Andrew Fabian, Institute of Astronomy, Cambridge
Marshall Bautz, Massachusetts Institute of Technology
Yuzuru Tawara, Nagoya University
We have analyzed spatially-resolved X-ray spectra of the cores of cooling flow clusters, observed during the PV phase of ASCA mission. The spectral resolution of the SIS and the moderate spatial resolution of the X-ray telescopes of ASCA enable us to unambiguously identify low temperature emission lines in the spectra of the cores of several clusters. However, simple model fits to these spectra do not require spectral components with temperatures below ~1 keV. Stated another way, we see no evidence for Fe XVII emission lines in our spectra. We suggest that the 0.5 - 1 keV spectra of cooling flows are complicated mixtures of emission and absorption components, which are not resolved by the SIS. Along the way we demonstrate a problem with the plasma emission codes and show that silicon is overabundant in the core of the Perseus cluster.