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23 April 2024

» arxiv » 1210.1359

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Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S
A. Abramowski ; F. Acero ; F. Aharonian ; A.G. Akhperjanian ; G. Anton ; S. Balenderan ; A. Balzer ; A. Barnacka ; Y. Becherini ; J. Becker Tjus ; K. Bernlöhr ; E. Birsin ; J. Biteau ; A. Bochow ; C. Boisson ; J. Bolmont ; P. Bordas ; J. Brucker ; F. Brun ; P. Brun ; T. Bulik ; S. Carrigan ; S. Casanova ; M. Cerruti ; P.M. Chadwick ; A. Charbonnier ; R.C.G. Chaves ; A. Cheesebrough ; G. Cologna ; J. Conrad ; C. Couturier ; M. Dalton ; M.K. Daniel ; I.D. Davids ; B. Degrange ; C. Deil ; P. deWilt ; H.J. Dickinson ; A. Djannati-Ataï ; W. Domainko ; L.O'C. Drury ; F. Dubois ; G. Dubus ; K. Dutson ; J. Dyks ; M. Dyrda ; K. Egberts ; P. Eger ; P. Espigat ; L. Fallon ; C. Farnier ; S. Fegan ; F. Feinstein ; M.V. Fernandes ; D. Fernandez ; A. Fiasson ; G. Fontaine ; A. Förster ; M. Füßling ; M. Gajdus ; Y.A. Gallant ; T. Garrigoux ; H. Gast ; B. Giebels ; J.F. Glicenstein ; B. Glück ; D. Göring ; M.-H. Grondin ; S. Häffner ; J.D. Hague ; J. Hahn ; D. Hampf ; J. Harris ; S. Heinz ; G. Heinzelmann ; G. Henri ; G. Hermann ; A. Hillert ; J.A. Hinton ; W. Hofmann ; P. Hofverberg ; M. Holler ; D. Horns ; A. Jacholkowska ; C. Jahn ; M. Jamrozy ; I. Jung ; M.A. Kastendieck ; K. Katarzyń ski ; U. Katz ; S. Kaufmann ; B. Khélifi ; D. Klochkov ; W. Kluź niak ; T. Kneiske ; Nu. Komin ; K. Kosack ; R. Kossakowski ; F. Krayzel ; P.P. Krüger ; H. Laffon ; G. Lamanna ; J.-P. Lenain ; D. Lennarz ; T. Lohse ; A. Lopatin ; C.-C. Lu ; V. Marandon ; A. Marcowith ; J. Masbou ; G. Maurin ; N. Maxted ; M. Mayer ; T.J.L. McCom ; M.C. Medina ; J. Méhault ; U. Menzler ; R. Moderski ; M. Mohamed ; E. Moulin ; C.L. Naumann ; M. Naumann-Godo ; M. deNaurois ; D. Nedbal ; N. Nguyen ; J. Niemiec ; S.J. Nolan ; S. Ohm ; E. deOñ aWilhelmi ; B. Opitz ; M. Ostrowski ; I. Oya ; M. Panter ; D. Parsons ; M. PazArribas ; N.W. Pekeur ; G. Pelletier ; J. Perez ; P.-O. Petrucci ; B. Peyaud ; S. Pita ; G. Pühlhofer ; M. Punch ; A. Quirrenbach ; M. Raue ; A. Reimer ; O. Reimer ; M. Renaud ; R. delosReyes ; F. Rieger ; J. Ripken ; L. Rob ; S. Rosier-Lees ; G. Rowell ; B. Rudak ; C.B. Rulten ; V. Sahakian ; D.A. Sanchez ; A. Santangelo ; R. Schlickeiser ; A. Schulz ; U. Schwanke ; S. Schwarzburg ; S. Schwemmer ; F. Sheidaei ; J.L. Skilton ; H. Sol ; G. Spengler ; L. Stawarz ; R. Steenkamp ; C. Stegmann ; F. Stinzing ; K. Stycz ; I. Sushch ; A. Szostek ; J.-P. Tavernet ; R. Terrier ; M. Tluczykont ; C. Trichard ; K. Valerius ; C. vanEldik ; G. Vasileiadis ; C. Venter ; A. Viana ; P. Vincent ; H.J. Völk ; F. Volpe ; S. Vorobiov ; M. Vorster ; S.J. Wagner ; M. Ward ; R. White ; A. Wierzcholska ; D. Wouters ; M. Zacharias ; A. Zajczyk ; A.A. Zdziarski ; A. Zech ; H.-S. Zechlin ;
Date:	4 Oct 2012
Abstract:	Vela X is a region of extended radio emission in the western part of the Vela constellation: one of the nearest pulsar wind nebulae (PWNe), and associated with the energetic Vela pulsar (PSR B0833-45). Extended very-high-energy (VHE) $gamma$-ray emission (HESS $mathrm{J0835mhyphen 455}$) was discovered using the H.E.S.S. experiment in 2004. The VHE $gamma$-ray emission was found to be coincident with a region of X-ray emission discovered with ${it ROSAT}$ above 1.5 keV (the so-called extit{Vela X cocoon}): a filamentary structure extending southwest from the pulsar to the centre of Vela X. A deeper observation of the entire Vela X nebula region, also including larger offsets from the cocoon, has been performed with H.E.S.S. This re-observation was carried out in order to probe the extent of the non-thermal emission from the Vela X region at TeV energies and to investigate its spectral properties. In order to increase the sensitivity to the faint $gamma$-ray emission from the very extended Vela X region, a multivariate analysis method combining three complementary reconstruction techniques of Cherenkov-shower images is applied for the selection of $gamma$-ray events. The analysis is performed with the On/Off background method, which estimates the background from separate observations pointing away from Vela X; towards regions free of $gamma$-ray sources but with comparable observation conditions. The $gamma$-ray surface brightness over the large Vela X region reveals that the detection of non-thermal VHE $gamma$-ray emission from the PWN HESS $mathrm{J0835mhyphen 455}$ is statistically significant over a region of radius 1.2$^{circ}$ around the position $alpha$ = 08$^{mathrm{h}}$ 35$^{mathrm{m}}$ 00$^{mathrm{s}}$, $delta$ = -45$^{circ}$ 36$^{mathrm{prime}}$ 00$^{mathrm{prime}mathrm{prime}}$ (J2000).
Source:	arXiv, 1210.1359
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