File Download
  Links for fulltext
     (May Require Subscription)
Supplementary

Article: The luminosity function of Swift long gamma-ray bursts

TitleThe luminosity function of Swift long gamma-ray bursts
Authors
KeywordsGamma-ray burst: general
Issue Date2011
PublisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR
Citation
Monthly Notices Of The Royal Astronomical Society, 2011, v. 416 n. 3, p. 2174-2181 How to Cite?
AbstractThe accumulation of Swift observed gamma-ray bursts (GRBs) has gradually made it possible to directly derive a GRB luminosity function (LF) from the observational luminosity distribution. However, two complexities are involved: (i) the evolving connection between GRB rate and cosmic star formation rate; and (ii) observational selection effects due to telescope thresholds and redshift measurements. With a phenomenological investigation of these two complexities, we constrain and discriminate two popular competing LF models (i.e. the broken-power-law LF and the single-power-law LF with an exponential cut-off at low luminosities). As a result, we find that the broken-power-law LF may be more favoured by observations, with a break luminosity L b= 2.5 × 10 52ergs -1 and prior- and post-break indices ν 1= 1.72 and ν 2= 1.98. Regarding an extra evolution effect expressed by a factor (1 +z) δ, if the metallicity of GRB progenitors is lower than ~0.1Z ⊙ as expected by some collapsar models, then there may be no extra evolution effect other than the metallicity evolution (i.e. δ approaches zero). Alternatively, if we remove the theoretical metallicity requirement, then a relationship between the degenerate parameters δ and Z max can be found, very roughly, δ~ 2.4(Z max/Z ⊙- 0.06). This indicates that extra evolution could become necessary for relatively high metallicities. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/145569
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID
Funding AgencyGrant Number
National Natural Science Foundation of China11047121
11103004
CCNU from the Colleges' Basic Research and Operation of MOE of ChinaCCNU09A01020
Scientific Innovation Foundation of CCNU
Government of the Hong KongHKU7011/09P
Funding Information:

We acknowledge the use of public data from the Swift data archive and thank D. Yonetoku for his invaluable comments and suggestions which have significantly improved our work. This work is supported by the National Natural Science Foundation of China (grant nos 11047121 and 11103004) and by the Self-Determined Research Funds of CCNU (grant no. CCNU09A01020) from the Colleges' Basic Research and Operation of MOE of China. X-FC is supported by the Scientific Innovation Foundation of CCNU. KSC is supported by the GRF Grants of the Government of the Hong Kong SAR under HKU7011/09P.

References

 

DC FieldValueLanguage
dc.contributor.authorCao, XFen_HK
dc.contributor.authorYu, YWen_HK
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorZheng, XPen_HK
dc.date.accessioned2012-02-28T01:55:37Z-
dc.date.available2012-02-28T01:55:37Z-
dc.date.issued2011en_HK
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society, 2011, v. 416 n. 3, p. 2174-2181en_HK
dc.identifier.issn0035-8711en_HK
dc.identifier.urihttp://hdl.handle.net/10722/145569-
dc.description.abstractThe accumulation of Swift observed gamma-ray bursts (GRBs) has gradually made it possible to directly derive a GRB luminosity function (LF) from the observational luminosity distribution. However, two complexities are involved: (i) the evolving connection between GRB rate and cosmic star formation rate; and (ii) observational selection effects due to telescope thresholds and redshift measurements. With a phenomenological investigation of these two complexities, we constrain and discriminate two popular competing LF models (i.e. the broken-power-law LF and the single-power-law LF with an exponential cut-off at low luminosities). As a result, we find that the broken-power-law LF may be more favoured by observations, with a break luminosity L b= 2.5 × 10 52ergs -1 and prior- and post-break indices ν 1= 1.72 and ν 2= 1.98. Regarding an extra evolution effect expressed by a factor (1 +z) δ, if the metallicity of GRB progenitors is lower than ~0.1Z ⊙ as expected by some collapsar models, then there may be no extra evolution effect other than the metallicity evolution (i.e. δ approaches zero). Alternatively, if we remove the theoretical metallicity requirement, then a relationship between the degenerate parameters δ and Z max can be found, very roughly, δ~ 2.4(Z max/Z ⊙- 0.06). This indicates that extra evolution could become necessary for relatively high metallicities. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.en_HK
dc.languageengen_US
dc.publisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNRen_HK
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_HK
dc.rightsThe definitive version is available at www.blackwell-synergy.com-
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.rights© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS-
dc.subjectGamma-ray burst: generalen_HK
dc.titleThe luminosity function of Swift long gamma-ray burstsen_HK
dc.typeArticleen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1111/j.1365-2966.2011.19194.xen_HK
dc.identifier.scopuseid_2-s2.0-84860393570en_HK
dc.identifier.hkuros198616en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-84860393570&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume416en_HK
dc.identifier.issue3en_HK
dc.identifier.spage2174en_HK
dc.identifier.epage2181en_HK
dc.identifier.isiWOS:000295378100043-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridCao, XF=23484109800en_HK
dc.identifier.scopusauthoridYu, YW=10939495100en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridZheng, XP=55201961600en_HK

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats