2005A&A...442L..25A

Query : 2005A&A...442L..25A

2005A&A...442L..25A - Astronomy and Astrophysics, volume 442, L25-29 (2005/11-2)

A possible association of the new VHE γ-ray source HESSJ1825-137 with the pulsar wind nebula G18.0-0.7.

AHARONIAN F.A., AKHPERJANIAN A.G., BAZER-BACHI A.R., BEILICKE M., BENBOW W., BERGE D., BERNLOEHR K., BOISSON C., BOLZ O., BORREL V., BRAUN I., BREITLING F., BROWN A.M., CHADWICK P.M., CHOUNET L.-M., CORNILS R., COSTAMANTE L., DEGRANGE B., DICKINSON H.J., DJANNATI-ATAIE A., DRURY L.O'C., DUBUS G., EMMANOULOPOULOS D., ESPIGAT P., FEINSTEIN F., FONTAINE G., FUCHS Y., FUNK S., GALLANT Y.A., GIEBELS B., GILLESSEN S., GLICENSTEIN J.F., GORET P., HADJICHRISTIDIS C., HAUSER M., HEINZELMANN G., HENRI G., HERMANN G., HINTON J.A., HOFMANN W., HOLLERAN M., HORNS D., JACHOLKOWSKA A., DE JAGER O.C., KHELIFI B., KOMIN N., KONOPELKO A., LATHAM I.J., LE GALLOU R., LEMIERE A., LEMOINE-GOUMARD M., LEROY N., LOHSE T., MARTIN J.M., MARTINEAU-HUYNH O., MARCOWITH A., MASTERSON C., McCOMB T.J.L., DE NAUROIS M., NOLAN S.J., NOUTSOS A., ORFORD K.J., OSBORNE J.L., OUCHRIF M., PANTER M., PELLETIER G., PITA S., PUEHLHOFER G., PUNCH M., RAUBENHEIMER B.C., RAUE M., RAUX J., RAYNER S.M., REIMER A., REIMER O., RIPKEN J., ROB L., ROLLAND L., ROWELL G., SAHAKIAN V., SAUGE L., SCHLENKER S., SCHLICKEISER R., SCHUSTER C., SCHWANKE U., SIEWERT M., SOL H., SPANGLER D., STEENKAMP R., STEGMANN C., TAVERNET J.-P., TERRIER R., THEORET C.G., TLUCZYKONT M., VASILEIADIS G., VENTER C., VINCENT P., VOELK H.J. and WAGNER S.J.

Abstract (from CDS):

We report on a possible association of the recently discovered very high-energy γ-ray source HESSJ1825-137 with the pulsar wind nebula (commonly referred to as G18.0-0.7) of the 2.1x10⁴ year old Vela-like pulsar PSRB1823-13. HESSJ1825-137 was detected with a significance of 8.1σ in the Galactic Plane survey conducted with the HESS instrument in 2004. The centroid position of HESSJ1825-137 is offset by 11' south of the pulsar position. XMM-Newton observations have revealed X-ray synchrotron emission of an asymmetric pulsar wind nebula extending to the south of the pulsar. We argue that the observed morphology and TeV spectral index suggest that HESSJ1825-137 and G18.0-0.7 may be associated: the lifetime of TeV emitting electrons is expected to be longer compared to the XMM-Newton X-ray emitting electrons, resulting in electrons from earlier epochs (when the spin-down power was larger) contributing to the present TeV flux. These electrons are expected to be synchrotron cooled, which explains the observed photon index of ∼2.4, and the longer lifetime of TeV emitting electrons naturally explains why the TeV nebula is larger than the X-ray size. Finally, supernova remnant expansion into an inhomogeneous medium is expected to create reverse shocks interacting at different times with the pulsar wind nebula, resulting in the offset X-ray and TeV γ-ray morphology.

Abstract Copyright: ∼

Journal keyword(s): ISM: plerions - ISM: individual objects: PSRB1823-13, HESSJ1825-137, G18.0-0.7 - gamma-rays: observations

Simbad objects: 3

Full paper

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Number of rows : 3

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag V	Sp type	#ref 1850 - 2023	#notes
1	NAME Vela Pulsar	Psr	08 35 20.65525	-45 10 35.1545	15.10	~	2252	1
2	PSR J1826-1256	Psr	18 26 08.570	-12 56 33.53		~	123	1
3	PSR B1823-13	Psr	18 26 13.06	-13 34 48.1		~	406	1

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