HESS J1632-478: an energetic relic
INTEGRAL Science Data Centre, Université de Genève, Chemin d'Ecogia 16, 1290
Versoix, Switzerland e-mail: Matteo.Balbo@unige.ch
2 Observatoire de Genève, Université de Genève, Chemin des Maillettes 51, 1290 Sauverny, Switzerland
3 Département de Physique Nucléaire et Corpusculaire, Université de Genève, Quai Ernest-Ansermet 24, 1211 Genève 4, Switzerland
4 AIM Paris Saclay, CEA/DSM-CNRS/INSU-Université Paris Diderot, IRFU/Service d'Astrophysique, 91191 Gif-sur-Yvette, France
Accepted: 4 July 2010
Aims. HESS J1632-478 is an extended and still unidentified TeV source in the galactic plane.
Methods. In order to identify the source of the very high energy emission and to constrain its spectral energy distribution, we used a deep observation of the field obtained with XMM-Newton together with data from Molonglo, Spitzer and Fermi to detect counterparts at other wavelengths.
Results. The flux density emitted by HESS J1632-478 peaks at very high energies and is more than 20 times weaker at all other wavelengths probed. The source spectrum features two large prominent bumps with the synchrotron emission peaking in the ultraviolet and the external inverse Compton emission peaking in the TeV. HESS J1632-478 is an energetic pulsar wind nebula with an age of the order of 104 years. Its bolometric (mostly GeV-TeV) luminosity reaches 10% of the current pulsar spin down power. The synchrotron nebula has a size of 1 pc and contains an unresolved point-like X-ray source, probably the pulsar with its wind termination shock.
Key words: acceleration of particles / stars: neutron / gamma rays: stars / X-rays: stars / pulsar: general
© ESO, 2010