The BATSE-Swift luminosity and redshift distributions of short-duration GRBs

  title={The BATSE-Swift luminosity and redshift distributions of short-duration GRBs},
  author={Dafne Guetta and Tsvi Piran},
  journal={Astronomy and Astrophysics},
We compare the luminosity function and rate inferred from the BATSE peak flux distribution of short hard bursts (SHBs) with the redshift and luminosity distributions of SHBs observed by Swift /HETE II. While the Swift /HETE II SHB sample is incompatible with the SHB population that follows the star formation rate, it is compatible with an SHB rate that reflects a distribution of delay times after the SFR. This would be the case if SHBs were associated with binary neutron star mergers. The… Expand

Figures and Tables from this paper

Do long duration gamma ray bursts follow star formation
We compare the luminosity function and rate inferred from the BATSE (Burst and Transient Source Experiment) long bursts peak flux distribution with those inferred from the Swift peak fluxExpand
The rate, luminosity function and time delay of non-Collapsar short GRBs
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. FollowingExpand
Revisiting the event rate of short GRBs and estimating their detectable number within the Advanced LIGO horizon
The redshift and luminosity distributions of 36 Swift short GRBs are fitted by connecting their event rates with cosmic star formation rates by power-law distributed delayed times f(τ) ∝ τ, where aExpand
Binary neutron star merger rate via the luminosity function of short gamma-ray bursts
The luminosity function of short Gamma Ray Bursts (GRBs) is modelled by using the available catalogue data of all short GRBs (sGRBs) detected till October, 2017. The luminosities are estimated viaExpand
The rate and luminosity function of long Gamma Ray Bursts
We derive, adopting a direct method, the luminosity function and the formation rate of long Gamma Ray Bursts through a complete, flux-limited, sample of Swift bursts which has a high level ofExpand
Short gamma-ray bursts at the dawn of the gravitational wave era
We derive the luminosity function and redshift distribution of short Gamma Ray Bursts (SGRBs) using (i) all the available observer-frame constraints (i.e. peak flux, fluence, peak energy and durationExpand
GRB 080913 and GRB 090423 are the most distant gamma-ray bursts (GRBs) known to date, with spectroscopically determined redshifts of z = 6.7 and z = 8.1, respectively. The detection of bursts at thisExpand
Origins of short gamma-ray bursts deduced from offsets in their host galaxies revisited
The spatial distribution of short Gamma-ray bursts (GRBs) in their host galaxies provides us with an opportunity to investigate their origins. Based on the currently observed distribution of shortExpand
Estimation of compact binary coalescense rates from short gamma-ray burst redshift measurements
Short gamma-ray bursts are believed to originate from the merger of two compact objects. If this scenario is correct, these bursts will be accompanied by the emission of strong gravitational waves,Expand
Short gamma‐ray bursts from SGR giant flares and neutron star mergers: two populations are better than one
There is increasing evidence of a local population of short duration gamma-ray bursts (sGRB), but it remains to be seen whether this is a separate population to higher redshift bursts. Here we chooseExpand


The luminosity and redshift distributions of short-duration GRBs
Using the BATSE peak flux distribution we rederive the short GRBs luminosity function and compare it with the observed redshift distribution of long bursts. We show that both distributions areExpand
The Luminosity and Angular Distributions of Long‐Duration Gamma‐Ray Bursts
The realization that the total energy of gamma-ray bursts (GRBs) is correlated with their jet break angles motivates the search for a similar relation between the peak luminosity L and the jet breakExpand
The afterglow and elliptical host galaxy of the short γ-ray burst GRB 050724
Despite a rich phenomenology, γ-ray bursts (GRBs) are divided into two classes based on their duration and spectral hardness—the long-soft and the short-hard bursts. The discovery of afterglowExpand
On the Association of Gamma-Ray Bursts with Massive Stars: Implications for Number Counts and Lensing Statistics
Recent evidence appears to link gamma-ray bursts (GRBs) to star-forming regions in galaxies at cosmological distances. If short-lived massive stars are the progenitors of GRBs, the rate of events perExpand
Short gamma-ray bursts as a possible probe of binary neutron star mergers
We study the properties of short gamma-ray bursts (GRBs), based on the assumption that they are all connected to binary neutron star mergers, whose mechanism contains a large amount of uncertainty.Expand
The afterglow of GRB 050709 and the nature of the short-hard γ-ray bursts
The final chapter in the long-standing mystery of the γ-ray bursts (GRBs) centres on the origin of the short-hard class of bursts, which are suspected on theoretical grounds to result from theExpand
Observational Prospects for Afterglows of Short-Duration Gamma-Ray Bursts
If the efficiency for producing gamma rays is the same in short-duration (2 s) gamma-ray bursts (GRBs) as in long-duration GRBs, then the average kinetic energy per solid angle in short GRBs must beExpand
The Long and the Short of Gamma-Ray Bursts
We report evidence from the Third BATSE Gamma-Ray Burst Catalog that long (T90 > 10 s) and short (T90 < 10 s) gamma-ray bursts (GRBs) represent distinct source populations. Their spatialExpand
Discovery of the short γ-ray burst GRB 050709
Gamma-ray bursts (GRBs) fall into two classes: short-hard and long-soft bursts. The latter are now known to have X-ray and optical afterglows, to occur at cosmological distances in star-formingExpand
Optical emission from GRB 050709 : a short/hard GRB in a star-forming galaxy
Optical observations of the short/hard gamma-ray burst GRB 050709 are presented, the first such event with an identified optical counterpart, and it is shown that at least some short GRBs originate in a young population. Expand