A comparison between short GRB afterglows and kilonova AT2017gfo: shedding light on kilonovae properties

Rossi, A.; Stratta, G.; Maiorano, E.; Spighi, D.; Masetti, N.; Palazzi, E.; Gardini, A.; Melandri, A.; Nicastro, L.; Pian, E.; Branchesi, M.; Dadina, M.; Testa, V.; Brocato, E.; Benetti, S.; Ciolfi, R.; Covino, S.; D’Elia, V.; Grado, A.; Izzo, L.; Perego, Albino; Piranomonte, S.; Salvaterra, R.; Selsing, J.; Tomasella, L.; Yang, S.; Vergani, D.; Amati, L.; Stephen, J. B.

doi:10.1093/mnras/staa479

Cited by 79 publications

(84 citation statements)

References 135 publications

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“…26 and other analyses, such as refs. 54,55 for GRB 160821B, have indicated that these SGRBs are consistent with having kilonovae present. On the other hand, GRB 060614 in particular has a number of possible interpretations, including a tidal disruption event 56 , a WD-NS system 57 or a long GRB 58 .…”

Section: Methodsmentioning

confidence: 93%

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: Methodsmentioning

confidence: 93%

Measuring the Hubble constant with a sample of kilonovae

et al. 2020

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“…Additionally, AT2017gfo is only one (well studied) event. The indication from cosmological GRBs is that KNe show considerable diversity in their emission (Fong et al 2017;Gompertz et al 2018;Ascenzi et al 2019;Rossi et al 2020), meaning that the model employed here may be too optimistic/pessimistic in its peak magnitude, or evolve faster/slower than any given future event. AT2017gfo is fainter than all but one sGRB KN candidate, but in several cases non-detections that probe deeper than the AT2017gfo models imply that there is room for a fainter, undetected population (Gompertz et al 2018;Pandey et al 2019).…”

Section: Factors That Influence Performancementioning

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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“…Thanks to the rich optical/infrared observations available, it is tempting to use AT2017gfo as a prototypical KN to set the fading (or rising) thresholds to photometrically select KN candidates based on their photometric evolution. However, AT2017gfo is unlikely to be representative for its class, as deep follow-up and joint afterglow and KN fits of short GRBs have demonstrated (Gompertz et al 2018;Ascenzi et al 2019;Rossi et al 2020). Instead, we chose thresholds for the fading rate based on a grid of KN models constructed with the Monte Carlo radiative transfer code POSSIS (Bulla 2019).…”

Section: Photometry and Candidate Selection Criteriamentioning

confidence: 99%

Constraining the Kilonova Rate with Zwicky Transient Facility Searches Independent of Gravitational Wave and Short Gamma-Ray Burst Triggers

Andreoni

Kool

Carracedo

et al. 2020

ApJ

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The first binary neutron star merger, GW170817, was accompanied by a radioactivity-powered optical/infrared transient called a kilonova. To date, no compelling kilonova has been found during optical surveys of the sky, independent of gravitational-wave triggers. In this work, we searched the first 23 months of the Zwicky Transient Facility (ZTF) data stream for candidate kilonovae in the form of rapidly evolving transients. We combined ZTF alert queries with forced point-spread-function photometry and nightly flux stacking to increase our sensitivity to faint and fast transients. Automatic queries yielded > 11, 200 candidates, 24 of which passed quality checks and strict selection criteria based on a grid of kilonova models tailored for both binary neutron star and neutron star-black hole mergers. None of the candidates in our sample was deemed a possible kilonova after thorough vetting, catalog cross-matching, and study of their color evolution. The sources that passed our selection criteria are dominated by Galactic cataclysmic variables. In addition, we identified two fast transients at high Galactic latitude, one of which is the confirmed afterglow of long-duration GRB 190106A, and the other is a possible cosmological afterglow. Using a survey simulation code, we constrained the kilonova rate for a range of models including top-hat and linearly decaying light curves and synthetic light curves obtained with radiative transfer simulations. For prototypical GW170817-like kilonovae, we constrain the rate to be R < 1775 Gpc −3 yr −1 at 95% confidence level by requiring at least 2 high-significance detections. By assuming a population of kilonovae with the same geometry and com

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A comparison between short GRB afterglows and kilonova AT2017gfo: shedding light on kilonovae properties

Cited by 79 publications

References 135 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)

Constraining the Kilonova Rate with Zwicky Transient Facility Searches Independent of Gravitational Wave and Short Gamma-Ray Burst Triggers

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