2012A&A...548A..46H

Query : 2012A&A...548A..46H

2012A&A...548A..46H - Astronomy and Astrophysics, volume 548A46-46 (2012/12-1)

Identification of HESS J1303-631 as a pulsar wind nebula through γ-ray, X-ray, and radio observations.

HESS COLLABORATION, ABRAMOWSKI A., ACERO F., AHARONIAN F., AKHPERJANIAN A.G., ANTON G., BALENDERAN S., BALZER A., BARNACKA A., BECHERINI Y., BECKER J., BERNLOEHR K., BIRSIN E., BITEAU J., BOCHOW A., BOISSON C., BOLMONT J., BORDAS P., BRUCKER J., BRUN F., BRUN P., BULIK T., BUESCHING I., CARRIGAN S., CASANOVA S., CERRUTI M., CHADWICK P.M., CHARBONNIER A., CHAVES R.C.G., CHEESEBROUGH A., COLOGNA G., CONRAD J., COUTURIER C., DALTON M., DANIEL M.K., DAVIDS I.D., DEGRANGE B., DEIL C., DICKINSON H.J., DJANNATI-ATAIE A., DOMAINKO W., DRURY L.O'C., DUBUS G., DUTSON K., DYKS J., DYRDA M., EGBERTS K., EGER P., ESPIGAT P., FALLON L., FARNIER C., FEGAN S., FEINSTEIN F., FERNANDES M.V., FIASSON A., FONTAINE G., FOERSTER A., FUESSLING M., GAJDUS M., GALLANT Y.A., GARRIGOUX T., GAST H., GERARD L., GIEBELS B., GLICENSTEIN J.F., GLUECK B., GOERING D., GRONDIN M.-H., HAEFFNER S., HAGUE J.D., HAHN J., HAMPF D., HARRIS J., HAUSER M., HEINZ S., HEINZELMANN G., HENRI G., HERMANN G., HILLERT A., HINTON J.A., HOFMANN W., HOFVERBERG P., HOLLER M., HORNS D., JACHOLKOWSKA A., JAHN C., JAMROZY M., JUNG I., KASTENDIECK M.A., KATARZYNSKI K., KATZ U., KAUFMANN S., KHELIFI B., KLOCHKOV D., KLUZNIAK W., KNEISKE T., KOMIN NU., KOSACK K., KOSSAKOWSKI R., KRAYZEL F., LAFFON H., LAMANNA G., LENAIN J.-P., LENNARZ D., LOHSE T., LOPATIN A., LU C.-C., MARANDON V., MARCOWITH A., MASBOU J., MAURIN G., MAXTED N., MAYER M., McCOMB T.J.L., MEDINA M.C., MEHAULT J., MENZLER U., MODERSKI R., MOHAMED M., MOULIN E., NAUMANN C.L., NAUMANN-GODO M., DE NAUROIS M., NEDBAL D., NEKRASSOV D., NGUYEN N., NICHOLAS B., NIEMIEC J., NOLAN S.J., OHM S., DE ONA WILHELMI E., OPITZ B., OSTROWSKI M., OYA I., PANTER M., PAZ ARRIBAS M., PEKEUR N.W., PELLETIER G., PEREZ J., PETRUCCI P.-O., PEYAUD B., PITA S., PUEHLHOFER G., PUNCH M., QUIRRENBACH A., RAUE M., REIMER A., REIMER O., RENAUD M., DE LOS REYES R., RIEGER F., RIPKEN J., ROB L., ROSIER-LEES S., ROWELL G., RUDAK B., RULTEN C.B., SAHAKIAN V., SANCHEZ D.A., SANTANGELO A., SCHLICKEISER R., SCHULZ A., SCHWANKE U., SCHWARZBURG S., SCHWEMMER S., SHEIDAEI F., SKILTON J.L., SOL H., SPENGLER G., STAWARZ L., STEENKAMP R., STEGMANN C., STINZING F., STYCZ K., SUSHCH I., SZOSTEK A., TAVERNET J.-P., TERRIER R., TLUCZYKONT M., VALERIUS K., VAN ELDIK C., VASILEIADIS G., VENTER C., VIANA A., VINCENT P., VOELK H.J., VOLPE F., VOROBIOV S., VORSTER M., WAGNER S.J., WARD M., WHITE R., WIERZCHOLSKA A., ZACHARIAS M., ZAJCZYK A., ZDZIARSKI A.A., ZECH A. and ZECHLIN H.-S.

Abstract (from CDS):

The previously unidentified very high-energy (VHE; E>100GeV) γ-ray source HESS J1303-631, discovered in 2004, is re-examined including new data from the H.E.S.S. Cherenkov telescope array in order to identify this object. Archival data from the XMM-Newton X-ray satellite and from the PMN radio survey are also examined. Detailed morphological and spectral studies of VHE γ-ray emission as well as of the XMM-Newton X-ray data are performed. Radio data from the PMN survey are used as well to construct a leptonic model of the source. The γ-ray and X-ray spectra and radio upper limit are used to construct a one zone leptonic model of the spectral energy distribution (SED). Significant energy-dependent morphology of the γ-ray source is detected with high-energy emission (E>10TeV) positionally coincident with the pulsar PSR J1301-6305 and lower energy emission (E<2TeV) extending ∼0.4° to the southeast of the pulsar. The spectrum of the VHE source can be described with a power-law with an exponential cut-off N0=(5.6 ±0.5)x10–12TeV–1cm–2s–1, Γ=1.5±0.2) and Ecut=(7.7±2.2)TeV. The pulsar wind nebula (PWN) is also detected in X-rays, extending ∼2-3' from the pulsar position towards the center of the γ-ray emission region. A potential radio counterpart from the PMN survey is also discussed, showing a hint for a counterpart at the edge of the X-ray PWN trail and is taken as an upper limit in the SED. The extended X-ray PWN has an unabsorbed flux of F2–10keV∼1.6+0.2–0.4x10–13erg/cm2/s and is detected at a significance of 6.5σ. The SED is well described by a one zone leptonic scenario which, with its associated caveats, predicts a very low average magnetic field for this source. Significant energy-dependent morphology of this source, as well as the identification of an associated X-ray PWN from XMM-Newton observations enable identification of the VHE source as an evolved PWN associated to the pulsar PSR J1301-6305. This identification is supported by the one zone leptonic model, which suggests that the energetics of the γ-ray and X-ray radiation are such that they may have a similar origin in the pulsar nebula. However, the large discrepancy in emission region sizes and the low level of synchrotron radiation suggest a multi-population leptonic nature. The low implied magnetic field suggests that the PWN has undergone significant expansion. This would explain the low level of synchrotron radiation and the difficulty in detecting counterparts at lower energies, the reason this source was originally classified as a ``dark'' VHE γ-ray source.

Abstract Copyright: ∼

Journal keyword(s): Gamma rays: general - pulsars: individual: PSR J1301-6305 - ISM: individual objects: HESS J1303-631

Simbad objects: 24

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Number of rows : 24
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
2 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5476 0
3 PSR J1301-6310 Psr 13 01 28.30 -63 10 40.5           ~ 14 1
4 PSR J1302-6313 Psr 13 02 19.2 -63 13 29           ~ 4 1
5 CPD-63 2495 HXB 13 02 47.6544015048 -63 50 08.626970292 10.34 10.72 9.98 10.03   O9.5Ve 852 0
6 PSR J1301-6305 Psr 13 02 47.9992676 -63 10 48.001099           ~ 139 2
7 PSR J1303-6305 Psr 13 03 00.02 -63 05 00.8           ~ 9 1
8 IRAS 13010-6254 HII 13 04 09.7 -63 10 22           ~ 6 0
9 PSR J1305-6256 Psr 13 05 28.0 -62 56 39           ~ 6 0
10 PSR J1357-6429 Psr 13 57 02.525 -64 29 29.89           ~ 171 1
11 PSR J1614-5048 Psr 16 14 11.29 -50 48 03.5           ~ 128 0
12 HESS J1702-420 gam 17 02 44.0 -42 00 57           ~ 46 0
13 PSR B1731-33.5 Psr 17 34 26.6 -33 33 22           ~ 104 1
14 GCIRS 13 Em* 17 45 39.76 -29 00 29.8           ~ 144 0
15 CXOGC J174539.7-290022 Psr 17 45 39.80 -29 00 19.9           ~ 54 1
16 NAME Mouse Rad 17 47 15.78 -29 58 01.0           ~ 120 1
17 PSR B1757-24 Psr 18 01 00.016 -24 51 27.50           ~ 258 1
18 PSR B1800-21 Psr 18 03 51.40000 -21 37 07.0000           ~ 278 1
19 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 460 1
20 PSR B1929+10 Psr 19 32 14.0570 +10 59 33.380           ~ 801 0
21 PSR B1951+32 Psr 19 52 58.181 +32 52 40.98           ~ 615 2
22 PSR B1953+50 Psr 19 55 18.7637 +50 59 55.292           ~ 90 0
23 TeV J2032+4130 gam 20 31.7 +41 31           ~ 148 0
24 PSR B2223+65 Psr 22 25 52.8627 +65 35 36.371           ~ 342 0

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