C.D.S. - SIMBAD4 rel 1.7 - 2020.08.09CEST13:53:55

2007A&A...469L..17H - Astronomy and Astrophysics, volume 469, L17-21 (2007/7-1)

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


Abstract (from CDS):

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. A deep (≃50ks) 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. 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. An extended X-ray emission region with a full width half maximum (FWHM) size of ≃12arcmin 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±3arcmin). 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 f_2-10 keV_ ≃7x10–13 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 kBT≃10keV. 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≃10keV) 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.

Abstract Copyright:

Journal keyword(s): acceleration of particles - gamma rays: observations - X-rays: general - gamma rays: theory

Simbad objects: 3

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Number of rows : 3

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 TeV J2032+4130 gam 20 32.1 +41 34           ~ 122 0
2 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1767 2
3 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 794 0

    Equat.    Gal    SGal    Ecl

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