[AIT logo]

Institut für Astronomie und Astrophysik

Abteilung Astronomie

Sand 1, D-72076 Tübingen, Germany
[Uni logo]

Hinweis: Einige Seiten auf astro.uni-tuebingen.de können veraltet sein und werden nicht mehr aktualisiert.
Note: Some webpages at astro.uni-tuebingen.de may be outdated and will no longer be updated.


Preprint 06/07


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

D. Horns (1), A.I.D. Hoffmann (1), A. Santangelo (1), F.A. Aharonian (2), G.P. Rowell (3)

(1) Institute for Astronomy and Astrophysics, University of Tübingen, Germany
(2) Max-Planck-Institute for Nuclear Physics, Heidelberg, Germany
(3) School of Chemistry and Physics, University of Adelaide, Australia

To be published in: A&A Letters

Abstract. (abridged) 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. A deep (~50 ksec) exposure of TeV J2032+4130 with XMM-Newton has been obtained. 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 ~12 arc min is found. The centroid of the emission is co-located with the position of TeV J2032+4130.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 Gamma = 1.5 +/-0.2(stat) +/-0.3(sys) and an energy flux integrated between 2 and 10 keV of f2-10keV ~ 7x10-13 ergs/(cm2 s) which is lower than the very high energy gamma-ray flux observed from TeV J2032+4130. 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 ~ 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.
 

Preprint (195 kb PDF file including figures)
Astrophysics (astro-ph): 0705.0009


[Home Page] [Preprints 2007] [Quick Reference] [Feedback]


Jürgen Barnstedt | Impressum
Last modified 30 Jan 2013
[Valid HTML 4.0!]