XMM-Newton observations of HESS J1813-178 reveal a composite Supernova remnant

被引:53
作者
Funk, S.
Hinton, J. A.
Moriguchi, Y.
Aharonian, F. A.
Fukui, Y.
Hofmann, W.
Horns, D.
Puehlhofer, G.
Reimer, O.
Rowell, G.
Terrier, R.
Vink, J.
Wagner, S. J.
机构
[1] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany
[2] SLAC, Kavli Inst Astroparticle Phys & Cosmol, Menlo Pk, CA 94025 USA
[3] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
[4] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan
[5] Dublin Inst Adv Studies, Dublin 2, Ireland
[6] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany
[7] Heidelberg Univ, D-69117 Heidelberg, Germany
[8] Stanford Univ, HEPL, Moffett Field, CA 94035 USA
[9] Stanford Univ, KIPAC, Moffett Field, CA 94035 USA
[10] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia
[11] APC, F-75231 Paris 05, France
[12] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands
关键词
ISM : supernova remnants; ISM : individual objects : HESS J1813-178; ISM : individual objects : G12.82-0.02 ISM : individual objects : AXJ1813-178; gamma rays : observations; GAMMA-RAY EMISSION; GALACTIC PLANE; INNER GALAXY; DISCOVERY; RADIATION; GAS;
D O I
10.1051/0004-6361:20066779
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. We present X-ray and (CO)-C-12(J = 1-0) observations of the very-high-energy (VHE) gamma-ray source HESS J1813-178 with the aim of understanding the origin of the gamma-ray emission. Methods. High-angular resolution X-ray studies of the VHE gamma-ray emission region are performed using 18.6 ks of XMM-Newton data, taken on HESS J1813-178 in October 2005. Using this data set we are able to undertake spectral and morphological studies of the X-ray emission from this object with greater precision than previous studies. NANTEN (CO)-C-12(J=1-0) data are used to search for correlations of the X-ray emission with molecular clouds which could act as target material for X-ray production in a hadronic scenario. Results. The NANTEN (CO)-C-12(J = 1- 0) observations show a giant molecular cloud of mass 2.5 x 10(5) M-circle dot at a distance of 4 kpc in the vicinity of HESS J1813- 178. Even though there is no direct positional coincidence, this giant cloud may have influenced the evolution of the X-ray source and its surroundings. The X- ray data show a highly absorbed ( n(H) similar to 1. x 10(23) cm(-2)) non-thermal X-ray emitting object coincident with the previously known ASCA source AXJ1813-178 exhibiting a compact core and an extended tail towards the north- east, located in the centre of the radio shell- type Supernova remnant ( SNR) G12.82 - 0.02. This central object shows morphological and spectral resemblance to a Pulsar Wind Nebula ( PWN) and we therefore consider that this object is very likely to be a composite SNR. We discuss the scenario in which the gamma-rays originate in the shell of the SNR, and that in which they originate in the central object, in terms of a time- dependent one- zone leptonic model. We demonstrate, that in order to connect the core X-ray emission to the VHE gamma-ray emission electrons have to be accelerated to energies of at least 1 PeV.
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页码:249 / 257
页数:9
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