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On the FRB luminosity function - -II. Event rate density
Luo, Rui1,2,3; Men, Yunpeng1,2; Lee, Kejia1,4; Wang, Weiyang5,6; Lorimer, D. R.7,8; Zhang, Bing9
2020-05-01
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
ISSN0035-8711
Volume494Issue:1Pages:665-679
AbstractThe luminosity function of Fast Radio Bursts (FRBs), defined as the event rate per unit cosmic co-moving volume per unit luminosity, may help to reveal the possible origins of FRBs and design the optimal searching strategy. With the Bayesian modelling, we measure the FRB luminosity function using 46 known FRBs. Our Bayesian framework self-consistently models the selection effects, including the survey sensitivity, the telescope beam response, and the electron distributions from Milky Way/ the host galaxy/ local environment of FRBs. Different from the previous companion paper, we pay attention to the FRB event rate density and model the event counts of FRB surveys based on the Poisson statistics. Assuming a Schechter luminosity function form, we infer (at the 95 per cent confidence level) that the characteristic FRB event rate density at the upper cut-off luminosity L* = 2.9(-1.7)(+11.9) x 10(44) erg s(-1 )is phi* = 339(-313)(+1074) Gpc(-3) yr(-1), the power-law index is alpha = -1.79(-0.35)(+0.31), and the lower cut-off luminosity is L-0 <= 9.1 x 10(41) erg s(-1). The event rate density of FRBs is found to be 3.5(-2.4)(+5.7 )x 10(4 )Gpc(-3) yr(-1) above 10(42) erg s(-1), 5.0(-2.3)(+3.2) x 10(3) Gpc(-3) yr(-1) above 10(43 )erg s(-1), and 3.7(-2.0)(+3.5) x 10(2) Gpc(-3) yr(-1) above 10(44) erg s(-1). As a result, we find that, for searches conducted at 1.4 GHz, the optimal diameter of single-dish radio telescopes to detect FRBs is 30-40 m. The possible astrophysical implications of the measured event rate density are also discussed in the current paper.
Keywordmethods: data analysis methods: statistical stars: luminosity function, mass function
Funding OrganizationNSFC ; NSFC ; TianShanChuangXinTuanDui ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; Max-Planck Partner Group ; MoST grant ; MoST grant ; CAS ; CAS ; National Science Foundation ; National Science Foundation ; NSFC ; NSFC ; TianShanChuangXinTuanDui ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; Max-Planck Partner Group ; MoST grant ; MoST grant ; CAS ; CAS ; National Science Foundation ; National Science Foundation ; NSFC ; NSFC ; TianShanChuangXinTuanDui ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; Max-Planck Partner Group ; MoST grant ; MoST grant ; CAS ; CAS ; National Science Foundation ; National Science Foundation ; NSFC ; NSFC ; TianShanChuangXinTuanDui ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; Max-Planck Partner Group ; MoST grant ; MoST grant ; CAS ; CAS ; National Science Foundation ; National Science Foundation
DOI10.1093/mnras/staa704
WOS KeywordFAST RADIO-BURSTS ; GAMMA-RAY BURSTS ; OBSERVATORY SUPERNOVA SEARCH ; EXTENDED EMISSION ; DISTRIBUTIONS ; POPULATION ; GALAXY ; LIMITS
Language英语
Funding ProjectNSFC[U15311243] ; NSFC[XDB23010200] ; NSFC[2017YFA0402600] ; NSFC[11633004] ; NSFC[NSFC 11473044] ; NSFC[11653003] ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; MoST grant[2016YFE0100300] ; CAS[QYZDJ-SSW-SLH017] ; CAS[CAS XDB 23040100] ; National Science Foundation[AST1516958] ; National Science Foundation[OIA-1458952]
Funding OrganizationNSFC ; NSFC ; TianShanChuangXinTuanDui ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; Max-Planck Partner Group ; MoST grant ; MoST grant ; CAS ; CAS ; National Science Foundation ; National Science Foundation ; NSFC ; NSFC ; TianShanChuangXinTuanDui ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; Max-Planck Partner Group ; MoST grant ; MoST grant ; CAS ; CAS ; National Science Foundation ; National Science Foundation ; NSFC ; NSFC ; TianShanChuangXinTuanDui ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; Max-Planck Partner Group ; MoST grant ; MoST grant ; CAS ; CAS ; National Science Foundation ; National Science Foundation ; NSFC ; NSFC ; TianShanChuangXinTuanDui ; TianShanChuangXinTuanDui ; Max-Planck Partner Group ; Max-Planck Partner Group ; MoST grant ; MoST grant ; CAS ; CAS ; National Science Foundation ; National Science Foundation
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000535885900050
PublisherOXFORD UNIV PRESS
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/54847
Collection中国科学院国家天文台
Corresponding AuthorLuo, Rui; Lee, Kejia
Affiliation1.Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China
2.Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China
3.Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Box 76, Epping, NSW 1710, Australia
4.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
5.Chinese Acad Sci, Natl Astron Observ, Key Lab Computat Astrophys, 20A Datun Rd, Beijing 100012, Peoples R China
6.Univ Chinese Acad Sci, Sch Astron & Space Sci, Beijing 100049, Peoples R China
7.West Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA
8.West Virginia Univ, Ctr Gravitat Waves & Cosmol, Chestnut Ridge Res Bldg, Morgantown, WV 26505 USA
9.Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA
Recommended Citation
GB/T 7714		 Luo, Rui,Men, Yunpeng,Lee, Kejia,et al. On the FRB luminosity function - -II. Event rate density[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2020,494(1):665-679.
APA Luo, Rui,Men, Yunpeng,Lee, Kejia,Wang, Weiyang,Lorimer, D. R.,&Zhang, Bing.(2020).On the FRB luminosity function - -II. Event rate density.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,494(1),665-679.
MLA Luo, Rui,et al."On the FRB luminosity function - -II. Event rate density".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 494.1(2020):665-679.
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