A broadband X-ray study of the young SNR 3C397

Details A broadband X-ray study of the young SNR 3C397 A broadband X-ray study of the young SNR 3C397

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999head....4.3506s&link_type=abstract

American Astronomical Society, HEAD meeting #4, #35.06; Bulletin of the American Astronomical Society, Vol. 31, p.738

Astronomy and Astrophysics

Astronomy

Scientific paper

3C397 (G41.1-0.3) is one of the brightest radio SNR's, whose classification as a `mixed-morphology' Composite-type SNR is highly uncertain. We present a broadband imaging and spectral study of 3C397 with ROSAT, ASCA, & RXTE. We show that the X-ray emission from the center is dominated by soft emission (E below 4 keV), and that unlike the Plerionic Composites, the hard X-ray emission arises primarily from the shell-like component. A broadband spectral study of the X-ray emission in the 0.6-15 keV range shows that at least two components are required: a soft component dominated by line emission from heavily enriched material, and a harder component, characterized by a prominent Fe-K emission line. While equilibrium models fail to describe the soft component, non-equilibrium ionization (NEI) models fit the data adequately, implying that 3C397 is a young SNR. The harder component can be fitted with either a thermal model, or a power law plus a Gaussian line to account for the Fe-K emission line. The total observed flux is ~ 2.6 x 10(-11) erg cm(-2) s(-1) , which corresponds to an unabsorbed luminosity L_x (1-9 keV) = 4 x 10(36) erg s(-1) , assuming a distance of 10 kpc. The combined ASCA & RXTE PCA data in the 0.6-15 keV range suggest the presence of a weak third component, whose parameters are poorly determined because of the contamination of the RXTE signal with the emission from the Galactic ridge. We discuss the X-ray spectrum in the light of thermal emission from an ejecta-dominated component, associated with the SN explosion of a massive star. The harder component is consistent with thermal emission from the ISM shock-heated by the blast wave of an ~ 2,000-yr old SN explosion. However, it is possible that part of this emission is non-thermal. We speculate on the possibility that a compact object is hidden in 3C397, and draw similarities to the Composite-type SNR W50 powered by the jet source, SS433.

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