Quantifying the Luminosity Evolution in Gamma‐Ray Bursts

Kocevski, D.; Liang, Edison

doi:10.1086/500816

Cited by 50 publications

(83 citation statements)

References 54 publications

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“…To this aim we apply a direct method (Lynden-Bell 1971) and its specific version already applied to GRBs, e.g. Yonetoku et al (2004Yonetoku et al ( , 2014, Kocevski & Liang (2006), Wu et al (2012), P15, Y15. This is the first time this method has been applied to a well-defined sample of GRBs that is complete in flux and 82% complete in redshift.…”

Section: Summary and Discussionmentioning

confidence: 99%

“…Chiang & Mukherjee 1998;Maloney & Petrosian 1999;Singal et al 2012Singal et al , 2013 and it has been applied to GRBs (Lloyd & Petrosian 1999;Kocevski & Liang 2006). Wanderman & Piran (2010) adopt a maximum likelihood estimator to derive the discrete luminosity function and cosmic formation rate.…”

Section: φ(L) and ψ(Z) Of Long Grbsmentioning

confidence: 99%

“…Yonetoku et al (2004Yonetoku et al ( , 2014, Kocevski & Liang (2006), and Wu et al (2012). This method is based on the assumption that the luminosity is independent of the redshift.…”

Section: Luminosity Function and Grb Formation Ratementioning

confidence: 99%

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The rate and luminosity function of long gamma ray bursts

Pescalli

Ghirlanda

Salvaterra

et al. 2016

A&A

100

121

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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 of completeness in redshift z (∼82%). We parametrise the redshift evolution of the GRB luminosity as L = L 0 (1 + z) k and we derive k = 2.5, consistently with recent estimates. The de-evolved luminosity function φ(L 0 ) of GRBs can be represented by a broken power law with slopes a = −1.32 ± 0.21 and b = −1.84 ± 0.24 below and above, respectively, a break luminosity L 0,b = 10 51.45±0.15 erg/s. Under the hypothesis of luminosity evolution we find that the GRB formation rate increases with redshift up to z ∼ 2, where it peaks, and then decreases in agreement with the shape of the cosmic star formation rate. We test the direct method through numerical simulations and we show that if it is applied to incomplete (both in redshift and/or flux) GRB samples it can misleadingly result in an excess of the GRB formation rate at low redshifts.

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Section: Summary and Discussionmentioning

confidence: 99%

Section: φ(L) and ψ(Z) Of Long Grbsmentioning

confidence: 99%

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The rate and luminosity function of long gamma ray bursts

Pescalli

Ghirlanda

Salvaterra

et al. 2016

A&A

100

121

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“…Given the lack of real redshifts, many authors instead sought to derive pseudo-redshifts using properties of the LGRB lightcurves in order to derive a LGRB luminosity function; the most popular of which included the lag-luminosity relationship (Norris, Marani & Bonnell 2000; Kocevski & Liang 2006), the variability-luminosity relationship (Fenimore & RamirezRuiz 2000;Reichart et al 2001;Lloyd-Ronning, Fryer & Ramirez-Ruiz 2002;Wei & Gao 2003); and the Amati relationship (Amati et al 2002;Atteia 2003;Firmani et al 2004;Yonetoku et al 2004;Salvaterra & Chincarini 2007;Salvaterra et al 2009). The large intrinsic scatter within these relationships produces however a redshift distribution that, whilst arguably it represents that of the true LGRB redshift distribution, also shows significant uncertainty in the fitted parameters.…”

Section: Introductionmentioning

confidence: 99%

The pulse luminosity function ofSwiftgamma-ray bursts

Amaral-Rogers¹,

Willingale²,

O’Brien³

2016

Mon. Not. R. Astron. Soc.

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The complete Swift BAT and XRT light curves of 118 GRBs with known redshifts were fitted using the physical model of GRB pulses by Willingale et al. (2010) to produce a total of 607 pulses. We compute the pulse luminosity function utilising three GRB formation rate models: a progenitor that traces the cosmic star formation rate density (CSFRD) with either a single population of GRBs, coupled to various evolutionary parameters, or a bimodal population of high and low luminosity GRBs; and a direct fit to the GRB formation rate excluding any a-priori assumptions.We find that a single population of GRB pulses with an evolving luminosity function is preferred over all other univariate evolving GRB models, or bimodal luminosity functions in reproducing the observed GRB pulse L-z distribution and that the magnitude of the evolution in brightness is consistent with studies that utilise only the brightest GRB pulses. We determine that the appearance of a GRB formation rate density evolution component is an artifact of poor parameterisation of the CSFRD at high redshifts rather than indicating evolution in the formation rate of early epoch GRBs. We conclude that the single brightest region of a GRB lightcurve holds no special property; by incorporating pulse data from the totality of GRB emission we boost the GRB population statistics by a factor of 5, rule out some models utilised to explain deficiencies in GRB formation rate modelling, and constrain more tightly some of the observed parameters of GRB behaviour.

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“…Previous works use the GRB redshift distribution to study the LF or GRB rate do not consider the missing redshift problem (e.g. Kocevski & Liang 2006;Salvaterra et al 2012). However, this selection effect is very important for these studies, as only ∼ 30% of Swift GRBs have measured redshifts.…”

Section: Introductionmentioning

confidence: 99%

Research on the redshift evolution of luminosity function and selection effect of GRBs

Tan

Wang

2015

Mon. Not. R. Astron. Soc.

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We study the redshift evolution of the luminosity function (LF) and redshift selection effect of long gamma-ray bursts (LGRBs). The method is to fit the observed peak flux and redshift distributions, simultaneously. To account for the complex triggering algorithm of Swift, we use a flux triggering efficiency function. We find evidence supporting an evolving LF, where the break luminosity scales as L b ∝ (1 + z) τ , with τ = 3.5 +0.4 −0.2 and τ = 0.8 +0.1 −0.08 for two kind of LGRB rate models. The corresponding local GRB rates arė R(0) = 0.86 +0.11 −0.08 yr −1 Gpc −3 andṘ(0) = 0.54 +0.25 −0.07 yr −1 Gpc −3 , respectively. Furthermore, by comparing the redshift distribution between the observed one and our mocked one, we find that the redshift detection efficiency of the flux triggered GRBs decreases with redshift. Especially, a great number of GRBs miss their redshifts in the redshift range of 1 < z < 2.5, where "redshift desert" effect may be dominated. More interestingly, our results show that the "redshift desert" effect is mainly introduced by the dimmer GRBs, e.g., P < 10 −7 erg/ s/ cm 2 , but has no effect on the brighter GRBs.

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Quantifying the Luminosity Evolution in Gamma‐Ray Bursts

Cited by 50 publications

References 54 publications

The rate and luminosity function of long gamma ray bursts

The rate and luminosity function of long gamma ray bursts

The pulse luminosity function ofSwiftgamma-ray bursts

Research on the redshift evolution of luminosity function and selection effect of GRBs

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