Reference : Hard X-ray emission clumps in the gamma-Cygni supernova remnant: An INTEGRAL-ISGRI view
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
Hard X-ray emission clumps in the gamma-Cygni supernova remnant: An INTEGRAL-ISGRI view
Bykov, A. M. [> > > >]
Krassilchtchikov, A. M. [> > > >]
Uvarov, Y. A. [> > > >]
Bloemen, H. [> > > >]
Chevalier, R. A. [> > > >]
Gustov, M. Y. [> > > >]
Hermsen, W. [> > > >]
Lebrun, F. [> > > >]
Lozinskaya, T. A. [> > > >]
Rauw, Grégor mailto [Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Smirnova, T. V. [> > > >]
Sturner, S. J. [> > > >]
Swings, Jean-Pierre mailto [Université de Liège - ULiège > Département d'astrophys.]
Terrier, R. [> > > >]
Toptygin, I. N. [> > > >]
Astronomy and Astrophysics
E D P Sciences
Yes (verified by ORBi)
Les Ulis Cedex A
[en] gamma rays : observations ; X rays : ISM : supernova remnants ; individual : G78.2+2.1 (gamma-Cygni) ; radiation mechanisms : nonthermal ; cosmic rays
[en] Spatially resolved images of the galactic supernova remnant G78.2+2.1 (gamma-Cygni) in hard X-ray energy bands from 25 keV to 120 keV are obtained with the IBIS-ISGRI imager aboard the International Gamma-Ray Astrophysics Laboratory INTEGRAL. The images are dominated by localized clumps of about ten arcmin in size. The flux of the most prominent North-Western (NW) clump is (1.7+/-0.4)x10(-11) erg cm(-2) s(-1) in the 25-40 keV band. The observed X-ray fluxes are in agreement with extrapolations of soft X-ray imaging observations of gamma-Cyg by ASCA GIS and spatially unresolved RXTE PCA data. The positions of the hard X-ray clumps correlate with bright patches of optical line emission, possibly indicating the presence of radiative shock waves in a shocked cloud. The observed spatial structure and spectra are consistent with model predictions of hard X-ray emission from nonthermal electrons accelerated by a radiative shock in a supernova interacting with an interstellar cloud, but the powerful stellar wind of the O9V star HD 193322 is a plausible candidate for the NW source as well.

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