Astronomy and Astrophysics – Astronomy
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21642806b&link_type=abstract
American Astronomical Society, AAS Meeting #216, #428.06; Bulletin of the American Astronomical Society, Vol. 41, p.841
Astronomy and Astrophysics
Astronomy
Scientific paper
Though SN 1604 (Kepler's Supernova Remnant) was determined to have a Type Ia progenitor, it also possesses a circumstellar medium (CSM), which is more characteristic of a Core-collapse (CC) remnant. As Type Ia supernovae are widely used as distance standards in astronomy, any opportunity to understand them better should be exploited. Using a 750 ks Chandra X-ray Observation of SN 1604, we have been working to separate the swept up CSM and ejected material. The original image was divided into segments with comparable photon statistics and then sliced into several significant broad energy bands. The segments would then form scatterplots in a multidimensional space of energy ratios. These scatterplots were analyzed using a Gaussian mixture model program, which divided all the pixels into an optimal number of clusters, each with similar spectral characteristics. By extracting the summed spectra of the clusters, their distinct characteristics can easily be seen. After experimentation, the most successful application of this process has been in four dimensions. The energy cuts that were utilized are 0.3 to 0.72 KeV (oxygen), 1.3 to 1.5 KeV (magnesium), 1.7 to 2.1 and 2.3 to 2.7 KeV (silicon and sulfur), and 0.72 to 1.3 KeV (iron), all normalized to a continuum of 1.5 to 1.7, 2.1 to 2.3, and 2.7 to 7.0 KeV. The clustering produced CSM areas that, when compared to a Spitzer infrared image, showed clear correspondence. We show that this method can successfully identify regions of contrasting spectral character such as synchrotron dominated, CSM, and ejecta regions of varying composition. We also present initial results of spectral fitting in the primary CSM regions.
Borkowski Kazik
Burkey Mary
Reynolds Stephen P.
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