2006A&A...460..365A

Query : 2006A&A...460..365A

2006A&A...460..365A - Astronomy and Astrophysics, volume 460365-374 (2006/12-3)

Energy dependent γ-ray morphology in the pulsar wind nebula HESS J1825-137.

AHARONIAN F., AKHPERJANIAN A.G., BAZER-BACHI A.R., BEILICKE M., BENBOW W., BERGE D., BERNLOEHR K., BOISSON C., BOLZ O., BORREL V., BRAUN I., BROWN A.M., BUEHLER R., BUESCHING I., CARRIGAN S., CHADWICK P.M., CHOUNET L.-M., CORNILS R., COSTAMANTE L., DEGRANGE B., DICKINSON H.J., DJANNATI-ATAIE A., DRURY L.O'C., DUBUS G., EGBERTS K., EMMANOULOPOULOS D., ESPIGAT P., FEINSTEIN F., FERRERO E., FIASSON A., FONTAINE G., FUNK S., FUNK S., FUESSLING M., GALLANT Y.A., GIEBELS B., GLICENSTEIN J.F., GORET P., HADJICHRISTIDIS C., HAUSER D., HAUSER M., HEINZELMANN G., HENRI G., HERMANN G., HINTON J.A., HOFFMANN A., HOFMANN W., HOLLERAN M., HORNS D., JACHOLKOWSKA A., DE JAGER O.C., KENDZIORRA E., KHELIFI B., KOMIN N., KONOPELKO A., KOSACK K., LATHAM I.J., LE GALLOU R., LEMIERE A., LEMOINE-GOUMARD M., LOHSE T., MARTIN J.M., MARTINEAU-HUYNH O., MARCOWITH A., MASTERSON C., MAURIN G., McCOMB T.J.L., MOULIN E., DE NAUROIS M., NEDBAL D., 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., RAYNER S.M., REIMER A., REIMER O., RIPKEN J., ROB L., ROLLAND L., ROWELL G., SAHAKIAN V., SANTANGELO A., SAUGE L., SCHLENKER S., SCHLICKEISER R., SCHROEDER R., SCHWANKE U., SCHWARZBURG S., SHALCHI A., SOL H., SPANGLER D., SPANIER F., STEENKAMP R., STEGMANN C., SUPERINA G., TAVERNET J.-P., TERRIER R., THEORET C.G., TLUCZYKONT M., VAN ELDIK C., VASILEIADIS G., VENTER C., VINCENT P., VOELK H.J., WAGNER S.J. and WARD M.

Abstract (from CDS):

We present results from deep γ-ray observations of the Galactic pulsar wind nebula HESS J1825-137 performed with the HESS array. Detailed morphological and spatially resolved spectral studies reveal the very high-energy (VHE) γ-ray aspects of this object with unprecedented precision. We confirm previous results obtained in a survey of the Galactic Plane in 2004. The γ-ray emission extends asymmetrically to the south and south-west of the energetic pulsar PSR J1826-1334, that is thought to power the pulsar wind nebula. The differential γ-ray spectrum of the whole emission region is measured over more than two orders of magnitude, from 270GeV to 35TeV, and shows indications for a deviation from a pure power law. Spectra have also been determined for spatially separated regions of HESS J1825-137. The photon indices from a power-law fit in the different regions show a softening of the spectrum with increasing distance from the pulsar and therefore an energy dependent morphology. This is the first time that an energy dependent morphology has been detected in the VHE γ-ray regime. The VHE γ-ray emission of HESS J1825-137 is phenomenologically discussed in the scenario where the γ-rays are produced by VHE electrons via Inverse Compton scattering. The high γ-ray luminosity of the source cannot be explained on the basis of constant spin-down power of the pulsar and requires higher injection power in past.

Abstract Copyright: ∼

Journal keyword(s): ISM: supernova remnants - ISM: individual objects: PSR B1823-13 - gamma rays: observations - pulsars: general - ISM: individual objects: HESS J1825 - ISM: individual objects: G18.0-0.7

Simbad objects: 15

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Number of rows : 15

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Sp type	#ref 1850 - 2026	#notes
1	SNR G130.7+03.1	SNR	02 05 35.73	+64 49 41.3					~	661	4
2	M 1	SNR	05 34 31.8	+22 01 03					~	6516	1
3	V* CM Tau	Psr	05 34 31.9474694616	+22 00 52.153698024					~	5476	0
4	NAME Vela X	Psr	08 33 08.880	-45 11 24.36					~	302	1
5	NAME Vela Pulsar	Psr	08 35 20.65525	-45 10 35.1545			15.10		~	2446	1
6	PSR J1418-6058	Psr	14 18 42.725	-60 58 01.89					~	129	0
7	NAME Kookaburra	reg	14 19	-60.9					~	56	1
8	PSR J1420-6048	Psr	14 20 08.190	-60 48 14.85					~	214	0
9	3A 1510-590	Psr	15 13 17.000	-59 04 54.00					~	434	3
10	SNR G347.3-00.5	SNR	17 12 27	-39 41.2			12.27		~	761	1
11	SNR G000.9+00.1	SNR	17 47.3	-28 09					~	222	1
12	PSR J1826-1256	Psr	18 26 08.570	-12 56 33.53					~	152	1
13	PSR B1823-13	Psr	18 26 13.06	-13 34 48.1					~	460	1
14	V* V479 Sct	HXB	18 26 15.0561548880	-14 50 54.247274304	12.02	12.23	11.27	11.04	ON6V((f))z	613	2
15	SNR G021.5-00.9	SNR	18 33 33.612	-10 34 07.69					~	490	1

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