paper

Chandra Spatially Resolved Spectroscopic Study and Multi-Wavelength Imaging of the Supernova Remnant 3C 397 (G41.1-0.3)

arXiv:astro-ph/0407121 · doi:10.1086/425960

Abstract

(Abridged) We present a Chandra observation of the supernova remnant (SNR) 3C 397 (G41.1-0.3) obtained with ACIS-S. Previous studies of this SNR have shown that it harbors a central X-ray `hot spot' suggestive of a compact object associated with 3C 397. With the Chandra data, we can rule out the nature of the hot spot as a pulsar or a pulsar wind nebula, and put an upper limit on the flux of a hidden compact object of F (0.5--10 keV)~6E-13 erg/cm2/s. We found two point sources in the Chandra field. We argue that none of them is associated with 3C 397; and that the hard source, CXO J190741.2+070650, is a newly discovered AGN. The Chandra image reveals arcseconds-scale clumps and knots which are strongly correlated with the radio VLA image, except for the X-ray hot spot. Our Chandra spatially resolved spectroscopic study shows that one-component models are inadequate, and that at least two non-equilibrium ionization thermal components are needed to fit the spectra of each selected region. The derived average spectral parameters are consistent with the previous global ASCA fits performed by Safi-Harb et al. (2000). However, the hard component requires a high abundance of Fe indicating the presence of hot Fe ejecta. When comparing the eastern with the western lobe, we find that the column density, the brightness, and the ionization timescales are generally higher for the western side. This result, combined with our study of the 3C397 environs at millimeter wavelengths, indicate a denser medium to the west of the SNR. Our multi-wavelength imaging and spectral study favors the scenario where 3C 397 is a ~5,300-year old SNR expanding in a medium with a marked density gradient, and which is likely to be encountering a molecular cloud on the western side. We propose that 3C 397 will evolve into a mixed-morphology SNR.

43 pages (including 19 figures & 6 tables; the resolution of most figures has been reduced for astro-ph submission only). The tex uses the aastex.cls style file. Minor revisions (mainly formal) following the referee's report. Accepted 14 Sep 2004 for publication in ApJ. A gzipped postscript version of the paper with high-resolution images can be downloaded from: (http://aurora.physics.umanitoba.ca/~samar/ms-ssh-apj.ps.gz). Astrophysical Journal, in press. Scheduled fcr the 1 Jan. 2005 issue

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