Chandra ACIS Survey of M33 (ChASeM33): X-ray Imaging and Spectroscopy of M33SNR21, the Brightest X-ray Supernova Remnant in M33

Details Chandra ACIS Survey of M33 (ChASeM33): X-ray Imaging and Spectroscopy of M33SNR21, the Brightest X-ray Supernova Remnant in M33 Chandra ACIS Survey of M33 (ChASeM33): X-ray Imaging and Spectroscopy of M33SNR21, the Brightest X-ray Supernova Remnant in M33

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.8704g&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #87.04; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

We present and interpret new X-ray data for M33SNR21, the brightest X-ray supernova remnant (SNR) in M33, obtained as part of the ChASeM33 project. M33SNR21 (SNR #21 in Gordon et al. 1998, ApJS 117, 89) is an optical SNR which was confirmed by nonthermal radio emission and X-ray (ROSAT) emission. It is seen in projection against (and is probably interacting with) the giant HII region NGC592. We have obtained 200 ks of high resolution X-ray imagery resolving the SNR into a slightly elliptical shell 5 arcsec (20 pc) in diameter. The eastern rim is nearly five times brighter than the western rim, which suggests the SNR is interacting with a large scale density gradient, consistent with its position in a complex environment. We fitted an elliptical shell model to determine accurately the SNR dimensions and also the X-ray center. The high spatial resolution data from near on-axis pointings, plus additional lower resolution data from pointings where the source is farther off-axis, together provide 10000 X-ray counts. An absorbed Xspec sedov model fit to spectra extracted from these data imply a shock temperature kT = 0.46 keV, an ionization timescale of 2e12 cm^-3 s, and an SNR age of 5000-10000 yr. The SNR X-ray luminosity (0.245-4.0 keV) is 1.2e37 erg/s (absorbed), compared to 1.1e36 erg/s (0.1-4.0 keV) for the Cygnus Loop (Ku et al. 1984, ApJ 278, 615) and 6.3e36 erg/s (0.5-5.0 keV) for the Large Magellanic Cloud remnant N49 (Hughes et al. 1998, ApJ 505, 732). A search for harder emission results in an upper limit of 1.2e35 erg/s for any central compact source or plerion.
This work was supported by NASA Chandra award number
G06-7073A and by NASA contract NAS8-03060.

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