XMM-Newton observations of the first unidentified TeV gamma-ray source TeV J2032+4130

被引：24

作者：

Horns, D.

Hoffmann, A. I. D.

Santangelo, A.

Aharonian, F. A.

Rowell, G. P.

机构：

[1] Inst Astron & Astrophys, D-72076 Tubingen, Germany

[2] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany

[3] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

来源：

ASTRONOMY & ASTROPHYSICS | 2007年 / 469卷 / 01期

关键词：

acceleration of particles; gamma rays : observations; X-rays : general; gamma rays : theory;

D O I：

10.1051/0004-6361:20066836

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The first unidentified very high energy gamma ray source (TeV J2032+4130) in the Cygnus region has been the subject of intensive search for a counterpart source at other wavelengths. In particular, observations in radio and X-rays are important to trace a population of non-thermal electrons. Aims. A deep (approximate to 50 ks) exposure of TeV J2032+4130 with XMM-Newton has been obtained. The large collection area and the field of view of the X-ray telescopes on-board of XMM-Newton allow to search for faint extended X-ray emission possibly linked to TeV J2032+4130. Methods. The contribution of point sources to the observed X-ray emission from TeV J2032+4130 is subtracted from the data. The point-source subtracted X-ray data are analyzed using blank sky exposures and regions adjacent to the position of TeV J2032+4130 in the field of view covered by the XMM-Newton telescopes to search for diffuse X-ray emission. Results. An extended X-ray emission region with a full width half maximum (FWHM) size of approximate to 12 arcmin is found. The centroid of the emission is co-located with the position of TeV J2032+4130. The angular extension of the X-ray emission region is slightly smaller than the angular size of TeV J2032+4130 (FWHM = 14 +/- 3 arcmin). The energy spectrum of the emission coinciding with the position and extension of TeV J2032+4130 can be modeled by a power-law model with a photon index G = 1.5 +/- 0.2(stat) +/- 0.3(sys) and an energy flux integrated between 2 and 10 keV of f(2-10) (keV) approximate to 7 x 10(-13) erg/(cm(2) s) which is lower than the very high energy gamma-ray flux observed from TeV J2032+4130. The energy flux detected from the extended emission region is about a factor of two smaller than the summed contribution of the point sources present. The energy spectrum can also be fit with a thermal emission model from an ionized plasma with a temperature k(B)T approximate to 10 keV. Conclusions. We conclude that the faint extended X-ray emission discovered in this observation is the X-ray counterpart of TeV J2032+4130. Formally, it can not be excluded that the extended emission is due to an unrelated population of faint, hot (kBT approximate to 10 keV) unresolved point-sources which by chance coincides with the position and extension of TeV J2032+4130. We discuss our findings in the frame of both hadronic and leptonic gamma-ray production scenarios.

引用

页码：L17 / L21

页数：5

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