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Article: Detection of an X-ray pulsation for the Gamma-ray pulsar centered in CTA 1

TitleDetection of an X-ray pulsation for the Gamma-ray pulsar centered in CTA 1
Authors
KeywordsGamma rays: general
Pulsars: individual (PSR J0007+7303, Geminga)
Radiation mechanisms: non-thermal
Radiation mechanisms: thermal
X-rays: general
Issue Date2010
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2010, v. 725 n. 1 PART 2, p. L1-L5 How to Cite?
AbstractWe report the detection of X-ray pulsations with a period of ∼315.87 ms from the 2009 XMM-Newton observation for the radio-quiet γ -ray pulsar, LAT PSR J0007+7303, centered in the supernova remnant CTA 1. The detected pulsed period is consistent with the γ -ray periodicity at the same epoch found with the Fermi Gamma-ray Space Telescope. The broader sinusoidal structure in the folded light curve of the X-ray emission is dissimilar to that of the γ -ray emission, and the phase of the peak is about 0.5 shifting from the peak in the γ -ray bands, indicating that the main component of the X-rays originates from different sites of the pulsar. We conclude that the main component of the X-ray pulsation is contributed by the thermal emission from the neutron star. Although with a significantly different characteristic age, PSR J0007+7303 is similar to Geminga in emission properties of X-rays and γ -rays; this makes PSR J0007+7303 the second radio-quiet γ -ray pulsar with detected X-ray pulsations after Geminga. © 2010 The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/135359
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
Funding AgencyGrant Number
National Science CouncilNSC 99-2811-M-008-057
NSC 099-2811-M-007-062
NSC 99-2112-M-008-014-MY3
NSC 99-2119-M-008-017
NSC 96-2112-M-007-037-MY3
NSC 99-2112-M-007-004-MY3
Chungnam National University
Funding Information:

The authors appreciate the anonymous referee for his/her fruitful comments. We also thank Dr Jau-Shian Liang for discussion on the application of the pulsed spectrum for our target. This work was partially supported by the National Science Council through grant NSC 99-2811-M-008-057, and R.H.H.H. is supported through grant NSC 099-2811-M-007-062. C. Y. Hwang acknowledges support from the National Science Council through grants NSC 99-2112-M-008-014-MY3 and NSC 99-2119-M-008-017. C. Y. Hui is supported by the research fund of Chungnam National University in 2010. A.K.H.K. acknowledges support from the National Science Council through grants NSC 96-2112-M-007-037-MY3 and NSC 99-2112-M-007-004-MY3.

References

 

DC FieldValueLanguage
dc.contributor.authorLin, LCCen_HK
dc.contributor.authorHuang, RHHen_HK
dc.contributor.authorTakata, Jen_HK
dc.contributor.authorHwang, CYen_HK
dc.contributor.authorKong, AKHen_HK
dc.contributor.authorHui, CYen_HK
dc.date.accessioned2011-07-27T01:34:09Z-
dc.date.available2011-07-27T01:34:09Z-
dc.date.issued2010en_HK
dc.identifier.citationAstrophysical Journal Letters, 2010, v. 725 n. 1 PART 2, p. L1-L5en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/135359-
dc.description.abstractWe report the detection of X-ray pulsations with a period of ∼315.87 ms from the 2009 XMM-Newton observation for the radio-quiet γ -ray pulsar, LAT PSR J0007+7303, centered in the supernova remnant CTA 1. The detected pulsed period is consistent with the γ -ray periodicity at the same epoch found with the Fermi Gamma-ray Space Telescope. The broader sinusoidal structure in the folded light curve of the X-ray emission is dissimilar to that of the γ -ray emission, and the phase of the peak is about 0.5 shifting from the peak in the γ -ray bands, indicating that the main component of the X-rays originates from different sites of the pulsar. We conclude that the main component of the X-ray pulsation is contributed by the thermal emission from the neutron star. Although with a significantly different characteristic age, PSR J0007+7303 is similar to Geminga in emission properties of X-rays and γ -rays; this makes PSR J0007+7303 the second radio-quiet γ -ray pulsar with detected X-ray pulsations after Geminga. © 2010 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.subjectGamma rays: generalen_HK
dc.subjectPulsars: individual (PSR J0007+7303, Geminga)en_HK
dc.subjectRadiation mechanisms: non-thermalen_HK
dc.subjectRadiation mechanisms: thermalen_HK
dc.subjectX-rays: generalen_HK
dc.titleDetection of an X-ray pulsation for the Gamma-ray pulsar centered in CTA 1en_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=2041-8205&volume=725&issue=1, article no. L1&spage=&epage=&date=2010&atitle=Detection+of+an+X-ray+pulsation+for+the+Gamma-ray+pulsar+centered+in+CTA+1-
dc.identifier.emailTakata, J: takata@hku.hken_HK
dc.identifier.authorityTakata, J=rp00786en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/2041-8205/725/1/L1en_HK
dc.identifier.scopuseid_2-s2.0-78650252135en_HK
dc.identifier.hkuros186453en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-78650252135&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume725en_HK
dc.identifier.issue1 PART 2en_HK
dc.identifier.spageL1en_HK
dc.identifier.epageL5en_HK
dc.identifier.isiWOS:000284575400001-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridLin, LCC=24366370500en_HK
dc.identifier.scopusauthoridHuang, RHH=36696348700en_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK
dc.identifier.scopusauthoridHwang, CY=7403387605en_HK
dc.identifier.scopusauthoridKong, AKH=35185316600en_HK
dc.identifier.scopusauthoridHui, CY=12781234500en_HK

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