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Fermi-LAT constraints on the Pulsar Wind Nebula nature of HESS J1857+026

hal.structure.identifierGLAST
dc.contributor.authorROUSSEAU, R.
dc.contributor.authorGRONDIN, M.-H.
dc.contributor.authorVAN ETTEN, A.
hal.structure.identifierGLAST
dc.contributor.authorLEMOINE-GOUMARD, M.
dc.contributor.authorBOGDANOV, S.
dc.contributor.authorW. T. HESSELS, J.
dc.contributor.authorM. KASPI, V.
dc.contributor.authorARZOUMANIAN, Z.
dc.contributor.authorCAMILO, F.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorM. CASANDJIAN, J.
dc.contributor.authorM. ESPINOZA, C.
dc.contributor.authorJOHNSTON, S.
dc.contributor.authorG. LYNE, A.
hal.structure.identifierGLAST
dc.contributor.authorSMITH, David Stanley
dc.contributor.authorW. STAPPERS, B.
dc.contributor.authorA. CALIANDRO, G.
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnSince its launch, the Fermi satellite has firmly identified 5 pulsar wind nebulae plus a large number of candidates, all powered by young and energetic pulsars. HESS J1857+026 is a spatially extended gamma-ray source detected by H.E.S.S. and classified as a possible pulsar wind nebula candidate powered by PSR J1856+0245. We search for gamma-ray pulsations from PSR J1856+0245 and explore the characteristics of its associated pulsar wind nebula. Using a rotational ephemeris obtained from the Lovell telescope at Jodrell Bank Observatory at 1.5 GHz, we phase-fold 36 months of gamma-ray data acquired by the Large Area Telescope (LAT) aboard Fermi. We also perform a complete gamma-ray spectral and morphological analysis. No gamma-ray pulsations were detected from PSR J1856+0245. However, significant emission is detected at a position coincident with the TeV source HESS J1857+026. The gamma-ray spectrum is well described by a simple power-law with a spectral index of 1.53 \pm 0.11_{\rm stat} \pm 0.55_{\rm syst}$ and an energy flux of $G(0.1$--100 GeV$)=(2.71 \pm 0.52_{\rm stat} \pm 1.51_{\rm syst}) \times 10^{-11}$ ergs cm$^{-2}$ s$^{-1}$. The $\gamma$-ray luminosity is $L_{PWN}^{\gamma} (0.1$--100 GeV$)=(2.5 \pm 0.5_{stat} \pm 1.5_{syst}) \times 10^{35} (\frac{d}{9 kpc})^2$ ergs s$^{-1}$, assuming a distance of 9 kpc. This implies a $\gamma-$ray efficiency of $\sim$ 5% for $\dot{E}=4.6 \times 10^{36}$ erg $s^{-1}$, in the range expected for pulsar wind nebulae. Detailed multi-wavelength modeling provides new constraints on its pulsar wind nebula nature.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enFermi-LAT constraints on the Pulsar Wind Nebula nature of HESS J1857+026
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201118685
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.arxiv1206.3324
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA3
bordeaux.volume544
bordeaux.peerReviewedoui
hal.identifierin2p3-00738825
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//in2p3-00738825v1
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