Gamma-ray burst cosmology: Hubble diagram and star formation history

Wei, Jun-Jie; Wu, Xue-Feng

doi:10.1142/s0218271817300026

Cited by 19 publications

(13 citation statements)

References 91 publications

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“…This collapsar model implies that the GRB formation rate should in principle trace the cosmic star formation rate (SFR; Totani 1997;Wijers et al 1998;Lamb & Reichart 2000;Porciani & Madau 2001;Piran 2004;Zhang & Mészáros 2004;Zhang 2007). However, the Swif t observations seem to indicate that the GRB rate does not closely follow the ⋆ E-mail: gxlan@pmo.ac.cn (GXL) † E-mail: zhd@pmo.ac.cn (ZHD) ‡ E-mail: jjwei@pmo.ac.cn (JJW) § E-mail: xfwu@pmo.ac.cn (XFW) SFR but is actually enhanced by some unknown mechanisms at high-z (Daigne et al 2006;Guetta & Piran 2007; Le & Dermer 2007;Salvaterra & Chincarini 2007;Kistler et al 2008Kistler et al , 2009Li 2008;Yüksel et al 2008;Salvaterra et al 2009Salvaterra et al , 2012Campisi et al 2010;Qin et al 2010;Wanderman & Piran 2010;Cao et al 2011;Virgili et al 2011;Elliott et al 2012;Lu et al 2012;Robertson & Ellis 2012;Tan et al 2013;Wang 2013;Wei et al 2014;Tan & Wang 2015;Deng et al 2016;Wei & Wu 2017;Paul 2018). 1 Several evolution models have been proposed to explain the observed enhancement, such as 1 Using the C − statistical method proposed by Lynden-Bell (1971), Pescalli et al (2015) and Yu et al (2015) found a relative excess of the GRB formation rate with respect to the SFR at low redshifts.…”

Section: Introductionmentioning

confidence: 99%

The luminosity function and formation rate of a complete sample of long gamma-ray bursts

Guang-Xuan

Zeng

Wei

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the luminosity function and formation rate of long gamma-ray bursts (GRBs) by using a maximum likelihood method. This is the first time this method is applied to a well-defined sample of GRBs that is complete in redshift. The sample is composed of 99 bursts detected by the Swif t satellite, 81 of them with measured redshift and luminosity for a completeness level of 82%. We confirm that a strong redshift evolution in luminosity (with an evolution index of δ = 2.22 +0.32 −0.31 ) or in density (δ = 1.92 +0.20 −0.21 ) is needed in order to reproduce the observations well. But since the predicted redshift and luminosity distributions in the two scenarios are very similar, it is difficult to distinguish between these two kinds of evolutions only on the basis of the current sample. Furthermore, we also consider an empirical density case in which the GRB rate density is directly described as a broken power-law function and the luminosity function is taken to be non-evolving. In this case, we find that the GRB formation rate rises like (1 + z) 3.85 +0.48 −0.45 for z < ∼ 2 and is proportional to (1 + z) −1.07 +0.98 −1.12 for z > ∼ 2. The local GRB rate is 1.49 +0.63 −0.64 Gpc −3 yr −1 . The GRB rate may be consistent with the cosmic star formation rate (SFR) at z < ∼ 2, but shows an enhancement compared to the SFR at z > ∼ 2.

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Section: Introductionmentioning

confidence: 99%

The luminosity function and formation rate of a complete sample of long gamma-ray bursts

Guang-Xuan

Zeng

Wei

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…On the other hand, Hao & Yuan (2013a) (see also Wei et al 2016;Wei & Wu 2017) showed that PM-CSFR can reproduce very well the cumulative function of Long Gamma Ray Bursts -LGRBs from redshift z = 0 up to z ∼ 8. These authors used a Kolmogorov-Smirnov test, which showed that PM-CSFR presents p-value ∼ 0.92; that is, much better than the other CSFRs discussed in the literature.…”

Section: Cosmic Star Formation Rate-csfrmentioning

confidence: 98%

Connecting the Cosmic Star Formation Rate with the Local Star Formation

Gribel¹,

Miranda²,

Vilas-Boas³

2017

ApJ

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We present a model that unifies the cosmic star formation rate (CSFR), obtained through the hierarchical structure formation scenario, with the (Galactic) local star formation rate (SFR). It is possible to use the SFR to generate a CSFR mapping through the density probability distribution functions (PDFs) commonly used to study the role of turbulence in the star-forming regions of the Galaxy. We obtain a consistent mapping from redshift z ∼ 20 up to the present (z = 0). Our results show that the turbulence exhibits a dual character, providing high values for the star formation efficiency ( ε ∼ 0.32) in the redshift interval z ∼ 3.5 − 20 and reducing its value to ε = 0.021 at z = 0. The value of the Mach number (M crit ), from which ε rapidly decreases, is dependent on both the polytropic index (Γ) and the minimum density contrast of the gas. We also derive Larson's first law associated with the velocity dispersion ( V rms ) in the local star formation regions. Our model shows good agreement with Larson's law in the ∼ 10 − 50 pc range, providing typical temperatures T 0 ∼ 10 − 80 K for the gas associated with star formation. As a consequence, dark matter halos of great mass could contain a number of halos of much smaller mass, and be able to form structures similar to globular clusters. Thus, Larson's law emerges as a result of the very formation of large-scale structures, which in turn would allow the formation of galactic systems, including our Galaxy.

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“…. Gamma-ray bursts are promising high-redshift probes (i.e., Wang et al 2015Wang et al , 2016Wei & Wu 2017;Cao et al 2021;Demi-anski et al 2021;Hu et al 2021). This sample is a compilation of 31…”

Section: Grbsmentioning

confidence: 99%

High-redshift cosmography: Application and comparison with different methods

Hu,

Wang

2022

Preprint

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Cosmography is used in cosmological data processing in order to constrain the kinematics of the universe in a model-independent way. In this paper, we first investigate the effect of the ultraviolet (UV) and X-ray relation of a quasar on cosmological constraints. By fitting the quasar relation and cosmographic parameters simultaneously, we find that the 4σ deviation from the cosmological constant cold dark matter (ΛCDM) model disappears. Next, utilizing the Pantheon sample and 31 long gamma-ray bursts (LGRBs), we make a comparison among the different cosmographic expansions (z-redshift, y-redshift, E(y), log(1 + z), log(1 + z) + k i j , and Padé approximations) with the third-order and fourth-order expansions. The expansion order can significantly affect the results, especially for the y-redshift method. Through analysis from the same sample, the lower-order expansion is preferable, except the y-redshift and E(y) methods. For the y-redshift and E(y) methods, despite adopting the same parameterization of y = z/(1 + z), the performance of the latter is better than that of the former. Logarithmic polynomials, log(1 + z) and log(1 + z) + k i j , perform significantly better than z-redshift, y-redshift, and E(y) methods, but worse than Padé approximations. Finally, we comprehensively analyze the results obtained from different samples. We find that the Padé (2,1) method is suitable for both low and high redshift cases. The Padé (2,2) method performs well in a high-redshift situation. For the y-redshift and E(y) methods, the only constraint on the first two parameters (q 0 and j 0 ) is reliable.

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Gamma-ray burst cosmology: Hubble diagram and star formation history

Cited by 19 publications

References 91 publications

The luminosity function and formation rate of a complete sample of long gamma-ray bursts

The luminosity function and formation rate of a complete sample of long gamma-ray bursts

Connecting the Cosmic Star Formation Rate with the Local Star Formation

High-redshift cosmography: Application and comparison with different methods

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