DETERMINING THE LUMINOSITY FUNCTION OF
                    <i>SWIFT</i>
                    LONG GAMMA-RAY BURSTS WITH PSEUDO-REDSHIFTS

Tan, Wei-Wei; Cao, Xuejun; Yu, Yun-Wei

doi:10.1088/2041-8205/772/1/l8

Cited by 26 publications

(20 citation statements)

References 45 publications

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“…Measuring the L z log log 1 -( ) + distribution by assuming that the GRB rate follows the SFR, Salvaterra et al (2012) reported k 2.3 0.6 b =  or strong comic evolution in GRB number density with a selected redshift-known sample of 52 Swift/BAT GRBs. Employing the L E p -relation to estimate the redshifts for a sample of 498 BAT GRBs, Tan et al (2013) obtained k 2 b~. The derived k and k b values from our analysis are systematically smaller than previous results by these authors.…”

Section: Conclusion and Discussioncontrasting

confidence: 57%

“…papers have no redshift information available (e.g., LloydRonning et al 2002;Yonetoku et al 2004;Kocevski & Liang 2006;Tan et al 2013) or have a small size or are collected from GRB surveys with instruments in different energy bands (e.g., Salvaterra et al 2012;Petrosian et al 2009). Before the Swift mission era, the large and uniform sample observed with the Burst and Transient Source Experiment(BATSE) on board theCompton Gamma-Ray Observatory(CGRO) is used for analysis.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…Thenk b can be estimated by fitting the observed L p and z distributions via Monte Carlo simulations under the assumption that the GRB rate follows the SFR. Using this approach, the k b derived from different samples is around 2 (Salvaterra et al 2012;Tan et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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Cosmic Evolution of Long Gamma-Ray Burst Luminosity

Deng¹,

Wang²,

Guo³

et al. 2016

ApJ

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The cosmic evolution of gamma-ray burst (GRB) luminosity is essential for revealing the GRB physics and for using GRBs as cosmological probes. We investigate the luminosity evolution of long GRBs with a large sample of 258 Swift/BAT GRBs. By describing the peak luminosity evolution of individual GRBs as L z 1, we get k 1.49 0.19 =  using the nonparametric τ statistics method without considering observational biases of GRB trigger and redshift measurement. By modeling these biases with the observed peak flux and characterizing the peak luminosity function of long GRBs as a smoothly broken powerlaw with a break that evolves as, we obtain k 1.14 b 0.47through simulations based on the assumption that the long GRB rate follows the star formation rate incorporatingthe cosmic metallicity history. The derived k and k b values are systematically smaller than thosereported in previous papers. By removing the observational biases of the GRB trigger and redshift measurement based on our simulation analysis, we generate mock complete samples of 258 and 1000 GRBs to examine how these biases affectthe τ statistics method. We get k 0.94 0.14 =  and k 0.80 0.09 =  for the two samples, indicating that these observational biases may lead to overestimatingthe k value. With the large uncertainty of k b derived from our simulation analysis, onecannot even convincingly argue for a robust evolution feature of the GRB luminosity.

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Section: Conclusion and Discussioncontrasting

confidence: 57%

Section: Conclusion and Discussionmentioning

confidence: 99%

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Cosmic Evolution of Long Gamma-Ray Burst Luminosity

Deng¹,

Wang²,

Guo³

et al. 2016

ApJ

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“…The correlations associated with GRBs have also been used to constrain the cosmological parameters (see Wang et al 2015, for a recent review). The relations between redshifts and other quantities have been used to derive the pseudo-redshift of GRBs (Wei & Gao 2003), and the pseudo-redshifts are used to derive the luminosity function (Tan et al 2013). The fundamental plane relation (Djorgovski & Davis 1987) is used to get the peculiar velocity (Colless et al 2001).…”

mentioning

confidence: 99%

Determining the Lorentz Factor and Viewing Angle of GRB 170817A

Zou

Wang

Moharana

et al. 2017

ApJL

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GRB 170817A is a weak short gamma-ray burst (GRB) accompanied by the gravitational wave (GW) event GW170817. It is believed, that an off beaming relativistic jet, produces this weak GRB. Here we use the E p,i − E iso and Γ − E iso relations to determine the Lorentz factor Γ and the viewing angle from the edge of the jet θ • . This corresponds to the on-axis E p,i = 415 +361 −167 keV and E iso = (2.447 ergs of the GRB, which is an intrinsically weak short GRB. Interestingly, the Doppler factor and the luminosity follow a universal relation from GRBs and blazars, which indicates they may share similar radiation mechanism.

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“…where C is a constant and γ is the observed spectral index in energy; see [5] for more details. The corrected luminosity is therefore:…”

Section: Observed Luminositymentioning

confidence: 99%

The Truncated Lognormal Distribution as a Luminosity Function for SWIFT-BAT Gamma-Ray Bursts

Zaninetti¹

2016

Galaxies

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Abstract:The determination of the luminosity function (LF) in Gamma ray bursts (GRBs) depends on the adopted cosmology, each one characterized by its corresponding luminosity distance. Here, we analyze three cosmologies: the standard cosmology, the plasma cosmology and the pseudo-Euclidean universe. The LF of the GRBs is firstly modeled by the lognormal distribution and the four broken power law and, secondly, by a truncated lognormal distribution. The truncated lognormal distribution fits acceptably the range in luminosity of GRBs as a function of the redshift.

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DETERMINING THE LUMINOSITY FUNCTION OF SWIFT LONG GAMMA-RAY BURSTS WITH PSEUDO-REDSHIFTS

Cited by 26 publications

References 45 publications

Cosmic Evolution of Long Gamma-Ray Burst Luminosity

Cosmic Evolution of Long Gamma-Ray Burst Luminosity

Determining the Lorentz Factor and Viewing Angle of GRB 170817A

The Truncated Lognormal Distribution as a Luminosity Function for SWIFT-BAT Gamma-Ray Bursts

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