ROSAT and BBXRT observations of IC443

Details ROSAT and BBXRT observations of IC443 ROSAT and BBXRT observations of IC443

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.5604r&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #56.04; Bulletin of the American Astronomical Society, Vol. 24, p.1213

Astronomy and Astrophysics

Astronomy

Scientific paper

We report the results of a preliminary analysis of ROSAT HRI and PSPC, and BBXRT (Broad Band X-ray Telescope) observations of the supernova remnant IC 443. The HRI and BBXRT were targeted at the northeastern corner of IC 443 where the X-rays are brightest and the interaction between the shock front and a large molecular cloud is occurring. The HRI detected 4.1cts/sec over 8,000 sec observation, with 5(') (') resolution. The X-ray gas shows sharp structure (17(') (') thickness filaments along the shock front) where the shock front is interacting with the molecular clouds. The X-ray filaments are produced by shock-heated gas cooling rapidly due to the molecular cloud. IR emission and excited molecular gas are also known to be correlated with the interaction. Three images (NE, NW and S) were taken using ROSAT PSPC and mosaiced showing a complete X-ray image of IC 443. The variation of temperature and column density over the remnant will be presented region by region using the PSPC and Einstein IPC spectra. The BBXRT provides coverage of the 0.5-10 keV band, with sufficient spectral resolution (160 eV at 6 keV) to resolve line emission due to Ne, Mg, Si, and S. Assuming a two-temperature model (Petre, 1988, Ap. J., 335, 215), the temperatures are 0.3keV and 1.2keV. An inward progression of ionization is observed: from Ne IX and Ne X (around 1keV) which are strongest at the shell, to Mg XI (1.35keV) strongest in the interior, and Si XIII (1.8keV) strongest still further in. A non-equilibrium model will be used to test how the ionization states are different with increasing distance behind the shell.

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