The Iron K-beta/K-alpha Line Ratios as Observed in Clusters and in the Laboratory
Abstract
One persistent difficulty in fitting the x-ray spectra of several clusters of galaxies, is that the ratio of the Fe K-beta to the K-alpha complexes is greater than can be explained by simple models (Akimoto et al., 1997; Molendi et al., 1998). While various suggestions have been made to explain this discrepancy (including confusion with Ni K-alpha, and self-absorption of K-alpha in the sources), consensus has not been reached as to the explanation. We will discuss recent laboratory measurements of the Fe K-line complexes (see abstracts by Gendreau, Beiersdorfer, and Brown, and other co-authors at this meeting for descriptions of the measurement system) and their implications to the modeling of x-ray emission from astrophysical sources. Work by the UC-LLNL was performed under the auspices of DOE under contract W-7405-ENG-48 and supported by NASA Space Astrophysics Research and Analysis grants to LLNL, GSFC, and Columbia University.
- Publication:
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AAS/High Energy Astrophysics Division #5
- Pub Date:
- October 2000
- Bibcode:
- 2000HEAD....5.1309S