Progenitor delay-time distribution of short gamma-ray bursts: Constraints from observations

Hao, J. M.; Yuan, Ye‐Fei

doi:10.1051/0004-6361/201321471

Cited by 21 publications

(32 citation statements)

References 38 publications

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“…This indicates that delay times are dominated by the gravitational radiation. On the other hand, such a delay time distribution has been widely and successfully applied in modeling the redshift distribution of SNe Ia originating from mergers of double WDs (Totani et al 2008;Maoz & Mannucci 2012) and of short GRBs originating from mergers of double NSs or a NS and a BH (Guetta & Piran 2006;Nakar et al 2006;Virgili et al 2011;Hao & Yuan 2013;Wanderman & Piran 2015). Furthermore, this power-law distribution could also be supported by the observations of six double NS systems (Champion et al 2004).…”

Section: The Rate Of Cbmsmentioning

confidence: 78%

Compact Binary Mergers and the Event Rate of Fast Radio Bursts

Cao

Xiao-Hong

2018

ApJ

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Fast radio bursts (FRBs) are usually suggested to be associated with mergers of compact binaries consisting of white dwarfs (WDs), neutron stars (NSs), or black holes (BHs). We test these models by fitting the observational distributions in both redshift and isotropic energy of 22 Parkes FRBs, where, as usual, the rates of compact binary mergers (CBMs) are connected with cosmic star formation rates by a power-law distributed time delay. It is found that the observational distributions can well be produced by the CBM model with a characteristic delay time from several ten to several hundred Myr and an energy function index 1.2 γ 1.7, where a tentative fixed spectral index β = 0.8 is adopted for all FRBs. Correspondingly, the local event rate of FRBs is constrained to (3 − 6) × 10 4 f −1 b (T /270s) −1 (A/2π) −1 Gpc −3 yr −1 for an adopted minimum FRB energy of E min = 3 × 10 39 erg, where f b is the beaming factor of the radiation, T is the duration of each pointing observation, and A is the sky area of the survey. This event rate, about an order of magnitude higher than the rates of NS-NS/NS-BH mergers, indicates that the most promising origin of FRBs in the CBM scenario could be mergers of WD-WD binaries. Here a massive WD could be produced since no FRB was found to be associated with a type Ia supernova. Alternatively, if actually all FRBs can repeat on a timescale much longer than the period of current observations, then they could also originate from a young active NS that forms from relatively rare NS-NS mergers and accretion-induced collapses of WD-WD binaries.

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Section: The Rate Of Cbmsmentioning

confidence: 78%

Compact Binary Mergers and the Event Rate of Fast Radio Bursts

Cao

Xiao-Hong

2018

ApJ

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“…When doing so one has to recall that different authors have used different definitions of the luminosity and these have to be normalized to ours. Hao & Yuan (2013) adopt an hierarchical structure formation model from Pereira & Miranda (2010), in which the SFR is derived using a Press-Schechter like formalism. That SFR peaks at z ≈ 3 and then drop very slowly as the redshift increases (by a factor ∼ 4 form z = 3 to z = 10), more resembling the Porciani & Madau (2001) SF2 SFR rather than the SFRs we consider here.…”

Section: Sfr Asmentioning

confidence: 99%

The rate, luminosity function and time delay of non-Collapsar short GRBs

Wanderman

Piran

2015

Monthly Notices of the Royal Astronomical Society

302

357

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We estimate the rate and the luminosity function of short (hard) Gamma-Ray Bursts (sGRBs) that are non-Collapsars, using the peak fluxes and redshifts of BATSE, Swift and Fermi GRBs. Following Bromberg et al. (2013) we select a sub-sample of Swift bursts which are most likely non-Collapsars. We find that these sGRBs are delayed relative to the global star formation rate (SFR) with a typical delay time of a 3−4 Gyr (depending on the SFR model). However, if two or three sGRB at high redshifts have been missed because of selection effects, a distribution of delay times of ∝ 1/t would be also compatible. The current event rate of these non-Collapsar sGRBs with L iso > 5×10 49 erg/s is 4.1 +2.3 −1.9 Gpc −3 yr −1 . The rate was significantly larger around z ∼ 1 and it declines since that time. The luminosity function we find is a broken power law with a break at 2.0 +1.4 −0.4 × 10 52 erg/s and power-law indices 0.95 +0.12 −0.12 and 2.0 +1.0 −0.8 . When considering the whole Swift sGRB sample we find that it is composed of two populations: One group (≈ 60% − 80% of Swift sGRBs) with the above rate and time delay and a second group (≈ 20% − 40% of Swift sGRBs) of potential "impostors" that follow the SFR with no delay. These two populations are in very good agreement with the division of sGRBs to non-Collapsars and Collapsars suggested recently by Bromberg et al. (2013). If non-Collapsar sGRBs arise from neutron star merger this rate suggest a detection rate of 3-100 yr −1 by a future gravitational wave detectors (e.g. Advanced Ligo/Virgo with detection horizon on 300 Mpc), and a co-detection with Fermi (Swift ) rate of 0.1-1 yr −1 (0.02-0.14 yr −1 ). We estimate that about 4 × 10 5 (f −1 b /30) mergers took place in the Milky Way. If 0.025m were ejected in each event this would have been sufficient to produce all the heavy r-process material in the Galaxy.

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“…The broad framework we adopt to model the redshift distribution is well established in the literature (Guetta & Piran 2005;Nakar et al 2006;Petrillo et al 2013;Hao & Yuan 2013;Wanderman & Piran 2015). Nevertheless, for the sake of completion, we describe it below.…”

Section: Modelling Redshift Distributionmentioning

confidence: 99%

Merger delay time distribution of extended emission short GRBs

Nikhil

Shahid

Resmi

2018

Monthly Notices of the Royal Astronomical Society

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The most popular progenitor model for short duration Gamma-Ray bursts (sGRBs) is the merger of two compact objects. However, the short GRB population exhibit a certain diversity: some bursts display an extended emission (EE), continuing in soft γ-rays for a few hundreds of seconds post the initial short pulse. It is currently unclear whether the origin of such bursts is linked to compact object mergers.Within the merger hypothesis, the redshift (z) distribution of short GRBs is influenced by the merger delay time, i.e., time elapsed between the merger and the formation of the binary star system, which is dominated by the time-scale for gravitational wave losses during the compact binary phase. We examine redshift distributions of short GRBs with extended emission to see whether their formation channel requires considerable delay post the star formation episode. Our results show that the z distribution of EE bursts is consistent with the merger model. We attempted to compare the delay time distribution of the EE and the non-EE short bursts. However, no statistically significant difference could be seen within the limited sample size.

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Progenitor delay-time distribution of short gamma-ray bursts: Constraints from observations

Cited by 21 publications

References 38 publications

Compact Binary Mergers and the Event Rate of Fast Radio Bursts

Compact Binary Mergers and the Event Rate of Fast Radio Bursts

The rate, luminosity function and time delay of non-Collapsar short GRBs

Merger delay time distribution of extended emission short GRBs

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