Letter to the Editor
XMM-Newton observations of the first unidentified TeV gamma-ray source TeV J2032+4130*
Institute for Astronomy and Astrophysics Tübingen (IAAT) Sand 1, 72076 Tübingen, Germany e-mail: email@example.com
2 Max-Planck Institut für Kernphysik (MPIK) PO Box 10 39 80, 69117 Heidelberg, Germany
3 School of Chemistry and Physics, University of Adelaide, Australia
Accepted: 26 April 2007
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 (≈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 ≈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 Γ=1.5 ± 0.2stat ± 0.3sys and an energy flux integrated between 2 and 10 keV of 710-13 erg/(cm2 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 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 ( 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.
Key words: acceleration of particles / gamma rays: observations / X-rays: general / gamma rays: theory
© ESO, 2007