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

By D. Wanderman, T. Piran. 2014

227 citations recorded by the source corpus.

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 Bromberg2013 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(-1.9,+2.3)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(-0.4,+1.4) * 10^52~erg/s and power-law indices 0.95(-0.12,+0.12) and 2.0(-0.8,+1.0). 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 Bromberg2013. 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_b^-1 / 30) mergers took place in the Milky Way. If $0.025 m_\odot$ were ejected in each event this would have been sufficient to produce all the heavy r-process material in the Galaxy.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/75be99ece210b2c5747292a9a46c60a6018f550a

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Bing Zhang
2. B. Metzger
3. E. Berger
4. E. Quataert
5. B. Margalit
6. Pawan Kumar
7. T. Thompson
8. N. Langer

Citations in the corpus

• The physics of gamma-ray bursts & relativistic jets (2014, background): “Both conclusions are confirmed recently by Wanderman and Piran (2014), who suggested that the typical delay time scale is closer to 3 Gyr.”
• A Magnetar Origin for the Kilonova Ejecta in GW170817 (2018, background): “The local (z=0) rate of binary NS mergers as measured by Advanced LIGO after GW170817 is 1540BNS 1220 3200 = - + Gpc−3 yr−1, while the observed rate of short GRBs is 2 6SGRB » – Gpc−3 yr−1 (Wanderman & Piran 2015).”
• FERMI GBM OBSERVATIONS OF LIGO GRAVITATIONAL-WAVE EVENT GW150914 (2016, methodology): “This luminosity is an order of magnitude dimmer than the peak luminosities of the dimmest short GRBs in the sample analyzed by Wanderman & Piran (2015).”
• Fast Radio Bursts from Magnetars Born in Binary Neutron Star Mergers and Accretion Induced Collapse (2019, background): “The observed SGRB rate (Wanderman & Piran 2015) and an estimated beaming factor of ∼30 (Fong et al. 2015) leads to an estimate of the BNS merger rate at z0.”
• The impact of individual nuclear properties on $r$-process nucleosynthesis (2015, background): “ origin of all r-process elements seems to t some new numerical galactic simulations [149, 150], though the delay time for mergers to begin contributing to galactic nucleosynthesis is still uncertain [34]. The bulk of the r-process nucleosynthesis occurs from relatively cold material ejected in the ”
• Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, background): “Besides double NS mergers, it is expected that also mixed NS/BH mergers produce sGRBs. Adding our simulated mixed NS/BH merger-rate densities to our double NS merger-rate density, we estimate a total of RsGRB ' 25 to 86 yr−1 Gpc−3 (at z ' 0, i.e. using Rz=0 or RcSFR in Table 8), based on our default”
• THE LIGHT CURVE OF THE MACRONOVA ASSOCIATED WITH THE LONG–SHORT BURST GRB 060614 (2015, methodology): “Note that this rate is corrected for beaming, as such it is compatible with the un-beamed SGRB rate of 4± 2 Gpc−3 yr−1 (Wanderman & Piran 2015).”