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Article: Radio and γ-ray constraints on the emission geometry and birthplace of PSR j2043+2740

TitleRadio and γ-ray constraints on the emission geometry and birthplace of PSR j2043+2740
Authors
Noutsos, AAbdo, AAAckermann, MAjello, MBallet, JBarbiellini, GBaring, MGBastieri, DBechtol, KBellazzini, RBerenji, BGiordano, FGiroletti, MGodfrey, GGrandi, PGrenier, IAGrove, JEGuillemot, LGuiriec, SHarding, AKHughes, REPanetta, JHJackson, MSJóhannesson, GJohnson, ASJohnson, TJJohnson, WNJohnston, SKamae, TKatagiri, HKataoka, JKnödlseder, JParent, DKramer, MKuss, MLande, JLee, SHLongo, FLoparco, FLovellette, MNLubrano, PLyne, AGMakeev, APelassa, VMarelli, MMazziotta, MNMcenery, JEMehault, JMichelson, PFMizuno, TMonte, CMonzani, MEMorselli, AMoskalenko, IVPepe, MMurgia, SNaumannGodo, MNolan, PLNuss, EOhsugi, TOkumura, AOmodei, NOrlando, EOrmes, JFPersic, MPesceRollins, MPiron, FPorter, TARainò, SRay, PSBonamente, ERazzano, MReimer, AReimer, OReposeur, TRomani, RWSadrozinski, HFWSander, ASaz Parkinson, PMSgrò, CSiskind, EJBorgland, AWSmith, DASmith, PDSpandre, GSpinelli, PStappers, BWStrickman, MSSuson, DJTakahashi, HTanaka, TTheureau, GBregeon, JThompson, DJThorsett, SETibolla, OTorres, DFTramacere, AUsher, TLVandenbroucke, JVianello, GVilchez, NVillata, MBrez, AVitale, VVon Kienlin, AWaite, APWang, PWatters, KWeltevrede, PWiner, BLWood, KSZiegler, MBrigida, MBruel, PBuehler, RBusetto, GCaliandro, GACameron, RACamilo, FCaraveo, PACasandjian, JMCecchi, CÇelik, ÖChaty, SChekhtman, AChiang, JCiprini, SClaus, RCognard, ICohenTanugi, JColafrancesco, SCutini, SDermer, CDDe Palma, FDrell, PSDumora, DEa, CMFavuzzi, CFerrara, ECFocke, WBFrailis, MFreire, PCCFukazawa, YFunk, SFusco, PGargano, FGermani, SGiglietto, N
KeywordsGamma Rays: Stars
Pulsars: Individual (Psr J2043 + 2740)
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. 728 n. 2 How to Cite?
AbstractWe report on the first year of Fermi γ-ray observations of pulsed high-energy emission from the old PSR J2043 + 2740. The study of the γ-ray efficiency of such old pulsars gives us an insight into the evolution of pulsars' ability to emit in γ rays as they age. The y-ray light curve of this pulsar above 0.1 GeV is clearly defined by two sharp peaks, 0.353 ± 0.035 periods apart. We have combined the γ-ray profile characteristics of PSR J2043 + 2740 with the geometrical properties of the pulsar's radio emission, derived from radio-polarization data, and constrained the pulsar-beam geometry in the framework of a two-pole caustic (TPC) and an outer gap (OG) model. The ranges of magnetic inclination and viewing angle were determined to be {α, ζ} ∼ {52°-57°, 61°-68°} for the TPC model, and {α, ζ} ∼ {62°-73°, 74°-81°} and {α, ζ,} ∼ {72°-83°, 60°-75°} for the OG model. Based on this geometry, we assess possible birth locations for this pulsar and derive a likely proper motion, sufficiently high to be measurable with VLBI. At a characteristic age of 1.2 Myr, PSR J2043 + 2740 is the third oldest of all discovered, non-recycled, γ-ray pulsars: it is twice as old as the next oldest, PSR J0357 + 32, and younger only than the recently discovered PSR J1836 + 5925 and PSR J2055 + 25, both of which are at least five and ten times less energetic, respectively. © 2011. The American Astronomical Society.
Persistent Identifierhttp://hdl.handle.net/10722/188410
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorNoutsos, Aen_US
dc.contributor.authorAbdo, AAen_US
dc.contributor.authorAckermann, Men_US
dc.contributor.authorAjello, Men_US
dc.contributor.authorBallet, Jen_US
dc.contributor.authorBarbiellini, Gen_US
dc.contributor.authorBaring, MGen_US
dc.contributor.authorBastieri, Den_US
dc.contributor.authorBechtol, Ken_US
dc.contributor.authorBellazzini, Ren_US
dc.contributor.authorBerenji, Ben_US
dc.contributor.authorGiordano, Fen_US
dc.contributor.authorGiroletti, Men_US
dc.contributor.authorGodfrey, Gen_US
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dc.contributor.authorGrove, JEen_US
dc.contributor.authorGuillemot, Len_US
dc.contributor.authorGuiriec, Sen_US
dc.contributor.authorHarding, AKen_US
dc.contributor.authorHughes, REen_US
dc.contributor.authorPanetta, JHen_US
dc.contributor.authorJackson, MSen_US
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dc.contributor.authorJohnson, ASen_US
dc.contributor.authorJohnson, TJen_US
dc.contributor.authorJohnson, WNen_US
dc.contributor.authorJohnston, Sen_US
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dc.contributor.authorKataoka, Jen_US
dc.contributor.authorKnödlseder, Jen_US
dc.contributor.authorParent, Den_US
dc.contributor.authorKramer, Men_US
dc.contributor.authorKuss, Men_US
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dc.contributor.authorMurgia, Sen_US
dc.contributor.authorNaumannGodo, Men_US
dc.contributor.authorNolan, PLen_US
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dc.contributor.authorOkumura, Aen_US
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dc.contributor.authorRainò, Sen_US
dc.contributor.authorRay, PSen_US
dc.contributor.authorBonamente, Een_US
dc.contributor.authorRazzano, Men_US
dc.contributor.authorReimer, Aen_US
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dc.contributor.authorRomani, RWen_US
dc.contributor.authorSadrozinski, HFWen_US
dc.contributor.authorSander, Aen_US
dc.contributor.authorSaz Parkinson, PMen_US
dc.contributor.authorSgrò, Cen_US
dc.contributor.authorSiskind, EJen_US
dc.contributor.authorBorgland, AWen_US
dc.contributor.authorSmith, DAen_US
dc.contributor.authorSmith, PDen_US
dc.contributor.authorSpandre, Gen_US
dc.contributor.authorSpinelli, Pen_US
dc.contributor.authorStappers, BWen_US
dc.contributor.authorStrickman, MSen_US
dc.contributor.authorSuson, DJen_US
dc.contributor.authorTakahashi, Hen_US
dc.contributor.authorTanaka, Ten_US
dc.contributor.authorTheureau, Gen_US
dc.contributor.authorBregeon, Jen_US
dc.contributor.authorThompson, DJen_US
dc.contributor.authorThorsett, SEen_US
dc.contributor.authorTibolla, Oen_US
dc.contributor.authorTorres, DFen_US
dc.contributor.authorTramacere, Aen_US
dc.contributor.authorUsher, TLen_US
dc.contributor.authorVandenbroucke, Jen_US
dc.contributor.authorVianello, Gen_US
dc.contributor.authorVilchez, Nen_US
dc.contributor.authorVillata, Men_US
dc.contributor.authorBrez, Aen_US
dc.contributor.authorVitale, Ven_US
dc.contributor.authorVon Kienlin, Aen_US
dc.contributor.authorWaite, APen_US
dc.contributor.authorWang, Pen_US
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dc.contributor.authorWeltevrede, Pen_US
dc.contributor.authorWiner, BLen_US
dc.contributor.authorWood, KSen_US
dc.contributor.authorZiegler, Men_US
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dc.contributor.authorBruel, Pen_US
dc.contributor.authorBuehler, Ren_US
dc.contributor.authorBusetto, Gen_US
dc.contributor.authorCaliandro, GAen_US
dc.contributor.authorCameron, RAen_US
dc.contributor.authorCamilo, Fen_US
dc.contributor.authorCaraveo, PAen_US
dc.contributor.authorCasandjian, JMen_US
dc.contributor.authorCecchi, Cen_US
dc.contributor.authorÇelik, Öen_US
dc.contributor.authorChaty, Sen_US
dc.contributor.authorChekhtman, Aen_US
dc.contributor.authorChiang, Jen_US
dc.contributor.authorCiprini, Sen_US
dc.contributor.authorClaus, Ren_US
dc.contributor.authorCognard, Ien_US
dc.contributor.authorCohenTanugi, Jen_US
dc.contributor.authorColafrancesco, Sen_US
dc.contributor.authorCutini, Sen_US
dc.contributor.authorDermer, CDen_US
dc.contributor.authorDe Palma, Fen_US
dc.contributor.authorDrell, PSen_US
dc.contributor.authorDumora, Den_US
dc.contributor.authorEa, CMen_US
dc.contributor.authorFavuzzi, Cen_US
dc.contributor.authorFerrara, ECen_US
dc.contributor.authorFocke, WBen_US
dc.contributor.authorFrailis, Men_US
dc.contributor.authorFreire, PCCen_US
dc.contributor.authorFukazawa, Yen_US
dc.contributor.authorFunk, Sen_US
dc.contributor.authorFusco, Pen_US
dc.contributor.authorGargano, Fen_US
dc.contributor.authorGermani, Sen_US
dc.contributor.authorGiglietto, Nen_US
dc.date.accessioned2013-09-03T04:05:36Z-
dc.date.available2013-09-03T04:05:36Z-
dc.date.issued2011en_US
dc.identifier.citationAstrophysical Journal Letters, 2011, v. 728 n. 2en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/188410-
dc.description.abstractWe report on the first year of Fermi γ-ray observations of pulsed high-energy emission from the old PSR J2043 + 2740. The study of the γ-ray efficiency of such old pulsars gives us an insight into the evolution of pulsars' ability to emit in γ rays as they age. The y-ray light curve of this pulsar above 0.1 GeV is clearly defined by two sharp peaks, 0.353 ± 0.035 periods apart. We have combined the γ-ray profile characteristics of PSR J2043 + 2740 with the geometrical properties of the pulsar's radio emission, derived from radio-polarization data, and constrained the pulsar-beam geometry in the framework of a two-pole caustic (TPC) and an outer gap (OG) model. The ranges of magnetic inclination and viewing angle were determined to be {α, ζ} ∼ {52°-57°, 61°-68°} for the TPC model, and {α, ζ} ∼ {62°-73°, 74°-81°} and {α, ζ,} ∼ {72°-83°, 60°-75°} for the OG model. Based on this geometry, we assess possible birth locations for this pulsar and derive a likely proper motion, sufficiently high to be measurable with VLBI. At a characteristic age of 1.2 Myr, PSR J2043 + 2740 is the third oldest of all discovered, non-recycled, γ-ray pulsars: it is twice as old as the next oldest, PSR J0357 + 32, and younger only than the recently discovered PSR J1836 + 5925 and PSR J2055 + 25, both of which are at least five and ten times less energetic, respectively. © 2011. The American Astronomical Society.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectGamma Rays: Starsen_US
dc.subjectPulsars: Individual (Psr J2043 + 2740)en_US
dc.titleRadio and γ-ray constraints on the emission geometry and birthplace of PSR j2043+2740en_US
dc.typeArticleen_US
dc.identifier.emailSaz Parkinson, PM: pablosp@hku.hken_US
dc.identifier.authoritySaz Parkinson, PM=rp01803en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1088/0004-637X/728/2/77en_US
dc.identifier.scopuseid_2-s2.0-84891222024en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-79960216459&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume728en_US
dc.identifier.issue2en_US
dc.identifier.isiWOS:000286973600004-
dc.publisher.placeUnited Kingdomen_US
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