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Exploring a SNR/molecular cloud association within HESS J1745-303

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posted on 2012-10-24, 09:09 authored by F. Aharonian, W. Benbow, K. Bernlöhr, O. Bolz, I. Braun, R. Bühler, S. Carrigan, A. C. Clapson, L. Costamante, W. Domainko, K. Egberts, J. -. P. Tavernet, M. Ostrowski, P. Vincent, D. Nedbal, L. Rob, J. Ruppel, R. Schlickeiser, G. Hermann, R. Schröder, Ł. Stawarz, T. Lohse, T. Bulik, J. Dyks, R. Moderski, B. Rudak, K. Katarzyński, J. F. Glicenstein, F. Volpe, S. Funk, A. Djannati-Ataï, E. Moulin, S. Hoppe, C. Hadjichristidis, K. Kosack, D. Nekrassov, S. Ohm, M. Panter, T. J. L. McComb, M. Renaud, Van Eldik C, H. J. Völk, U. Schwanke, A. G. Akhperjanian, V. Sahakian, A. R. Bazer-Bachi, D. Keogh, V. Borrel, J. -. P. Olive, M. Beilicke, P. Pgoret, R. Cornils, G. Heinzelmann, C. Boisson, M. Raue, J. Ripken, M. Dalton, M. Füßling, I. J. Latham, M. Kerschhaggl, J. -. P. Lenain, J. M. Martin, H. Sol, A. Zech, E. Brion, M. Vivier, De Oña Wilhelmi E, Barres De Almeida U, A. M. Brown, P. M. Chadwick, H. J. Dickinson, S. J. Nolan, D. Emmanoulopoulos, K. J. Orford, J. L. Osborne, S. M. Rayner, D. Spangler, G. Pedaletti, M. Ward, F. Feinstein, I. Büsching, M. Holleran, De Jager OC, B. C. Raubenheimer, A. Jacholkowska, C. Venter, L. -. M. Chounet, B. Degrange, S. Pita, G. Fontaine, B. Giebels, B. Khélifi, A. Fiasson, M. Lemoine-Goumard, M. Naumann-Godo, G. Superina, M. Hauser, G. Coignet, M. Punch, F. Dubois, G. Lamanna, S. Rosier-Lees, J. P. Vialle, Y. A. Gallant, P. Espigat, R. Terrier, L. O. Drury, C. Masterson, B. Behera, G. Pühlhofer, A. Shalchi, S. Schwemmer, P. Tam, S. J. Wagner, C. Farnier, N. Komin, A. A. Zdziarski, A. Marcowith, G. Vasileiadis, B. Glück, I. Jung, G. Rowell, F. M. Schöck, A. Förster, C. Stegmann, T. Boutelier, G. Dubus, G. Henri, W. Hofmann, G. Pelletier, P. -. O. Petrucci, A. Hoffmann, R. Steenkamp, D. Horns, E. Kendziorra, A. Santangelo, D. Hauser, S. Schwarzburg, O. Martineau-Huynh, D. Maurin, J. A. Hinton, De Naurois M
Aims. HESS J1745-303 is an extended, unidentified VHE (very high energy) gamma-ray source discovered using HESS in the Galactic Plane Survey. Since no obvious counterpart has previously been found in longer-wavelength data, the processes that power the VHE emission are not well understood. Methods. Combining the latest VHE data with recent XMM-Newton observations and a variety of source catalogs and lower-energy survey data, we attempt to match (from an energetic and positional standpoint) the various parts of the emission of HESS J1745-303 with possible candidates. Results. Though no single counterpart is found to fully explain the VHE emission, we postulate that at least a fraction of the VHE source may be explained by a supernova-remnant/molecular-cloud association and/or a high-spin-down-flux pulsar.

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Citation

Astronomy & Astrophysics, 2008, 483 (2), pp. 509-517

Version

  • VoR (Version of Record)

Published in

Astronomy & Astrophysics

Publisher

EDP Sciences for European Southern Observatory (ESO)

issn

0004-6361

eissn

1432-0746

Copyright date

2008

Available date

2012-10-24

Publisher version

http://www.aanda.org/articles/aa/abs/2008/20/aa9230-07/aa9230-07.html

Language

en

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