IAFE   05512
INSTITUTO DE ASTRONOMIA Y FISICA DEL ESPACIO
Unidad Ejecutora - UE
artículos
Título:
A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
Autor/es:
ACERO, F.; BALLET, J.; LEMOINE-GOURMAND, M.; ORTEGA, M.; GIACANI, E.; DUBNER, G.; CASSAM-CHENAI, G.
Revista:
ASTRONOMY AND ASTROPHYSICS
Editorial:
EDP SCIENCES S A
Referencias:
Lugar: Paris; Año: 2009 vol. 505 p. 157 - 167
ISSN:
0004-6361
Resumen:
Context. The supernova remnant (SNR) RX J1713.7-3946 (also known as G347.3-0.5) is part of the class of remnants dominated bysynchrotron emission in X-rays. It is also one of the few shell-type SNRs observed at TeV energies allowing us to investigate particleacceleration at SNRs shock.Aims. Our goal is to compare spatial and spectral properties of the remnant in X- and γ-rays to understand the nature of its TeV emission.This requires the study of the remnant on the same spatial scale at both energies. To complement the non-thermal spectrum ofthe remnant, we attempt to provide a reliable estimate of the radio flux density.Methods. In radio, we revisited ATCA data and used HI and mid-infrared observations to differentiate between the thermal and thenon-thermal emission. In X-rays, we produced a new mosaic of the remnant and degraded the spatial resolution of the X-ray data tothe resolution of the HESS instrument to perform spatially resolved spectroscopy at the same spatial scale in X- and γ-rays. Radialprofiles were obtained to investigate the extension of the emission at both energies.Results. We found that part of the radio emission within the SNR contours is thermal in nature. Taking this into account, we providenew lower and upper limits to the integrated synchrotron flux of the remnant at 1.4 GHz, of 22 Jy and 26 Jy, respectively. In X-rays,we obtained the first full coverage of RX J1713.7-3946 with XMM-Newton. The spatial variation in the photon index seen on smallscale in X-rays is smeared out at HESS resolution. A non-linear correlation between the X- and γ-ray fluxes of the type FX ∝ F2.41γ isfound. If the flux variation is mainly caused by density variation around the remnant then a leptonic model can more easily reproducethe observed X/γ-ray correlation. In some angular sectors, radial profiles indicate that the bulk of the X-ray emission comes morefrom the inside of the remnant than in γ-rays.