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PSRs J0248+6021 and J2240+5832: Young Pulsars in the Northern Galactic Plane. Discovery, Timing, and Gamma-ray observations

hal.structure.identifierLaboratoire de physique et chimie de l'environnement [LPCE]
hal.structure.identifierUnité Scientifique de la Station de Nançay [USN]
dc.contributor.authorTHEUREAU, Gilles
hal.structure.identifierGeorge Mason University [Fairfax]
hal.structure.identifierCentre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG]
hal.structure.identifierSpace Science Division [Washington]
dc.contributor.authorPARENT, D.
hal.structure.identifierLaboratoire de physique et chimie de l'environnement [LPCE]
hal.structure.identifierUnité Scientifique de la Station de Nançay [USN]
dc.contributor.authorCOGNARD, Ismaël
hal.structure.identifierLaboratoire de physique et chimie de l'environnement [LPCE]
hal.structure.identifierUnité Scientifique de la Station de Nançay [USN]
hal.structure.identifierBerkeley Radio Astronomy Laboratory [RAL]
dc.contributor.authorDESVIGNES, G.
hal.structure.identifierCentre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG]
dc.contributor.authorSMITH, D. A.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorCASANDJIAN, J. M.
hal.structure.identifierNational Research Council Associate
hal.structure.identifierSpace Science Division [Washington]
dc.contributor.authorCHEUNG, C. C.
hal.structure.identifierHansen Experimental Physics Lab [Stanford] [HEPL]
dc.contributor.authorCRAIG, H. A.
hal.structure.identifierCenter for Research and Exploration in Space Science and Technology [GSFC] [CRESST]
hal.structure.identifierDepartment of Physics and Department of Astronomy
dc.contributor.authorDONATO, D.
hal.structure.identifierHigh Performance Technologies
dc.contributor.authorFOSTER, R.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
hal.structure.identifierCentre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG]
dc.contributor.authorGUILLEMOT, L.
hal.structure.identifierNASA Goddard Space Flight Center [GSFC]
dc.contributor.authorHARDING, A. K.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorLESTRADE, J. -F.
hal.structure.identifierSpace Science Division [Washington]
dc.contributor.authorRAY, P. S.
hal.structure.identifierHansen Experimental Physics Lab [Stanford] [HEPL]
dc.contributor.authorROMANI, R. W.
hal.structure.identifierNASA Goddard Space Flight Center [GSFC]
dc.contributor.authorTHOMPSON, D. J.
hal.structure.identifierNational Astronomical Observatories of China
hal.structure.identifierDepartment of Physics and Astronomy [Hamilton NY]
dc.contributor.authorTIAN, W. W.
hal.structure.identifierHansen Experimental Physics Lab [Stanford] [HEPL]
dc.contributor.authorWATTERS, K.
dc.date.issued2011-01
dc.identifier.issn0004-6361
dc.description.abstractEnPulsars PSR J0248+6021 (rotation period P=217 ms and spin-down power Edot = 2.13E35 erg/s) and PSR J2240+5832 (P=140 ms, Edot = 2.12E35 erg/s) were discovered in 1997 with the Nancay radio telescope during a northern Galactic plane survey, using the Navy-Berkeley Pulsar Processor (NBPP) filter bank. GeV gamma-ray pulsations from both were discovered using the Fermi Large Area Telescope. Twelve years of radio and polarization data allow detailed investigations. The two pulsars resemble each other both in radio and in gamma-ray data. Both are rare in having a single gamma-ray pulse offset far from the radio peak. The high dispersion measure for PSR J0248+6021 (DM = 370 pc cm^-3) is most likely due to its being within the dense, giant HII region W5 in the Perseus arm at a distance of 2 kpc, not beyond the edge of the Galaxy as obtained from models of average electron distributions. Its high transverse velocity and the low magnetic field along the line-of-sight favor this small distance. Neither gamma-ray, X-ray, nor optical data yield evidence for a pulsar wind nebula surrounding PSR J0248+6021. The gamma-ray luminosity for PSR J0248+6021 is L_ gamma = (1.4 \pm 0.3)\times 10^34 erg/s. For PSR J2240+5832, we find either L_gamma = (7.9 \pm 5.2) \times 10^34 erg/s if the pulsar is in the Outer arm, or L_gamma = (2.2 \pm 1.7) \times 10^34 erg/s for the Perseus arm. These luminosities are consistent with an L_gamma ~ sqrt(Edot) rule. Comparison of the gamma-ray pulse profiles with model predictions, including the constraints obtained from radio polarization data, favor emission in the far magnetosphere. These two pulsars differ mainly in their inclination angles and acceleration gap widths, which in turn explains the observed differences in the gamma-ray peak widths.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enPSRs J0248+6021 and J2240+5832: Young Pulsars in the Northern Galactic Plane. Discovery, Timing, and Gamma-ray observations
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201015317
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Phénomènes cosmiques de haute energie [astro-ph.HE]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Phénomènes cosmiques de haute energie [astro-ph.HE]
dc.identifier.arxiv1010.4230
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA94
bordeaux.volume525
bordeaux.peerReviewedoui
hal.identifierin2p3-00586111
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//in2p3-00586111v1
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