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Article: Discovery of GeV γ-ray emission from PSR B1259-63/LS 2883

TitleDiscovery of GeV γ-ray emission from PSR B1259-63/LS 2883
Authors
Keywordsgamma rays: stars
pulsars: individual (PSR B1259-63)
radiation mechanisms: non-thermal
X-rays: binaries
Issue Date2011
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2011, v. 736 n. 1 How to Cite?
AbstractThe binary system PSR B1259-63/LS 2883 consists of a 47.8 ms radio pulsar that orbits the companion Be star with a period of 3.4 years in a highly eccentric orbit. The system has been well sampled in radio, X-ray, and TeV γ-ray bands, and shows orbital phase-dependent variability in all observed frequencies. Here we report on the discovery of >100MeV γ-rays from PSR B1259-63/LS 2883 through the 2010 periastron passage. Using data collected with the Large Area Telescope on board Fermi from 33 days before periastron to 75 days after periastron, PSR B1259-63/LS 2883 was detected at a significance of 13.6 standard deviations. The γ-ray light curve was highly variable over this period, with a changing photon index that correlates with the γ-ray flux. In particular, two major flares that occur after the periastron passage were observed. The onset of γ-ray emission occurs close to, but not at the same orbital phases as, the two disk passages that occur ∼1 month before and ∼1 month after the periastron passage. The fact that the GeV orbital light curve is different from that of the X-ray and TeV light curves strongly suggests that GeV γ-ray emission originates from a different component. We speculate that the observed GeV flares may be resulting from Doppler boosting effects. © 2011. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/139640
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
Funding AgencyGrant Number
HK GovernmentHKU700908P
National Science Council of the Republic of China (Taiwan)NSC99-2112-M-007-004-MY3
NSC100-2923-M-007-001-MY3
Chungnam National University
Funding Information:

We acknowledge the use of data and software facilities from the FSSC, managed by the HEASARC at GSFC. J.T. and K.S.C. are supported by a GRF grant of HK Government under HKU700908P, and A.K.H.K. is supported partly by the National Science Council of the Republic of China (Taiwan) through grants NSC99-2112-M-007-004-MY3 and NSC100-2923-M-007-001-MY3. C.Y.H. is supported by research fund of Chungnam National University in 2010.

References

 

DC FieldValueLanguage
dc.contributor.authorTam, PHTen_HK
dc.contributor.authorHuang, RHHen_HK
dc.contributor.authorTakata, Jen_HK
dc.contributor.authorHui, CYen_HK
dc.contributor.authorKong, AKHen_HK
dc.contributor.authorCheng, KSen_HK
dc.date.accessioned2011-09-23T05:52:50Z-
dc.date.available2011-09-23T05:52:50Z-
dc.date.issued2011en_HK
dc.identifier.citationAstrophysical Journal Letters, 2011, v. 736 n. 1en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/139640-
dc.description.abstractThe binary system PSR B1259-63/LS 2883 consists of a 47.8 ms radio pulsar that orbits the companion Be star with a period of 3.4 years in a highly eccentric orbit. The system has been well sampled in radio, X-ray, and TeV γ-ray bands, and shows orbital phase-dependent variability in all observed frequencies. Here we report on the discovery of >100MeV γ-rays from PSR B1259-63/LS 2883 through the 2010 periastron passage. Using data collected with the Large Area Telescope on board Fermi from 33 days before periastron to 75 days after periastron, PSR B1259-63/LS 2883 was detected at a significance of 13.6 standard deviations. The γ-ray light curve was highly variable over this period, with a changing photon index that correlates with the γ-ray flux. In particular, two major flares that occur after the periastron passage were observed. The onset of γ-ray emission occurs close to, but not at the same orbital phases as, the two disk passages that occur ∼1 month before and ∼1 month after the periastron passage. The fact that the GeV orbital light curve is different from that of the X-ray and TeV light curves strongly suggests that GeV γ-ray emission originates from a different component. We speculate that the observed GeV flares may be resulting from Doppler boosting effects. © 2011. The American Astronomical Society. All rights reserved.en_HK
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsThe Astrophysical Journal Letters. Copyright © Institute of Physics Publishing Ltd.-
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectgamma rays: starsen_HK
dc.subjectpulsars: individual (PSR B1259-63)en_HK
dc.subjectradiation mechanisms: non-thermalen_HK
dc.subjectX-rays: binariesen_HK
dc.titleDiscovery of GeV γ-ray emission from PSR B1259-63/LS 2883en_HK
dc.typeArticleen_HK
dc.identifier.emailTakata, J: takata@hku.hken_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityTakata, J=rp00786en_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepostprint-
dc.identifier.doi10.1088/2041-8205/736/1/L10en_HK
dc.identifier.scopuseid_2-s2.0-79960909660en_HK
dc.identifier.hkuros195561en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-79960909660&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume736en_HK
dc.identifier.issue1en_HK
dc.identifier.isiWOS:000293138300010-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridTam, PHT=35243989500en_HK
dc.identifier.scopusauthoridHuang, RHH=36696348700en_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK
dc.identifier.scopusauthoridHui, CY=12781234500en_HK
dc.identifier.scopusauthoridKong, AKH=35185316600en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK

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