 0.25 + 0.5 ( D / 200 Mpc ) 3 yr − 1 ?> ).

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/dce68c3c7799ff8a3212d2c62c7888b17c2ae54c

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Citations in the corpus

COMPACT BINARY MERGER RATES: COMPARISON WITH LIGO/VIRGO UPPER LIMITS (2015, result): “Finally, our merger rate densities for NS-NS mergers (50–150 Gpc−3 yr−1) are consistent with kilonova rate estimated from the most recent event reported to accompany a long-short GRB 060614: ∼> 10 Gpc −3 yr−1 (Jin et al. 2015).”
Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, background): “…as of now, several candidate kilonova/macronova events have been identified (Tanvir et al. 2013; de Ugarte Postigo et al. 2014; Berger et al. 2013; Yang et al. 2015; Jin et al. 2015), but their nature is still very ambiguous due to sparse observational data and uncertainties in theoretical models.”
The THESEUS space mission concept: science case, design and expected performances (2017, background): “Until the detection of GW170817, observational evidence of the macronova emission was obtained only in few cases during the follow-up campaigns of the optical afterglows of short GRBs (Tanvir et al., 2013; Jin et al., 2015).”
The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, methodology): “There have been a handful of observational searches for KN emission: GRB 050709 [424, 425]; GRB 051221A [426]; GRB 060614 [396, 427]; GRB 070724A [428, 429]; GRB 080503 [430, 431]; GRB 080905A [432]; and GRB 130603B [395, 433].”
The Emergence of a Lanthanide-rich Kilonova Following the Merger of Two Neutron Stars (2017, background): “The candidate KN/MNe discussed by Yang et al. (2015) and Jin et al. (2015, 2016) are more difficult to disentangle from the afterglow contribution, but have absolute AB magnitudes (roughly rest frame r-band) around −14 to −15 in the range 3–10 days post-burst, which is again in excess of the…”
The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks (2018, unknown): “…∼ 500− 1500 Gpc−3 yr−1 based on the analysis of Petrillo et al. 2013; ∼ 92− 1154 Gpc−3 yr−1 as estimated by Siellez et al. 2014, and 270+1580−180 Gpc −3 yr−1 according to Fong et al. 2015), but quite large with respect to the rate predicted from kilonovae (∼ 63+63−31 Gpc −3 yr−1, Jin et al. 2015).”
The cosmic merger rate of neutron stars and black holes (2018, methodology): “Alternative observational estimates of the DNS merger rate are based either on the rate of short gamma-ray bursts (Coward et al. 2012; Petrillo et al. 2013; Siellez et al. 2014; Fong et al. 2015), or on kilonova observations (Jin et al. 2015), or on the properties of Galactic DNSs (Kim et al. 2015).”