Hard X-ray emission clumps in the γ-Cygni supernova remnant:: An INTEGRAL-ISGRI view

被引：17

作者：

Bykov, AM

Krassilchtchikov, AM

Uvarov, YA

Bloemen, H

Chevalier, RA

Gustov, MY

Hermsen, W

Lebrun, F

Lozinskaya, TA

Rauw, G

Smirnova, TV

Sturner, SJ

Swings, JP

Terrier, R

Toptygin, IN

机构：

[1] AF Ioffe Phys & Technol, St Petersburg 194021, Russia

[2] SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands

[3] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA

[4] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France

[5] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119899, Russia

[6] Univ Liege, Inst Astron & Geophys, B-4000 Liege, Belgium

[7] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117810, Russia

[8] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2004年 / 427卷 / 03期

关键词：

gamma rays : observations; X rays : ISM : supernova remnants; individual : G78.2+2.1 (gamma-Cygni); radiation mechanisms : nonthermal; cosmic rays;

D O I：

10.1051/0004-6361:200400089

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页码：L21 / L24

页数：4

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