Infrared Emission from Kilonovae: The Case of the Nearby Short Hard Burst GRB 160821B

Kasliwal, M. M.; Korobkin, Oleg; Lau, Ryan M.; Wollaeger, Ryan; Fryer, Chris L.

doi:10.3847/2041-8213/aa799d

Cited by 74 publications

(80 citation statements)

References 50 publications

(61 reference statements)

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“…26 , which combined state-of-the-art afterglow and kilonova models, jointly fitting the observational data to determine whether there was any excess light from a kilonova. The analysis showed light curves consistent with kilonovae in the cases of GRB 150101B 27 , GRB 050709 28 , GRB 160821B 29 , and GRB 060614 30 . Naturally, the error bars on the kilonova parameters are larger for these objects than for GW170817, which have light curves with potentially significant contamination from the afterglow.…”

Section: Resultsmentioning

confidence: 86%

Measuring the Hubble constant with a sample of kilonovae

et al. 2020

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Kilonovae produced by the coalescence of compact binaries with at least one neutron star are promising standard sirens for an independent measurement of the Hubble constant (H 0). Through their detection via follow-up of gravitational-wave (GW), short gamma-ray bursts (sGRBs) or optical surveys, a large sample of kilonovae (even without GW data) can be used for H 0 contraints. Here, we show measurement of H 0 using light curves associated with four sGRBs, assuming these are attributable to kilonovae, combined with GW170817. Including a systematic uncertainty on the models that is as large as the statistical ones, we find H 0 ¼ 73:8 þ6:3 À5:8 km s À1 Mpc À1 and H 0 ¼ 71:2 þ3:2 À3:1 km s À1 Mpc À1 for two different kilonova models that are consistent with the local and inverse-distance ladder measurements. For a given model, this measurement is about a factor of 2-3 more precise than the standard-siren measurement for GW170817 using only GWs.

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Section: Resultsmentioning

confidence: 86%

Measuring the Hubble constant with a sample of kilonovae

et al. 2020

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“…KNe and sGRBs are already known to be linked to one another through coincident detections (Berger et al 2013;Tanvir et al 2013;Yang et al 2015;Jin et al 2016;Kasliwal et al 2017;Gompertz et al 2018;Jin et al 2018;Troja et al 2018a;Jin et al 2020;Lamb et al 2019b;Troja et al 2019;Jin et al 2020), with both BNS and NSBH KN models employed. KNe and sGRBs were also confirmed to be linked to BNS mergers by the detections of GRB 170817A (Abbott et al 2017b;Goldstein et al 2017;Hallinan et al 2017;Margutti et al 2017;Savchenko et al 2017;Troja et al 2017;Margutti et al 2018;Mooley et al 2018;Troja et al 2018b;D'Avanzo et al 2018;Lyman et al 2018) and the associated kilonova AT2017gfo (Blanchard et al 2017;Chornock et al 2017;Coulter et al 2017;Covino et al 2017;Cowperthwaite et al 2017;Drout et al 2017;Evans et al 2017;Hjorth et al 2017;Levan et al 2017;Nicholl et al 2017;Pian et al 2017;Smartt et al 2017;Soares-Santos et al 2017;Tanvir et al 2017;Villar et al 2017) alongside GW170817 (Abbott et al 2017a).…”

Section: Introductionmentioning

confidence: 99%

Searching for electromagnetic counterparts to gravitational-wave merger events with the prototype Gravitational-Wave Optical Transient Observer (GOTO-4)

Gompertz

Cutter

Steeghs

et al. 2020

Monthly Notices of the Royal Astronomical Society

100

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Abstract We report the results of optical follow-up observations of 29 gravitational-wave triggers during the first half of the LIGO-Virgo Collaboration (LVC) O3 run with the Gravitational-wave Optical Transient Observer (GOTO) in its prototype 4-telescope configuration (GOTO-4). While no viable electromagnetic counterpart candidate was identified, we estimate our 3D (volumetric) coverage using test light curves of on- and off-axis gamma-ray bursts and kilonovae. In cases where the source region was observable immediately, GOTO-4 was able to respond to a GW alert in less than a minute. The average time of first observation was 8.79 hours after receiving an alert (9.90 hours after trigger). A mean of 732.3 square degrees were tiled per event, representing on average 45.3 per cent of the LVC probability map, or 70.3 per cent of the observable probability. This coverage will further improve as the facility scales up alongside the localisation performance of the evolving gravitational-wave detector network. Even in its 4-telescope prototype configuration, GOTO is capable of detecting AT2017gfo-like kilonovae beyond 200 Mpc in favourable observing conditions. We cannot currently place meaningful electromagnetic limits on the population of distant ($\hat{D}_L = 1.3$ Gpc) binary black hole mergers because our test models are too faint to recover at this distance. However, as GOTO is upgraded towards its full 32-telescope, 2 node (La Palma & Australia) configuration, it is expected to be sufficiently sensitive to cover the predicted O4 binary neutron star merger volume, and will be able to respond to both northern and southern triggers.

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“…In addition, possible macronova emission was reported in this burst (Troja et al 2016;Kasliwal et al 2017).…”

Section: +021mentioning

confidence: 99%

Search for the signatures of a new-born black hole from the collapse of a supra-massive millisecond magnetar in short GRB light curves

Zhang

Lei

Zhang

et al. 2017

Monthly Notices of the Royal Astronomical Society

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'Internal plateau' followed by a sharp decay is commonly seen in short gamma-ray burst (GRB) light curves. The plateau component is usually interpreted as the dipole emission from a supra-massive magnetar, and the sharp decay may imply the collapse of the magnetar to a black hole (BH). Fall-back accretion onto the new-born BH could produce long-lasting activities via the Blandford-Znajek (BZ) process. The magnetic flux accumulated near the BH would be confined by the accretion disks for a period of time. As the accretion rate decreases, the magnetic flux is strong enough to obstruct gas infall, leading to a magnetically-arrested disk (MAD). Within this scenario, we show that the BZ process could produce two types of typical X-ray light curves: type I exhibits a long-lasting plateau, followed by a power-law decay with slopes ranging from 5/3 to 40/9; type II shows roughly a single power-law decay with slope of 5/3. The former requires low magnetic filed strength, while the latter corresponds to relatively high values. We search for such signatures of the new-born BH from a sample of short GRBs with an internal plateau, and find two candidates: GRB 101219A and GRB 160821B, corresponding to type II and type I light curve, respectively. It is shown that our model can explain the data very well.

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Infrared Emission from Kilonovae: The Case of the Nearby Short Hard Burst GRB 160821B

Cited by 74 publications

References 50 publications

Measuring the Hubble constant with a sample of kilonovae

Measuring the Hubble constant with a sample of kilonovae

Searching for electromagnetic counterparts to gravitational-wave merger events with the prototype Gravitational-Wave Optical Transient Observer (GOTO-4)

Search for the signatures of a new-born black hole from the collapse of a supra-massive millisecond magnetar in short GRB light curves

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