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

被引:72
作者
Aharonian, F. [1 ,14 ]
Akhperjanian, A. G. [2 ]
de Almeida, U. Barres [8 ]
Bazer-Bachi, A. R. [3 ]
Behera, B. [15 ]
Beilicke, M. [4 ]
Benbow, W. [1 ]
Bernloehr, K. [1 ,5 ]
Boisson, C. [6 ]
Bolz, O. [1 ]
Borrel, V. [3 ]
Braun, I. [1 ]
Brion, E. [7 ]
Brown, A. M. [8 ]
Buehler, R. [1 ]
Bulik, T. [25 ]
Buesching, I. [9 ]
Boutelier, T. [18 ]
Carrigan, S. [1 ]
Chadwick, P. M. [8 ]
Chounet, L. -M. [10 ]
Clapson, A. C. [1 ]
Coignet, G. [11 ]
Cornils, R. [4 ]
Costamante, L. [1 ,29 ,30 ]
Dalton, M. [5 ]
Degrange, B. [10 ]
Dickinson, H. J. [8 ]
Djannati-Atai, A. [12 ,13 ]
Domainko, W. [1 ]
Drury, L. O'C. [14 ]
Dubois, F. [11 ]
Dubus, G. [18 ]
Dyks, J. [25 ]
Egberts, K. [1 ]
Emmanoulopoulos, D. [15 ]
Espigat, P. [12 ,13 ]
Farnier, C. [16 ]
Feinstein, F. [16 ]
Fiasson, A. [16 ]
Foerster, A. [1 ]
Fontaine, G. [10 ]
Funk, S. [31 ]
Fuessling, M. [5 ]
Gallant, Y. A. [16 ]
Giebels, B. [10 ]
Glicenstein, J. F. [7 ]
Glueck, B. [17 ]
Goret, P. [7 ]
Hadjichristidis, C. [8 ]
机构
[1] Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany
[2] Yerevan Phys Inst, Yerevan 375036, Armenia
[3] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31029 Toulouse 4, France
[4] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany
[5] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany
[6] Univ Paris 05, CNRS, Observ Paris, LUTH, F-92190 Meudon, France
[7] CE Saclay, CEA, DSM, DAPNIA, F-91191 Gif Sur Yvette, France
[8] Univ Durham, Dept Phys, Durham DH1 3LE, England
[9] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa
[10] Ecole Polytech, IN2P3, Lab Leprince Ringuet, CNRS, F-91128 Palaiseau, France
[11] CNRS IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France
[12] Univ Paris 07, CNRS, F-75205 Paris 13, France
[13] Univ Paris 07, CNRS, Observ Paris, CEA,UMR 7164, F-75221 Paris 05, France
[14] Dublin Inst Adv Studies, Dublin 2, Ireland
[15] Heidelberg Univ, D-69117 Heidelberg, Germany
[16] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, F-34095 Montpellier, France
[17] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany
[18] Univ Grenoble 1, CNRS, INSU, Lab Astrophys Grenoble, F-38041 Grenoble, France
[19] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany
[20] Univ Paris 07, Univ Paris 06, LPNHE, CNRS,IN2P3, F-75252 Paris 5, France
[21] Charles Univ Prague, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic
[22] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany
[23] Univ Namibia, Windhoek, Namibia
[24] Jagiellonian Univ, Obserwatorium Astron, Krakow, Poland
[25] Nicholas Copernicus Astron Ctr, Warsaw, Poland
[26] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
[27] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia
[28] Nicholas Copernicus Univ, Torun Ctr Astron, Torun, Poland
[29] CNRS, European Associated Lab Gamma Ray Astron, Paris, France
[30] MPG, European Associated Lab Gamma Ray Astron, Munich, Germany
[31] SLAC, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA
来源
ASTRONOMY & ASTROPHYSICS | 2008年 / 483卷 / 02期
基金
英国科学技术设施理事会;
关键词
gamma rays : observations; X-rays : general; galaxy : general; ISM : cosmic rays; ISM : clouds;
D O I
10.1051/0004-6361:20079230
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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.
引用
收藏
页码:509 / 517
页数:9
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