Demographics of the Galaxies Hosting Short-Duration Gamma-Ray Bursts

Fong, W.; Berger, E.; Chornock, R.; Margutti, R.; Levan, A. J.; Tanvir, N. R.; Tunnicliffe, Rachel; Czekala, Ian; Fox, D. B.; Perley, D. A.; Cenko, S. B.; Zauderer, B. A.; Laskar, T.; Persson, S. E.; Monson, Andrew; Kelson, D. D.; Birk, Christoph; Murphy, David; Servillat, Mathieu; Anglada, Guillem

doi:10.1088/0004-637x/769/1/56

Cited by 174 publications

(138 citation statements)

References 101 publications

(140 reference statements)

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“…For the extinction distribution, we notice that the host environment of neutron stars mergers is often compared to the host environment of SNe Ia since both types of systems are found in early-type and star-forming galaxies (Fong et al 2013). For this reason, we adopted for the extinction distribution P (A V ) = e −A V /τ V , with τ V = 0.334 ± 0.088 mag (Kessler et al 2009), which we label 'SN Ia extinction' scenario.…”

Section: Rate Measurementmentioning

confidence: 99%

An Empirical Limit on the Kilonova Rate from the DLT40 One Day Cadence Supernova Survey

Yang

Valenti

Cappellaro

et al. 2017

ApJL

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Binary neutron star mergers are important to understand stellar evolution, the chemical enrichment of the universe via the r-process, the physics of short gamma-ray bursts, gravitational waves and pulsars. The rates at which these coalescences happen is uncertain, but it can be constrained in different ways. One of those is to search for the optical transients produced at the moment of the merging, called a kilonova, in ongoing SN searches. However, until now, only theoretical models for kilonovae light curve were available to estimate their rates.The recent kilonova discovery AT 2017gfo/DLT17ck gives us the opportunity to constrain the rate of kilonovae using the light curve of a real event. We constrain the rate of binary neutron star mergers using the DLT40 Supernova search, and the native AT 2017gfo/DLT17ck light curve obtained with the same telescope and software system. Excluding AT 2017gfo/DLT17ck due to visibility issues, which was only discovered thanks to the aLIGO/aVirgo trigger,no other similar transients detected during 13 months of daily cadence observations of ∼ 2200 nearby (<40 Mpc) galaxies. We find that the rate of BNS mergers is lower than 0.47 -0.55 kilonovae per 100 years per 10 10 L B (depending on the adopted extinction distribution). In volume, this translates to < 0.99 × 10 −4 +0.19−0.15 , Mpc −3 yr −1 (SNe Ia-like extinction distribution), consistent with previous BNS coalescence rates.Based on our rate limit, and the sensitivity of aLIGO/aVirgo during O2, it is very unlikely that kilonova events are lurking in old pointed galaxy SN search datasets.

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Section: Rate Measurementmentioning

confidence: 99%

An Empirical Limit on the Kilonova Rate from the DLT40 One Day Cadence Supernova Survey

Yang

Valenti

Cappellaro

et al. 2017

ApJL

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“…With a redshift of z = 0.718 (Chornock & Berger 2010), the resulting isotropic γ-ray energy in the observed 20 keV-10 MeV range is E γ,iso ≈ 4.8 × 10 51 erg (Fong et al 2013).…”

Section: +103mentioning

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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“…Short GRBs are thought to be the very bright EM counterpart of binary neutron star or neutron star-black hole coalescence (Kocevski et al 2010;Fong et al 2013;Fong and Berger 2013). If a short GRB is accompanied by GW emission, joint GW+EM detection would confirm the binary nature of the short GRB engine as well as help constrain the binary parameters.…”

Section: Grb Joint Localizationsmentioning

confidence: 99%

Facilitating Follow-up of LIGO–Virgo Events Using Rapid Sky Localization

Chen

Holz

2017

ApJ

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Fast and effective localization of gravitational wave (GW) events could play a crucial role in identifying possible electromagnetic counterparts, and thereby help usher in an era of GW multi-messenger astronomy. We discuss an algorithm for accurate and very low latency (< 1 second) localization of GW sources using only the relative times of arrival, relative phases, and relative signal-to-noise ratios for pairs of detectors. The algorithm is independent of distances and masses to leading order, and can be generalized to all discrete sources detected by ground-based detector networks. Our approach, while developed independently, is similar to that of BAYESTAR with a few modifications in the algorithm which result in increased computational efficiency. For the LIGO two detector configuration (Hanford+Livingston) expected in late 2015 we find a median 50% (90%) localization of 143 deg 2 (558 deg 2 ) for binary neutron stars (for network SNR threshold of 12, corresponding to a horizon distance of ∼ 130 Mpc), consistent with previous findings. We explore the improvement in localization resulting from high SNR events, finding that the loudest out of the first 4 (or 10) events reduces the median sky localization area by a factor of 1.9 (3.0) for the case of 2 GW detectors, and 2.2 (4.0) for 3 detectors. We consider the case of multi-messenger joint detections in both the GW and the electromagnetic (EM) spectra. We specifically explore the case of independent, and possibly highly uncertain, localizations, showing that the joint localization area is significantly reduced. We also show that a prior on the binary inclination, potentially arising from GRB observations, has a negligible effect on GW localization. Our algorithm is simple, fast, and accurate, and may be of particular utility in the development of multi-messenger astronomy.

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Demographics of the Galaxies Hosting Short-Duration Gamma-Ray Bursts

Cited by 174 publications

References 101 publications

An Empirical Limit on the Kilonova Rate from the DLT40 One Day Cadence Supernova Survey

An Empirical Limit on the Kilonova Rate from the DLT40 One Day Cadence Supernova Survey

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

Facilitating Follow-up of LIGO–Virgo Events Using Rapid Sky Localization

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