paper

ROSAT HRI and ASCA Observations of the Spiral Galaxy NGC 6946 and Its Northeast Complex of Luminous SNRs

arXiv:astro-ph/0004365 · doi:10.1086/301498

Abstract

Analysis of 80 ksec ASCA and 60 ksec ROSAT HRI observations of the face-on spiral galaxy NGC 6946 are presented. The ASCA image is the first observation of this galaxy above ~2 keV. Diffuse emission may be present in the inner ~4' extending to energies above ~2-3 keV. In the HRI data, fourteen point-like sources are detected, the brightest two being a source very close to the nucleus and a source to the northeast that corresponds to a luminous complex of interacting supernova remnants (SNRs). We detect a point source that lies \~30 west of the SNR complex but with a luminosity ~1/15 of it. None of the point sources shows evidence of strong variability; weak variability would escape our detection. The ASCA spectrum of the SNR complex shows evidence for an emission line at \~0.9 keV which could be either Ne IX at ~0.915 keV or a blend of ion stages of Fe L-shell emission if the continuum is fit with a power law. However, a two component, Raymond-Smith thermal spectrum with no lines gives an equally valid continuum fit and may be more physically plausible given the observed spectrum below 3 keV. Adopting this latter model, we derive a density for the SNR complex of 10-35 cm^{-3}, consistent with estimates inferred from optical emission line ratios. The complex's extraordinary X-ray luminosity may be related more to the high density of the surrounding medium than to a small but intense interaction region where two of the complex's SNRs are apparently colliding.

17 pages, 9 figures; LaTeX version 5 to be published in Astron. J., scheduled for August

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