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28 March 2024
 
  » arxiv » 1009.3012

 Article overview


Revisiting the Westerlund 2 Field with the H.E.S.S. Telescope Array
HESS Collaboration ; A. Abramowski ; F. Acero ; F. Aharonian ; A.G. Akhperjanian ; G. Anton ; A. Barnacka ; U. Barres de Almeida ; A.R. Bazer-Bachi ; Y. Becherini ; J. Becker ; B. Behera ; K. Bernlöhr ; A. Bochow ; C. Boisson ; J. Bolmont ; P. Bordas ; V. Borrel ; J. Brucker ; F. Brun ; P. Brun ; T. Bulik ; I. Büsching ; T. Boutelier ; S. Casanova ; M. Cerruti ; P.M. Chadwick ; A. Charbonnier ; R.C.G. Chaves ; A. Cheesebrough ; J. Conrad ; L.-M. Chounet ; A.C. Clapson ; G. Coignet ; M. Dalton ; M.K. Daniel ; I.D. Davids ; B. Degrange ; C. Deil ; H.J. Dickinson ; A. Djannati-Ataï ; W. Domainko ; L.O'C. Drury ; F. Dubois ; G. Dubus ; J. Dyks ; M. Dyrda ; K. Egberts ; P. Eger ; P. Espigat ; L. Fallon ; C. Farnier ; S. Fegan ; F. Feinstein ; M.V. Fernandes ; A. Fiasson ; A. Förster ; G. Fontaine ; M. Füßling ; S. Gabici ; Y.A. Gallant ; L. Gérard ; D. Gerbig ; B. Giebels ; J.F. Glicenstein ; B. Glück ; P. Goret ; D. Göring ; J.D. Hague ; D. Hampf ; M. Hauser ; S. Heinz ; G. Heinzelmann ; G. Henri ; G. Hermann ; J.A. Hinton ; A. Hoffmann ; W. Hofmann ; P. Hofverberg ; M. Holleran ; S. Hoppe ; D. Horns ; A. Jacholkowska ; O.C. de Jager ; C. Jahn ; I. Jung ; K. Katarzyński ; U. Katz ; S. Kaufmann ; M. Kerschhaggl ; D. Khangulyan ; B. Khélifi ; D. Keogh ; D. Klochkov ; W. Kluźniak24 ; T. Kneiske ; Nu. Komin ; K. Kosack ; R. Kossakowski ; G. Lamanna ; J.-P. Lenain ; D. Lennarz ; T. Lohse ; C.-C. Lu ; V. Marandon ; A. Marcowith ; J. Masbou ; D. Maurin ; T.J.L. McComb ; M.C. Medina ; J. Méhault ; R. Moderski ; E. Moulin ; M. Naumann-Godo ; M. de Naurois ; D. Nedbal ; D. Nekrassov ; N. Nguyen ; B. Nicholas ; J. Niemiec ; S.J. Nolan ; S. Ohm ; J-F. Olive ; E. de Oña Wilhelmi ; B. Opitz ; K.J. Orford ; M. Ostrowski ; M. Panter ; M. Paz Arribas ; G. Pedaletti1 ; G. Pelletier ; P.-O. Petrucci ; S. Pita1 ; G. Pühlhofer ; M. Punch ; A. Quirrenbach ; M. Raue ; S.M. Rayner ; A. Reimer ; O. Reimer ; M. Renaud ; R. de los Reyes ; F. Rieger1 ; J. Ripken ; L. Rob ; S. Rosier-Lees ; G. Rowell ; B. Rudak ; C.B. Rulten ; J. Ruppel ; F. Ryde ; V. Sahakian ; A. Santangelo ; R. Schlickeiser ; F.M. Schöck ; A. Schönwald ; U. Schwanke ; S. Schwarzburg ; S. Schwemmer ; A. Shalchi ; I. Sushch ; M. Sikora ; J.L. Skilton ; H. Sol ; G. Spengler ; Ł. Stawarz ; R. Steenkamp ; C. Stegmann ; F. Stinzing ; A. Szostek ; P.H. Tam ; J.-P. Tavernet ; R. Terrier ; O. Tibolla ; M. Tluczykont ; K. Valerius ; C. van Eldik ; G. Vasileiadis ; C. Venter ; J.P. Vialle ; A. Viana ; P. Vincent ; M. Vivier ; H.J. Völk ; F. Volpe ; S. Vorobiov ; S.J. Wagner ; M. Ward ; A.A. Zdziarski ; A. Zech ; H.-S. Zechlin ; Y. Fukui ; N. Furukawa ; A. Ohama ; H. Sano ; J. Dawson ; A. Kawamura ;
Date 15 Sep 2010
AbstractAims. Previous observations with the H.E.S.S. telescope array revealed the existence of extended very-high-energy (VHE; E>100 GeV) {gamma}-ray emission, HESS J1023-575, coincident with the young stellar cluster Westerlund 2. At the time of discovery, the origin of the observed emission was not unambiguously identified, and follow-up observations have been performed to further investigate the nature of this {gamma}-ray source. Methods. The Carina region towards the open cluster Westerlund 2 has been re-observed, increasing the total exposure to 45.9 h. The combined dataset includes 33 h of new data and now permits a search for energy-dependent morphology and detailed spectroscopy. Results. A new, hard spectrum VHE {gamma}-ray source, HESSJ1026-582, was discovered with a statistical significance of 7{sigma}. It is positionally coincident with the Fermi LAT pulsar PSR J1028-5819. The positional coincidence and radio/{gamma}-ray characteristics of the LAT pulsar favors a scenario where the TeV emission originates from a pulsar wind nebula. The nature of HESS J1023-575 is discussed in light of the deep H.E.S.S. observations and recent multi-wavelength discoveries, including the Fermi LAT pulsar PSRJ1022-5746 and giant molecular clouds in the region. Despite the improved VHE dataset, a clear identification of the object responsible for the VHE emission from HESS J1023-575 is not yet possible, and contribution from the nearby high-energy pulsar and/or the open cluster remains a possibility.
Source arXiv, 1009.3012
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