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Article: Proper motion, spectra, and timing of PSR J1813–1749 using Chandra and NICER

TitleProper motion, spectra, and timing of PSR J1813–1749 using Chandra and NICER
Authors
Keywordspulsars: general
pulsars: individual: CXOU J181335.16–174957.4
PSR J1813–1749
ISM: individual: G12.82–0.02
HESS J1813–178
Issue Date2020
PublisherRoyal Astronomical Society. The Journal's web site is located at http://www.oxfordjournals.org/our_journals/mnras/
Citation
Monthly Notices of the Royal Astronomical Society, 2020, v. 498 n. 3, p. 4396-4403 How to Cite?
AbstractPSR J1813–1749 is one of the most energetic rotation-powered pulsars known, producing a pulsar wind nebula (PWN) and gamma-ray and TeV emission, but whose spin period is only measurable in X-ray. We present analysis of two Chandra data sets that are separated by more than 10 yr and recent NICER data. The long baseline of the Chandra data allows us to derive a pulsar proper motion μRA=(−0.067±0.010)arcsecyr−1 and μDec.=(−0.014±0.007)arcsecyr−1 and velocity v⊥≈900−1600kms−1 (assuming a distance d = 3–5 kpc), although we cannot exclude a contribution to the change in measured pulsar position due to a change in brightness structure of the PWN very near the pulsar. We model the PWN and pulsar spectra using an absorbed power law and obtain best-fitting absorption NH=(13.1±0.9)×1022cm−2⁠, photon index Γ = 1.5 ± 0.1, and 0.3–10 keV luminosity LX≈5.4×1034ergs−1(d/ 5 kpc)2 for the PWN and Γ = 1.2 ± 0.1 and LX≈9.3×1033ergs−1(d/ 5 kpc)2 for PSR J1813–1749. These values do not change between the 2006 and 2016 observations. We use NICER observations from 2019 to obtain a timing model of PSR J1813–1749, with spin frequency ν = 22.35 Hz and spin frequency time derivative ν˙=(−6.428±0.003)×10−11Hzs−1⁠. We also fit ν measurements from 2009 to 2012 and our 2019 value and find a long-term spin-down rate ν˙=(−6.3445±0.0004)×10−11Hzs−1⁠. We speculate that the difference in spin-down rates is due to glitch activity or emission mode switching.
Persistent Identifierhttp://hdl.handle.net/10722/294658
ISSN
2023 Impact Factor: 4.7
2023 SCImago Journal Rankings: 1.621
PubMed Central ID
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorHo, WCG-
dc.contributor.authorGuillot, S-
dc.contributor.authorSaz Parkinson, PM-
dc.contributor.authorLimyansky, B-
dc.contributor.authorNg, CY-
dc.contributor.authorBejger, M-
dc.contributor.authorEspinoza, CM-
dc.contributor.authorHaskell, B-
dc.contributor.authorJaisawal, GK-
dc.contributor.authorMalacaria, C-
dc.date.accessioned2020-12-08T07:40:04Z-
dc.date.available2020-12-08T07:40:04Z-
dc.date.issued2020-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2020, v. 498 n. 3, p. 4396-4403-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/294658-
dc.description.abstractPSR J1813–1749 is one of the most energetic rotation-powered pulsars known, producing a pulsar wind nebula (PWN) and gamma-ray and TeV emission, but whose spin period is only measurable in X-ray. We present analysis of two Chandra data sets that are separated by more than 10 yr and recent NICER data. The long baseline of the Chandra data allows us to derive a pulsar proper motion μRA=(−0.067±0.010)arcsecyr−1 and μDec.=(−0.014±0.007)arcsecyr−1 and velocity v⊥≈900−1600kms−1 (assuming a distance d = 3–5 kpc), although we cannot exclude a contribution to the change in measured pulsar position due to a change in brightness structure of the PWN very near the pulsar. We model the PWN and pulsar spectra using an absorbed power law and obtain best-fitting absorption NH=(13.1±0.9)×1022cm−2⁠, photon index Γ = 1.5 ± 0.1, and 0.3–10 keV luminosity LX≈5.4×1034ergs−1(d/ 5 kpc)2 for the PWN and Γ = 1.2 ± 0.1 and LX≈9.3×1033ergs−1(d/ 5 kpc)2 for PSR J1813–1749. These values do not change between the 2006 and 2016 observations. We use NICER observations from 2019 to obtain a timing model of PSR J1813–1749, with spin frequency ν = 22.35 Hz and spin frequency time derivative ν˙=(−6.428±0.003)×10−11Hzs−1⁠. We also fit ν measurements from 2009 to 2012 and our 2019 value and find a long-term spin-down rate ν˙=(−6.3445±0.0004)×10−11Hzs−1⁠. We speculate that the difference in spin-down rates is due to glitch activity or emission mode switching.-
dc.languageeng-
dc.publisherRoyal Astronomical Society. The Journal's web site is located at http://www.oxfordjournals.org/our_journals/mnras/-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectpulsars: general-
dc.subjectpulsars: individual: CXOU J181335.16–174957.4-
dc.subjectPSR J1813–1749-
dc.subjectISM: individual: G12.82–0.02-
dc.subjectHESS J1813–178-
dc.titleProper motion, spectra, and timing of PSR J1813–1749 using Chandra and NICER-
dc.typeArticle-
dc.identifier.emailSaz Parkinson, PM: pablosp@hku.hk-
dc.identifier.emailNg, CY: ncy@astro.physics.hku.hk-
dc.identifier.authoritySaz Parkinson, PM=rp01803-
dc.identifier.authorityNg, CY=rp01706-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1093/mnras/staa2653-
dc.identifier.pmid33204043-
dc.identifier.pmcidPMC7668304-
dc.identifier.scopuseid_2-s2.0-85096922440-
dc.identifier.hkuros320429-
dc.identifier.volume498-
dc.identifier.issue3-
dc.identifier.spage4396-
dc.identifier.epage4403-
dc.identifier.isiWOS:000587752500101-
dc.publisher.placeUnited Kingdom-

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