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Article: Observations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1

TitleObservations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1
Authors
Issue Date2004
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
Astrophysical Journal, 2004, v. 612 n. 1 I, p. 389-397 How to Cite?
AbstractWe present the results from X-ray and radio observations of the recently discovered young Vela-like pulsar PSR J2021+3651, which is coincident with the EGRET γ-ray source GeV 2020+3658. A 19.0 ks Chandra ACIS-S observation has revealed a ∼20″ × 10″ pulsar wind nebula that is reminiscent of the equatorial tori seen around some young pulsars, along with thermal emission from an embedded point source (kT ∞ = 0.15 ± 0.02 keV). We have named the nebula G75.2+0.1. Its spectrum is well fitted by an absorbed power-law model with a photon index of Γ = 1.7 -0.2 -0.3, a hydrogen column density of N H = (7.8 -1.4 +1.7) × 10 21 cm -2, and an unabsorbed 0.5-10.0 keV flux of (1.7 ± 0.1) × 10 -12 ergs cm -2 s -1. We have spatially fitted G75.2+0.1 with a model that assumes a toroidal morphology, and from this we infer that the axis of the torus is highly inclined to the line of sight. A 20.8 ks Chandra observation in continuous-clocking mode reveals a possible pulse detection, with a pulsed fraction of ∼65% and an H-test probability of occurring by chance of 8.9 × 10 -5. Timing observations with the Arecibo radio telescope spanning 2 yr show that PSR J2021+3651 glitched sometime between MJD 52,616 and 52,645 with parameters Δν/ν = (2.587 ± 0.002) × 10 -6 and Δν̇/ν̇ = (6.2 ± 0.3) × 10 -3, similar to those of the largest glitches observed in the Vela pulsar. PSR J2021+3651 is heavily scattered (τ scsc = 17.7 ± 0.9 ms at 1 GHz) and exhibits a significant amount of timing noise.
Persistent Identifierhttp://hdl.handle.net/10722/180508
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorHessels, JWTen_US
dc.contributor.authorRoberts, MSEen_US
dc.contributor.authorRansom, SMen_US
dc.contributor.authorKaspi, VMen_US
dc.contributor.authorRoman, RWen_US
dc.contributor.authorNg, CYen_US
dc.contributor.authorFreire, PCCen_US
dc.contributor.authorGaensler, BMen_US
dc.date.accessioned2013-01-28T01:38:56Z-
dc.date.available2013-01-28T01:38:56Z-
dc.date.issued2004en_US
dc.identifier.citationAstrophysical Journal, 2004, v. 612 n. 1 I, p. 389-397en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/180508-
dc.description.abstractWe present the results from X-ray and radio observations of the recently discovered young Vela-like pulsar PSR J2021+3651, which is coincident with the EGRET γ-ray source GeV 2020+3658. A 19.0 ks Chandra ACIS-S observation has revealed a ∼20″ × 10″ pulsar wind nebula that is reminiscent of the equatorial tori seen around some young pulsars, along with thermal emission from an embedded point source (kT ∞ = 0.15 ± 0.02 keV). We have named the nebula G75.2+0.1. Its spectrum is well fitted by an absorbed power-law model with a photon index of Γ = 1.7 -0.2 -0.3, a hydrogen column density of N H = (7.8 -1.4 +1.7) × 10 21 cm -2, and an unabsorbed 0.5-10.0 keV flux of (1.7 ± 0.1) × 10 -12 ergs cm -2 s -1. We have spatially fitted G75.2+0.1 with a model that assumes a toroidal morphology, and from this we infer that the axis of the torus is highly inclined to the line of sight. A 20.8 ks Chandra observation in continuous-clocking mode reveals a possible pulse detection, with a pulsed fraction of ∼65% and an H-test probability of occurring by chance of 8.9 × 10 -5. Timing observations with the Arecibo radio telescope spanning 2 yr show that PSR J2021+3651 glitched sometime between MJD 52,616 and 52,645 with parameters Δν/ν = (2.587 ± 0.002) × 10 -6 and Δν̇/ν̇ = (6.2 ± 0.3) × 10 -3, similar to those of the largest glitches observed in the Vela pulsar. PSR J2021+3651 is heavily scattered (τ scsc = 17.7 ± 0.9 ms at 1 GHz) and exhibits a significant amount of timing noise.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637Xen_US
dc.relation.ispartofAstrophysical Journalen_US
dc.titleObservations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1en_US
dc.typeArticleen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hken_US
dc.identifier.authorityNg, CY=rp01706en_US
dc.description.naturelink_to_OA_fulltexten_US
dc.identifier.doi10.1086/422408en_US
dc.identifier.scopuseid_2-s2.0-8744281321en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-8744281321&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume612en_US
dc.identifier.issue1 Ien_US
dc.identifier.spage389en_US
dc.identifier.epage397en_US
dc.identifier.isiWOS:000223634400031-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridHessels, JWT=6701717720en_US
dc.identifier.scopusauthoridRoberts, MSE=7404028764en_US
dc.identifier.scopusauthoridRansom, SM=7005562794en_US
dc.identifier.scopusauthoridKaspi, VM=7006755510en_US
dc.identifier.scopusauthoridRoman, RW=46561391900en_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US
dc.identifier.scopusauthoridFreire, PCC=7005742539en_US
dc.identifier.scopusauthoridGaensler, BM=34769921200en_US
dc.customcontrol.immutablejt 130807-

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