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Cosmological tests using gamma-ray bursts, the star formation rate and possible abundance evolution
Wei, Jun-Jie1,2; Wu, Xue-Feng1,3,4; Melia, Fulvio5,6; Wei, Da-Ming1,7; Feng, Long-Long1,3
2014-04-01
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
ISSN0035-8711
Volume439Issue:4Pages:3329-3341
AbstractThe principal goal of this paper is to use attempts at reconciling the Swift long gamma-ray bursts (LGRBs) with the star formation history (SFH) to compare the predictions of Lambda cold dark matter (Lambda CDM) with those in the R-h = ct Universe. In the context of the former, we confirm that the latest Swift sample of GRBs reveals an increasing evolution in the GRB rate relative to the star formation rate (SFR) at high redshifts. The observed discrepancy between the GRB rate and the SFR may be eliminated by assuming a modest evolution parametrized as (1 + z)(0.8) - perhaps indicating a cosmic evolution in metallicity. However, we find a higher metallicity cut of Z = 0.52 Z(circle dot) than was seen in previous studies, which suggested that LGRBs occur preferentially in metal-poor environments, i.e. Z similar to 0.1-0.3 Z(circle dot). We use a simple power-law approximation to the high-z ( greater than or similar to 3.8) SFH, i.e. R-SF proportional to [(1 + z)/4.8](alpha), to examine how the high-z SFR may be impacted by a possible abundance evolution in the Swift GRB sample. For an expansion history consistent with Lambda CDM, we find that the Swift redshift and luminosity distributions can be reproduced with reasonable accuracy if alpha = -2.41(-2.09)(+1.87). For the R-h = ct Universe, the GRB rate is slightly different from that in Lambda CDM, but also requires an extra evolutionary effect, with a metallicity cut of Z = 0.44 Z(circle dot). Assuming that the SFR and GRB rate are related via an evolving metallicity, we find that the GRB data constrain the slope of the high-z SFR in R-h = ct to be alpha = -3.60(-2.45)(+2.45). Both cosmologies fit the GRB/SFR data rather well. However, in a one-on-one comparison using the Akaike information criterion, the best-fitting R-h = ct model is statistically preferred over the best-fitting Lambda CDM model with a relative probability of similar to 70 per cent versus similar to 30 per cent.
KeywordMethods: Statistical Stars: Formation Gamma-ray Burst: General Cosmology: Observations Cosmology: Theory
WOS HeadingsScience & Technology ; Physical Sciences
DOI10.1093/mnras/stu166
WOS KeywordCOSMIC METALLICITY EVOLUTION ; LUMINOSITY FUNCTION ; HIGH-REDSHIFT ; HOST GALAXIES ; FORMATION HISTORY ; CHEMICAL EVOLUTION ; FORMING GALAXIES ; ALERT TELESCOPE ; MASSIVE STARS ; CT UNIVERSE
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Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000334115400011
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Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/10612
Collection南极天文中心
Affiliation1.Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China
2.Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China
3.Chinese Ctr Antarctic Astron, Nanjing 210008, Peoples R China
4.Nanjing Univ, Purple Mt Observ, Joint Ctr Particle Nucl Phys & Cosmol, Nanjing 210008, Peoples R China
5.Univ Arizona, Program Appl Math, Dept Phys, Tucson, AZ 85721 USA
6.Univ Arizona, Dept Astron, Tucson, AZ 85721 USA
7.Chinese Acad Sci, Key Lab Dark Matter & Space Astron, Nanjing 210008, Peoples R China
Recommended Citation
GB/T 7714
Wei, Jun-Jie,Wu, Xue-Feng,Melia, Fulvio,et al. Cosmological tests using gamma-ray bursts, the star formation rate and possible abundance evolution[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2014,439(4):3329-3341.
APA Wei, Jun-Jie,Wu, Xue-Feng,Melia, Fulvio,Wei, Da-Ming,&Feng, Long-Long.(2014).Cosmological tests using gamma-ray bursts, the star formation rate and possible abundance evolution.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,439(4),3329-3341.
MLA Wei, Jun-Jie,et al."Cosmological tests using gamma-ray bursts, the star formation rate and possible abundance evolution".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 439.4(2014):3329-3341.
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