The Swift short gamma-ray burst rate density: implications for binary neutron star merger rates

Coward, D. M.; Howell, E. J.; Piran, Tsvi; Stratta, G.; Branchesi, M.; Bromberg, Omer; Gendre, B.; Burman, R.; Guetta, Dafne

doi:10.1111/j.1365-2966.2012.21604.x

Cited by 132 publications

(164 citation statements)

References 64 publications

(79 reference statements)

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“…Such an expected rate is consistent with the observed short-γ ray burst (sGRB) rate assuming a half-opening beaming angle of »  10 ( Guetta & Piran 2005, 2006Nakar et al 2006;Coward et al 2012;Wanderman & Piran 2015) and solar system abundance patterns of r-process elements (Bauswein et al 2014;Piran et al 2014;Shen et al 2015;van de Voort et al 2015;Wehmeyer et al 2015;Vangioni et al 2016). Based entirely on population synthesis models, since we have yet to observe a BH-NS system, we expect to detect 0.2-200 BH-NS systems per year with detectable distances of ∼1 Gpc.…”

Section: Introductionsupporting

confidence: 86%

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Hotokezaka

Nissanke

Hallinan

et al. 2016

ApJ

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113

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Mergers of binary neutron stars and black hole-neutron star binaries produce gravitational-wave(GW) emission and outflows with significant kinetic energies. These outflows result in radio emissions through synchrotron radiation. We explore the detectability of these synchrotron-generated radio signals by follow-up observations of GW merger events lacking a detection of electromagnetic counterparts in other wavelengths. We model radio light curves arising from (i) sub-relativistic merger ejecta and (ii) ultra-relativistic jets. The former produce radio remnants on timescales of a few years and the latter produce γ-ray bursts in the direction of the jet and orphan-radio afterglows extending over wider angles on timescales of weeks. Based on the derived light curves, we suggest an optimized survey at 1.4 GHz with five epochs separated by a logarithmic time interval. We estimate the detectability of the radio counterparts of simulated GW-merger events to be detected by advanced LIGO and Virgo by current and future radio facilities. The detectable distances for these GW merger events could be as high as 1 Gpc. Around 20%-60% of the long-lasting radio remnants will be detectable in the case of the moderate kinetic energy of 3 10 50 · erg and a circum-merger density of -0.1 cm 3 or larger, while 5%-20% of the orphan-radio afterglows with kinetic energy of 10 48 erg will be detectable. The detection likelihood increases if one focuses on the well-localizable GW events. We discuss the background noise due to radio fluxes of host galaxies and false positives arising from extragalactic radio transients and variable activegalacticnuclei, and we show that the quiet radio transient sky is of great advantage when searching for the radio counterparts.

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Section: Introductionsupporting

confidence: 86%

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Hotokezaka

Nissanke

Hallinan

et al. 2016

ApJ

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113

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“…These methods however, either suffer from sample incompleteness or require information, such as redshift, that might not be available for the majority of GRBs (e.g., Coward et al 2012Coward et al , 2013.…”

Section: Sample Selectionmentioning

confidence: 99%

“…Only a small fraction of heterogeneously-detected SGRBs have measured redshifts to this date (e.g., Coward et al 2012) and redshift completeness often limits studies to the brightest events (e.g., D 'Avanzo et al 2014). It is therefore, perceivable that the current observed redshift distribution of SGRBs is likely strongly biased and not representative of the entire population of SGRBs (e.g., Nakar 2007;Coward et al 2013).…”

Section: The Sgrb Rate Densitymentioning

confidence: 99%

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Short versus long gamma-ray bursts: a comprehensive study of energetics and prompt gamma-ray correlations

Shahmoradi

Nemiroff

2015

Monthly Notices of the Royal Astronomical Society

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We present the results of a comprehensive study of the luminosity function, energetics, prompt gamma-ray correlations, and classification methodology of short-hard and long-soft GRBs (SGRBs & LGRBs), based on observational data in the largest catalog of GRBs available to this date: BATSE catalog of 2702 GRBs. We find that: 1. The least-biased classification method of GRBs into short and long, solely based on prompt-emission properties, appears to be the ratio of the observed spectral peak energy to the observed duration (R = E p /T 90 ) with the dividing line at R 50[keV s −1 ]. 2. Once data is carefully corrected for the effects of the detection threshold of gammaray instruments, the population distribution of SGRBs and LGRBs can be individually well described as multivariate log-normal distribution in the 4-dimensional space of the isotropic peak gamma-ray luminosity, total isotropic gamma-ray emission, the intrinsic spectral peak energy, and the intrinsic duration. 3. Relatively large fractions of SGRBs and LGRBs with moderate-to-low spectral peak energies have been missed by BATSE detectors. 4. Relatively strong and highly significant intrinsic hardnessbrightness and duration-brightness correlations likely exist in both populations of SGRBs and LGRBs, once data is corrected for selection effects. The strengths of these correlations are very similar in both populations, implying similar mechanisms at work in both GRB classes, leading to the emergence of these prompt gamma-ray correlations.

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“…Our new rate estimates may have implications for SGRB progenitor models assuming they are powered (solely) by DNS or NSBH mergers. For instance, after accounting for the beaming effect, the rate of observed SGRBs, 3 − 30 Gpc −3 yr −1 (Coward et al 2012), can not be accounted for only by a population of NSBH mergers whereas the DNS merger rates may account for SGRBs with an appropriate beaming correction. The beaming angle for SGRBs is given as…”

Section: Discussionmentioning

confidence: 99%

Implications of Binary Black Hole Detections on the Merger Rates of Double Neutron Stars and Neutron Star–Black Holes

Gupta

Arun

Sathyaprakash

2017

ApJL

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We show that the inferred merger rate and chirp masses of binary black holes (BBHs) detected by advanced LIGO (aLIGO) can be used to constrain the rate of double neutron star (DNS) and neutron star -black hole (NSBH) mergers in the universe. We explicitly demonstrate this by considering a set of publicly available population synthesis models of Dominik et al. (2012a) and show that if all the BBH mergers, GW150914, LVT151012, GW151226, and GW170104, observed by aLIGO arise from isolated binary evolution, the predicted DNS merger rate may be constrained to be 2.3−471.0 Gpc −3 yr −1 and that of NSBH mergers will be constrained to 0.2 − 48.5 Gpc −3 yr −1 . The DNS merger rates are not constrained much but the NSBH rates are tightened by a factor of ∼ 4 as compared to their previous rates. Note that these constrained DNS and NSBH rates are extremely model dependent and are compared to the unconstrained values 2.3 − 472.5 Gpc −3 yr −1 and 0.2 − 218 Gpc −3 yr −1 , respectively, using the same models of Dominik et al. (2012a). These rate estimates may have implications for short Gamma Ray Burst progenitor models assuming they are powered (solely) by DNS or NSBH mergers. While these results are based on a set of open access population synthesis models which may not necessarily be the representative ones, the proposed method is very general and can be applied to any number of models thereby yielding more realistic constraints on the DNS and NSBH merger rates from the inferred BBH merger rate and chirp mass.

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The Swift short gamma-ray burst rate density: implications for binary neutron star merger rates

Cited by 132 publications

References 64 publications

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Short versus long gamma-ray bursts: a comprehensive study of energetics and prompt gamma-ray correlations

Implications of Binary Black Hole Detections on the Merger Rates of Double Neutron Stars and Neutron Star–Black Holes

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