Simulations on high-z long gamma-ray burst rate

Qin, Shu-Fu; Liang, En‐Wei; Lu, Rui-Jing; Wei, Jianyan; Zhang, Shuang‐Nan

doi:10.1111/j.1365-2966.2010.16691.x

Cited by 49 publications

(48 citation statements)

References 78 publications

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“…6. There is increasing evidence for an enhanced LGRB rate at z > 3 ( Daigne et al 2006;Kistler et al 2008;Wanderman & Piran 2010;Qin et al 2010), as expected from the increase in the specific star formation rate (SFR) with decreasing metallicity (Mannucci et al 2010). …”

Section: Formation Rate Of Stellar Black Holes As a Function Of Metalmentioning

confidence: 98%

Stellar black holes at the dawn of the universe

Mirabel

Dijkstra

Laurent

et al. 2011

A&A

251

292

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Context. It is well established that between 380 000 and 1 billion years after the Big Bang the Inter Galactic Medium (IGM) underwent a "phase transformation" from cold and fully neutral to warm (≈10 4 K) and ionized. Whether this phase transformation was fully driven and completed by photoionization by young hot stars is a question of topical interest in cosmology. Aims. We propose here that besides the ultraviolet radiation from massive stars, feedback from accreting black holes in high-mass X-ray binaries (BH-HMXBs) was an additional, important source of heating and reionization of the IGM in regions of low gas density at large distances from star-forming galaxies. Methods. We use current theoretical models on the formation and evolution of primitive massive stars of low metallicity, and the observations of compact stellar remnants in the near and distant universe, to infer that a significant fraction of the first generations of massive stars end up as BH-HMXBs. Results. The total number of energetic ionizing photons from an accreting stellar black hole in an HMXB is comparable to the total number of ionizing photons of its progenitor star. However, the X-ray photons emitted by the accreting black hole are capable of producing several secondary ionizations and the ionizing power of the resulting black hole could be greater than that of its progenitor. Feedback by the large populations of BH-HMXBs heats the IGM to temperatures of ≈10 4 K and maintains it ionized on large distance scales. Conclusions. BH-HMXBs determine the early thermal history of the universe and maintain it as ionized over large volumes of space in regions of low density. This has a direct impact on the properties of the faintest galaxies at high redshifts, the smallest dwarf galaxies in the local universe, and on the existing and future surveys at radio wavelengths of atomic hydrogen in the early universe.

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Section: Formation Rate Of Stellar Black Holes As a Function Of Metalmentioning

confidence: 98%

Stellar black holes at the dawn of the universe

Mirabel

Dijkstra

Laurent

et al. 2011

A&A

251

292

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“…Another possibility that could explain the excess of events at high redshift is to assume that the efficiency of massive stars of forming GRBs increases with redshift. A variable efficiency of forming GRBs could be an effect due to the metallicity of the environment (Daigne et al 2006;Salvaterra & Chincarini 2007;Qin et al 2010;Cao et al 2011;Virgili et al 2011). If one accepts that LGRBs are formed preferentially in a metal-poor medium, the association of (at least a fraction of them) with type Ibc supernovae is difficult to understand since SNIbc preferentially occur in galaxies with high metallicity (Prantzos & Boissier 2003;Prieto et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Revisiting the formation rate and redshift distribution of long gamma-ray bursts

Kanaan

Pacheco

2013

A&A

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Using a novel approach, the distribution of fluences of long gamma-ray bursts derived from the Swift-BAT catalog was reproduced by a jet-model characterized by the distribution of the total radiated energy in γ-rays and the distribution of the aperture angle of the emission cone. The best fit between simulated and observed fluence distributions permits one to estimate the parameters of the model. An evolution of the median energy of the bursts is required to adequately reproduce the observed redshift distribution of the events when the formation rate of γ-ray bursts follows the cosmic star formation rate. For our preferred model, the median jet energy evolves as E J ∝ e 0.5(1+z) and the mean expected jet energy is 3.0 × 10 49 erg, which agrees with the mean value derived from afterglow data. The estimated local formation rate is R grb = 290 Gpc −3 yr −1 , representing less than 9% of the local formation rate of type Ibc supernovae. This result also suggests that the progenitors of long gamma-ray bursts have masses ≥90 M when a Miller-Scalo initial mass function is assumed.

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“…, D com is the co-moving distance, η grb is the probability of stars resulting in a LGRB and then detected by an instrument, and δ is the power of proportionality for the CSFH to LGRBR (see e.g., Bromm & Loeb 2006;Daigne et al 2006;Young & Fryer 2007;Wolf & Podsiadlowski 2007;Salvaterra & Chincarini 2007;Kistler et al 2009;Campisi et al 2010;Qin et al 2010;Butler et al 2010;Wanderman & Piran 2010;Belczynski et al 2010;Virgili et al 2011;de Souza et al 2011;Wang & Dai 2011;Ishida et al 2011). The LGRB probability can be parameterised as (explained similarly in Bromm & Loeb 2006):…”

Section: Long Gamma-ray Burst Ratementioning

confidence: 99%

The longγ-ray burst rate and the correlation with host galaxy properties

Elliott

Greiner

Khochfar

et al. 2012

A&A

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Context. To answer questions on the start and duration of the epoch of reionisation, periods of galaxy mergers and properties of other cosmological encounters, the cosmic star formation history,ρ * or CSFH, is of fundamental importance. Using the association of long-duration gamma-ray bursts (LGRBs) with the death of massive stars and their ultra-luminous nature (>10 52 erg s −1 ), the CSFH can be probed to higher redshifts than current conventional methods. Unfortunately, no consensus has been reached on the manner in which the LGRB rate,ρ grb or LGRBR, traces the CSFH, leaving many of the questions mentioned mostly unexplored by this method. Aims. Observations by the gamma-ray burst near-infrared detector (GROND) over the past 4 years have, for the first time, acquired highly complete LGRB samples. Driven by these completeness levels and new evidence of LGRBs also occurring in more massive and metal rich galaxies than previously thought, the possible biases of theρ grb -ρ * connection are investigated over a large range of galaxy properties. Methods. The CSFH is modelled using empirical fits to the galaxy mass function and galaxy star formation rates. Biasing the CSFH by means of metallicity cuts, mass range boundaries, and other unknown redshift dependencies of the formρ grb ∝ρ * (1 + z) δ , aρ grb is generated and compared to the highly complete GROND LGRB sample. Results. It is found that there is no strong preference for a metallicity cut or fixed galaxy mass boundaries and that there are no unknown redshift effects (δ = 0), in contrast to previous work which suggest values of Z/Z ∼ 0.1−0.3. From the best-fit models obtained, we predict that ∼1.2% of the LGRB burst sample exists above z = 6. Conclusions. The linear relationship betweenρ grb andρ * suggested by our results implies that redshift biases present in previous LGRB samples significantly affect the inferred dependencies of LGRBs on their host galaxy properties. Such biases can lead to, for example, an interpretation of metallicity limitations and evolving LGRB luminosity functions.

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Simulations on high-z long gamma-ray burst rate

Cited by 49 publications

References 78 publications

Stellar black holes at the dawn of the universe

Stellar black holes at the dawn of the universe

Revisiting the formation rate and redshift distribution of long gamma-ray bursts

The longγ-ray burst rate and the correlation with host galaxy properties

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