Gamma-ray burst rate: high-redshift excess and its possible origins

Virgili, F. J.; Zhang, Bing; Nagamine, Kentaro; Choi, June-Seek

doi:10.1111/j.1365-2966.2011.19459.x

Cited by 69 publications

(95 citation statements)

References 96 publications

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“…(1)- (3) or (4)). To make reliable judgements at high redshifts (z > 3), further observations able to study these relations at higher redshift are needed or other techniques used such as, Monte Carlo Markov chain (e.g., Virgili et al 2011), Principal Component Analysis (e.g., Ishida et al 2011), or simulations introduced into our model (e.g., Campisi et al 2010;de Souza et al 2011;Ishida et al 2011). Another important consideration is the assumptions and simplifications made at the beginning of the modelling, i.e., the stellar IMF, the LGRB luminosity function, the LGRB explosion mechanism and the GMF.…”

Section: Summary Of Results and Limitationsmentioning

confidence: 99%

“…The UL1 and UL2 samples show a preference for the metallicity limits L = 1.7 Z and 1.75 Z and the mass ranges (M 1 , M 2 ) = (8.0, 11.0) and (7.15, 11.85) respectively. These limits are very lax in comparison to the normal measured results of L ≤ 0.3 Z (see e.g., Yoon et al 2006;Salvaterra & Chincarini 2007;Campisi et al 2010;Virgili et al 2011) and the range of (M 1 , M 2 ) = (9.4, 9.6) (Savaglio et al 2009), and are interpreted as no limit. The predominant difference in our best-fit model compared to previous studies in this area is a result of the differences in the peak of the redshift number distribution whereby previous samples usually peaked at z ∼ 4, and required a metallicity cut-off (see Fig.…”

Section: Parameter Spacesmentioning

confidence: 99%

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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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Section: Summary Of Results and Limitationsmentioning

confidence: 99%

Section: Parameter Spacesmentioning

confidence: 99%

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

Elliott

Greiner

Khochfar

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…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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“…Article published by EDP Sciences A90, page 1 of 7 A&A 556, A90 (2013) Virgili et al (2011) discuss the possibility that the evolution of the GRB luminosity function break with redshift may explain this discrepancy. Observations also show differences in the population of GRB host galaxies compared to expectations for an unbiased star-formation tracer (Tanvir et al 2004;Fruchter et al 2006;Svensson et al 2010).…”

Section: Introductionmentioning

confidence: 99%

The high-redshift star formation rate derived from gamma-ray bursts: possible origin and cosmic reionization

Wang

2013

A&A

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The collapsar model of long gamma-ray bursts (GRBs) indicates that they may trace the star formation history, so long GRBs may be a useful tool for measuring the high-redshift star formation rate (SFR). The collapsar model explains GRB formation via the collapse of a rapidly rotating massive star with M > 30 M into a black hole, which may imply a decrease in SFR at high redshift. However, we find that the Swift GRBs during 2005 to 2012 are biased when tracing the SFR, including a factor about (1 + z) 0.5 , which agrees with recent results. After taking this factor, the SFR derived from GRBs does not show a steep drop up to z ∼ 9.4. We consider the GRBs produced by rapidly rotating metal-poor stars with low masses to explain the high-redshift GRB rate excess. The chemically homogeneous evolution scenario (CHES) of rapidly rotating stars with mass higher than 12 M is recognized as a promising path towards collapsars in connection with long GRBs. Our results indicate that the stars in the mass range 12 M < M < 30 M for low enough metallicity Z ≤ 0.004 with the GRB efficiency factor 10 −5 can fit the derived SFR with good accuracy. Combining these two factors, we find that the conversion efficiency from massive stars to GRBs is enhanced by a factor of 10, which may explain the excess of the high-redshift GRB rate. We also investigate the cosmic reionization history using the derived SFR. The GRB-inferred SFR would be sufficient to maintain cosmic reionization over 6 < z < 10 and reproduce the observed optical depth of Thomson scattering to the cosmic microwave background.

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Gamma-ray burst rate: high-redshift excess and its possible origins

Cited by 69 publications

References 96 publications

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

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

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

The high-redshift star formation rate derived from gamma-ray bursts: possible origin and cosmic reionization

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