Guest Observer Facilities & Science Centers Select One AGILE ASCA BeppoSAX COBE CGRO Chandra EUVE Fermi (formerly GLAST) GALEX HETE-2 INTEGRAL ROSAT RXTE Suzaku Swift WMAP XMM-Newton NASA Archives Select One ADS AstroGravS EOSDIS HORIZONS IRSA LAMBDA MAST Michelson NED NSSDC NStED PDS SDAC SPDF Spitzer Science Center HEASARC Tip: View all tips NOTICE: This Legacy journal article was published in Volume 1, May 1992, and has not been updated since publication. Please use the search facility above to find regularly-updated information about this topic elsewhere on the HEASARC site. Number 1 May 1992 On the cover An analysis of the Einstein Observatory Solid State Spectrometer data from clusters of galaxies has recently been reported by White, D.A., Fabian, A.C., Johnstone, R.M., Mushotzky, R.F. & Arnaud, K.A. 1991, Mon Not R. astr. Soc, 252, 72. The new SSS ice model enabled significant excess absorption above that due to the line-of-sight through the Galaxy (from 21 cm measurements) to be detected in 12 out of 21 clusters studied. This excess absorption is most likely due to cold clouds and represents a significant new component to the intracluster medium. The cluster spectra requiring excess absorption also require significant cooling flow components, implying the absorption may originate from mass deposited through the cooling flow region of the clusters. The front cover (upper panel) shows the SSS spectrum of the central region (3 arcmin radius), of NGC 6166 in A2199. The model spectra shown by the dotted line indicate the best-fitting thermal model with Galactic absorption only and the solid line represents the best-fitting thermal and cooling flow model with additional absorption. The lower panel shows the residuals for the bremsstrahlung spectral model which best fits the A2199 above 1.57 keV, extrapolated to lower energies. Galactic absorption only has been assumed. Evidence for the excess absorption is clearly visible in the negative residuals below 1 keV, as is evidence for additional line and continuum emission from the cooling gas by the positive peak in the residual around 1 keV. Goddard Space Flight Center Proceed to the next article Return to the previous article Select another article HEASARC Home | Observatories | Archive | Calibration | Software | Tools | Students/Teachers/Public Last modified: Monday, 19-Jun-2006 11:40:52 EDT