2011A&A...533A.103H

Query : 2011A&A...533A.103H

2011A&A...533A.103H - Astronomy and Astrophysics, volume 533A103-103 (2011/9-1)

Discovery of the source HESS J1356-645 associated with the young and energetic PSR J1357-6429.

HESS COLLABORATION, ABRAMOWSKI A., ACERO F., AHARONIAN F., AKHPERJANIAN A.G., ANTON G., BALZER A., BARNACKA A., BARRES DE ALMEIDA U., BECHERINI Y., BECKER J., BEHERA B., BERNLOEHR K., 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., CHOUNET L.-M., CLAPSON A.C., COIGNET G., COLOGNA G., CONRAD J., DALTON M., DANIEL M.K., DAVIDS I.D., DEGRANGE B., DEIL C., DICKINSON H.J., DJANNATI-ATAIE A., DOMAINKO W., DRURY L.O'C., DUBOIS F., 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., GALLANT Y.A., GAST H., GERARD L., GERBIG D., GIEBELS B., GLICENSTEIN J.F., GLUECK B., GORET P., GOERING D., HAEFFNER S., HAGUE J.D., HAMPF D., HAUSER M., HEINZ S., HEINZELMANN G., HENRI G., HERMANN G., HINTON J.A., HOFFMANN A., HOFMANN W., HOFVERBERG P., HOLLER M., HORNS D., JACHOLKOWSKA A., DE JAGER O.C., JAHN C., JAMROZY M., JUNG I., KASTENDIECK M.A., KATARZYNSKI K., KATZ U., KAUFMANN S., KEOGH D., KHANGULYAN D., KHELIFI B., KLOCHKOV D., KLUZNIAK W., KNEISKE T., KOMIN NU., KOSACK K., KOSSAKOWSKI R., LAFFON H., LAMANNA G., LENNARZ D., LOHSE T., LOPATIN A., LU C.-C., MARANDON V., MARCOWITH A., MASBOU J., MAURIN D., MAXTED N., MAYER M., McCOMB T.J.L., MEDINA M.C., MEHAULT J., MODERSKI R., 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., PEDALETTI G., PELLETIER G., PETRUCCI P.-O., PITA S., PUEHLHOFER G., PUNCH M., QUIRRENBACH A., RAUE M., RAYNER S.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., RUPPEL J., SAHAKIAN V., SANCHEZ D., SANTANGELO A., SCHLICKEISER R., SCHOECK F.M., SCHULZ A., SCHWANKE U., SCHWARZBURG S., SCHWEMMER S., SIKORA M., 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., VIALLE J.P., 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):

Several newly discovered very-high-energy (VHE; E>100GeV) γ-ray sources in the Galaxy are thought to be associated with energetic pulsars. Among them, middle-aged (>104yr) systems exhibit large centre-filled VHE nebulae, offset from the pulsar position, which result from the complex relationship between the pulsar wind and the surrounding medium, and reflect the past evolution of the pulsar. Imaging Atmospheric Cherenkov Telescopes (IACTs) have been successful in revealing extended emission from these sources in the VHE regime. Together with radio and X-ray observations, this observational window allows one to probe the energetics and magnetic field inside these large-scale nebulae. H.E.S.S., with its large field of view, angular resolution of ≲0.1° and unprecedented sensitivity, has been used to discover a large population of such VHE sources. In this paper, the H.E.S.S. data from the continuation of the Galactic Plane Survey (-80°<l<60°, |b|<3°), together with the existing multi-wavelength observations, are used. A new VHE γ-ray source was discovered at RA(J2000)=13h56m00s, Dec(J2000)=-64°30m00s with a 2m statistical error in each coordinate, namely HESS J1356-645. The source is extended, with an intrinsic Gaussian width of (0.20±0.02)°. Its integrated energy flux between 1 and 10 TeV of 8x10–12erg/cm2/s represents ∼11% of the Crab Nebula flux in the same energy band. The energy spectrum between 1 and 20TeV is well described by a power law dN/dE ∝ E–Γ with photon index Γ=2.2±0.2stat±0.2sys. The inspection of archival radio images at three frequencies and the analysis of X-ray data from ROSAT/PSPC and XMM-Newton/MOS reveal the presence of faint non-thermal diffuse emission coincident with HESS J1356-645. HESS J1356-645 is most likely associated with the young and energetic pulsar PSR J1357-6429 (d=2.4kpc, τc=7.3kyr and {dot}(E)=3.1x1036erg/s), located at a projected distance of ∼5pc from the centroid of the VHE emission. HESS J1356-645 and its radio and X-ray counterparts would thus represent the nebula resulting from the past history of the PSR J1357-6429 wind. In a simple one-zone model,

Abstract Copyright: ∼

Journal keyword(s): surveys - gamma rays: general - ISM: individual objects: PSR J1357-6429 - ISM: individual objects: HESS J1356-645

Simbad objects: 21

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Number of rows : 21
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 NAME Vela X Psr 08 33 08.880 -45 11 24.36           ~ 302 1
4 NAME Vela SNR 08 34.0 -45 50           ~ 1331 2
5 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1
6 PMN J1355-6435 Rad 13 55 23.00 -64 33 50.0           ~ 3 0
7 [DSH95] 309.8-2.6 SR? 13 56.0 -64 36           ~ 6 0
8 1RXS J135605.5-642902 X 13 56 05.5 -64 29 02           ~ 2 0
9 1RXS J135615.9-642757 X 13 56 15.9 -64 27 57           ~ 1 0
10 MGPS J135623-643323 Rad 13 56 23.9489 -64 33 23.706           ~ 1 0
11 PSR J1357-6429 Psr 13 57 02.525 -64 29 29.89           ~ 171 1
12 3A 1510-590 Psr 15 13 17.000 -59 04 54.00           ~ 434 3
13 PSR B1706-44 Psr 17 09 42.62000 -44 29 12.0000     13.30     ~ 670 1
14 HESS J1718-385 gam 17 18 07 -38 33.0           ~ 32 0
15 SNR G000.9+00.1 SNR 17 47.3 -28 09           ~ 222 1
16 HESS J1809-193 gam 18 10 31 -19 18.0           ~ 70 1
17 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 460 1
18 SNR G021.5-00.9 SNR 18 33 33.612 -10 34 07.69           ~ 490 1
19 SNR G029.7-00.3 SNR 18 46 22.8 -02 59 47           ~ 375 2
20 [DSH95] 310.5-3.5 SR? ~ ~           ~ 4 0
21 [DSH95] 310.6-2.0 SR? ~ ~           ~ 4 0

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