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29 March 2024
 
  » arxiv » 1310.6956

 Article overview


HESS J1818-154, a new composite supernova remnant discovered in TeV gamma rays and X-rays
H.E.S.S. Collaboration ; A. Abramowski ; F. Aharonian ; F. Ait Benkhali ; A.G. Akhperjanian ; E. Angüner ; G. Anton ; S. Balenderan ; A. Balzer ; A. Barnacka ; Y. Becherini ; J. Becker Tjus ; K. Bernlöhr ; E. Birsin ; E. Bissaldi ; J. Biteau ; M. Böttcher ; C. Boisson ; J. Bolmont ; P. Bordas ; J. Brucker ; F. Brun ; P. Brun ; T. Bulik ; S. Carrigan ; S. Casanova ; M. Cerruti ; P.M. Chadwick ; R. Chalme-Calvet ; R.C.G. Chaves ; A. Cheesebrough ; M. Chrétien ; S. Colafrancesco ; G. Cologna ; J. Conrad ; C. Couturier ; Y. Cui ; M. Dalton ; M.K. Daniel ; I.D. Davids ; B. Degrange ; C. Deil ; P. de Wilt ; H.J. Dickinson ; A. Djannati-Ataï ; W. Domainko ; L.O'C. Drury ; G. Dubus ; K. Dutson ; J. Dyks ; M. Dyrda ; T. Edwards ; K. Egberts ; P. Eger ; P. Espigat ; 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 ; G. Giavitto ; B. Giebels ; J.F. Glicenstein ; M.-H. Grondin ; M. Grudzińska ; S. Häffner ; J. Hahn ; J. Harris ; G. Heinzelmann ; G. Henri ; G. Hermann ; O. Hervet ; A. Hillert ; J.A. Hinton ; W. Hofmann ; P. Hofverberg ; M. Holler ; D. Horns ; A. Jacholkowska ; C. Jahn ; M. Jamrozy ; M. Janiak ; F. Jankowsky ; I. Jung ; M.A. Kastendieck ; K. Katarzynski ; U. Katz ; S. Kaufmann ; B. Khélifi ; M. Kieffer ; S. Klepser ; D. Klochkov ; W. Kluźniak ; T. Kneiske ; D. Kolitzus ; Nu. Komin ; K. Kosack ; S. Krakau ; F. Krayzel ; P.P. Krüger ; H. Laffon ; G. Lamanna ; J. Lefaucheur ; A. Lemière ; M. Lemoine-Goumard ; J.-P. Lenain ; D. Lennarz ; T. Lohse ; A. Lopatin ; C.-C. Lu ; V. Marandon ; A. Marcowith ; R. Marx ; G. Maurin ; N. Maxted ; M. Mayer ; T.J.L. McComb ; J. Méhault ; P.J. Meintjes ; U. Menzler ; M. Meyer ; R. Moderski ; M. Mohamed ; E. Moulin ; T. Murach ; C.L. Naumann ; M. de Naurois ; J. Niemiec ; S.J. Nolan ; L. Oakes ; S. Ohm ; E. de Ona Wilhelmi ; B. Opitz ; M. Ostrowski ; I. Oya ; M. Panter ; R.D. Parsons ; M. Paz Arribas ; N.W. Pekeur ; G. Pelletier ; J. Perez ; P.-O. Petrucci ; B. Peyaud ; S. Pita ; H. Poon ; G. Pühlhofer ; M. Punch ; A. Quirrenbach ; S. Raab ; M. Raue ; A. Reimer ; O. Reimer ; M. Renaud ; R. de los Reyes ; F. Rieger ; L. Rob ; C. Romoli ; S. Rosier-Lees ; G. Rowell ; B. Rudak ; C.B. Rulten ; V. Sahakian ; D.A. Sanchez ; A. Santangelo ; R. Schlickeiser ; F. Schüssler ; A. Schulz ; U. Schwanke ; S. Schwarzburg ; S. Schwemmer ; H. Sol ; G. Spengler ; F. Spies ; L. Stawarz ; R. Steenkamp ; C. Stegmann ; F. Stinzing ; K. Stycz ; I. Sushch ; A. Szostek ; J.-P. Tavernet ; T. Tavernier ; A.M. Taylor ; R. Terrier ; M. Tluczykont ; C. Trichard ; K. Valerius ; C. van Eldik ; B. van Soelen ; G. Vasileiadis ; C. Venter ; A. Viana ; P. Vincent ; H.J. Völk ; F. Volpe ; M. Vorster ; T. Vuillaume ; S.J. Wagner ; P. Wagner ; M. Ward ; M. Weidinger ; Q. Weitzel ; R. White ; A. Wierzcholska ; P. Willmann ; A. Wörnlein ; D. Wouters ; V. Zabalza ; M. Zacharias ; A. Zajczyk ; A.A. Zdziarski ; A. Zech ; H.-S. Zechlin ;
Date 25 Oct 2013
AbstractComposite supernova remnants (SNRs) constitute a small subclass of remnants of massive stellar explosions where non-thermal radiation is observed from both the expanding shell-like shock front and from a pulsar wind nebula (PWN) located inside of the SNR. These systems represent a unique evolutionary phase of SNRs where observations in the radio, X-ray and gamma-ray regimes allow the study of the co-evolution of both of these energetic phenomena. In this article, we report results from observations of the shell-type SNR G15.4+0.1 performed with the High Energy Stereoscopic System (H.E.S.S.) and XMM-Newton. A compact TeV gamma-ray source, HESSJ1818-154, located in the center and contained within the shell of G15.4+0.1 is detected by H.E.S.S. featuring a spectrum best represented by a power-law model with a spectral index of $-2.3 pm 0.3_{stat} pm 0.2_{sys}$ and an integral flux of F$(>0.42,mathrm{TeV}$)=($0.9 pm 0.3_{mathrm{stat}} pm 0.2_{mathrm{sys}}) imes 10^{-12}$ cm$^{-2}$ s$^{-1}$. Furthermore, a recent observation with XMM-Newton reveals extended X-ray emission strongly peaked in the center of G15.4+0.1. The X-ray source shows indications for an energy-dependent morphology featuring a compact core at energies above 4 keV and more extended emission that fills the entire region within the SNR at lower energies. Together, the X-ray and VHE gamma-ray emission provide strong evidence for the existence of a PWN located inside the shell of G15.4+0.1 and this SNR can therefore be classified as a composite based on these observations. The radio, X-ray and gamma-ray emission from the PWN is compatible with a one-zone leptonic model which requires a low average magnetic field inside the emission region. An unambiguous counterpart to the putative pulsar, thought to power the PWN, has not been detected neither in radio nor in X-ray observations of G15.4+0.1.
Source arXiv, 1310.6956
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