Query : 2004A&A...427..199C

2004A&A...427..199C - Astronomy and Astrophysics, volume 427, 199-216 (2004/11-3)

XMM-Newton observations of the supernova remnant RX J1713.7-3946 and its central source.


Abstract (from CDS):

We present new results from the observations of the supernova remnant (SNR) RX J1713.7-3946 (also G347.3-0.5) performed in five distinct pointings with the EPIC instrument on board the satellite XMM-Newton. RX J1713.7-3946 is a shell-type SNR dominated by synchrotron radiation in the X-rays. Its emission (emission measure and photon index) as well as the absorption along the line-of-sight has been characterized over the entire SNR. The X-ray mapping of the absorbing column density has revealed strong well-constrained variations (0.4x1022cm–2≤NH≤1.1x1022cm–2) and, particularly, a strong absorption in the southwest. Moreover, there are several clues indicating that the shock front of RX J1713.7-3946 is impacting the clouds responsible for the absorption as revealed for instance by the positive correlation between X-ray absorption and X-ray brightness along the western rims. The CO and HI observations show that the inferred cumulative absorbing column densities are in excellent agreement with the X-ray findings in different parts of the remnant on condition that the SNR lies at a distance of 1.3±0.4kpc, probably in the Sagittarius galactic arm, instead of the commonly-accepted value of 6kpc. An excess in the CO emission is found in the southwest suggesting that the absorption is due to molecular clouds. A search for OH masers in the southwestern region has been unsuccessful, possibly due to the low density of the clouds. The X-ray mapping of the photon index has also revealed strong variations (1.8=Γ≤2.6). The spectrum is steep in the faint central regions and flat at the presumed shock locations, particularly in the southeast. Nevertheless, the regions where the shock impacts molecular clouds have a steeper spectrum than those where the shock propagates into a low density medium. The search for the thermal emission in RX J1713.7-3946 has been unsuccessful leading to a number density upper limit of 2x10–2cm–3 in the ambient medium. This low density corresponds to a reasonable kinetic energy of the explosion provided that the remnant is less than a few thousand years old. A scenario based on a modified ambient medium due to the effect of a progenitor stellar wind is proposed and leads to an estimate of RX J1713.7-3946's progenitor mass between 12 and 16M. The X-ray bright central point source 1WGA J1713.4-3949 detected at the center of SNR RX J1713.7-3946 shows spectral properties very similar to those of the Compact Central Objects found in SNRs and consistent in terms of absorption with that of the central diffuse X-ray emission arising from the SNR. It is highly probable that the point source 1WGA J1713.4-3949 is the compact relic of RX J1713.7-3946's supernova progenitor.

Abstract Copyright:

Journal keyword(s): acceleration of particles - radiation mechanisms: non-thermal - ISM: supernova remnants - ISM: individual objects: G347.3-0.5 (RX J1713.7-3946) - X-rays: ISM - stars: individual: 1WGA J1713.4-3949

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 NAME Vela Jr SN SNR 08 52.0 -46 20           ~ 466 2
2 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1315 1
3 GAL 347.6+00.2 HII 17 11 33.8 -39 08 20           ~ 21 0
4 SNR G347.3-00.5 SNR 17 12 27 -39 41.2     12.27     ~ 710 1
5 PSR J1713-3945 Psr 17 13 02.4438883512 -38 44 29.816068236           ~ 19 0
6 RX J1713.4-3949 X 17 13 28 -39 49.8           ~ 42 0
7 SN 393 SN* 17 14 -39.8           ~ 45 1

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