Further Investigation of

Details Further Investigation of Further Investigation of

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...20510607t&link_type=abstract

American Astronomical Society Meeting 205, #106.07; Bulletin of the American Astronomical Society, Vol. 36, p.1521

Astronomy and Astrophysics

Astronomy

Scientific paper

Radioactive 44Ti (τ 1/2=60y) produced in supernovae is the source for the abundance of 44Ca in our Galaxy. It is synthesized in the deepest material to be ejected by a core-collapse supernova, and so is an excellent diagnostic of the ejections process. This isotope's decay chain (44Ti => 44Sc => 44Ca) produces both gamma- and x-ray lines, including the prominently studied 1157 keV nuclear de-excitation of 44Ca. Our methods utilize the Sc K-shell photon emission from the 44Ti electron capture decay. At current resolution capabilities in x-ray satelite observations, this emission should fall within the limits of observation for young, nearby core-collapse supernovae.
Our target for investigating 44Ti production and decay via this line is SNR Casseiopeia A. Our ongoing analysis of both existing Chandra and XMM observations has established a 2σ upper limit for the 4.1 keV line flux of ≈3.0*10-5 γ /cm2s. Further, we have extended our search to a smaller regional analysis within the iron-rich regions of CasA and will report on those results as well.

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