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Fe VIII, IX, and X Line Emission From the Soft X-ray Background: Previous Limits and a Future Measurement

Published online by Cambridge University Press:  12 April 2016

J. J. Bloch ,
W. C. Priedhorsky  and
Barham W. Smith
J. J. Bloch
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM, USA
W. C. Priedhorsky
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM, USA
Barham W. Smith
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM, USA

Abstract

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We discuss pulse height analysis of Be band data in relation to the important 72 eV Fe line cluster emission from the soft X-ray background (SXRB). Pulse height fits to the Be band data suggest that the Fe lines must be suppressed by a factor of ~10 with respect to the rest of the X-ray spectrum. The broad band rates and the mean energy of the pulse height data for the Be band can be brought into agreement by using depleted elemental abundance emission models. A planned measurement of the SXRB Fe lines using the Array of Low Energy X-ray Imaging Sensors (ALEXIS) experiment could resolve this issue.

Type
4. Supernova Remnants, Soft X-ray Background
Information
International Astronomical Union Colloquium , Volume 115: High Resolution X-ray Spectroscopy of Cosmic Plasmas , 1990 , pp. 160 - 163
Copyright
Copyright © Cambridge University Press 1990

References

Bloch, J. J., Jahoda, K., Juda, M., McCammon, D., Sanders, W. T., and Snowden, S. L. 1986, Ap. J. (Utters), 308, L59.CrossRefGoogle Scholar
Bloch, J. J. 1988, Ph. D. thesis, University of Wisconsin-Madison.Google Scholar
Juda, M. 1988, Ph. D. thesis, University of Wisconsin-Madison.Google Scholar
Marshall, F. J., and Clark, G. W. 1984, Ap. J., 287, 633.CrossRefGoogle Scholar
McCammon, D., Burrows, D. N., Sanders, W. T., and Kraushaar, W. L. 1983, Ap.J., 269, 107.CrossRefGoogle Scholar
Priedhorsky, W.C., Bloch, J. J., Smith, B W., Strobel, K., Ulibarri, M., Chavez, J., Evans, E., Siegmund, O. H. W., Marshall, H., Vallerga, J., and Vedder, P., X-ray Instrumentation in Astronomy, SPIE Proceedings, 982, 1988.Google Scholar
Raymond, J. C., and Smith, B. W. 1977, Ap. J. Suppl., 35, 419.CrossRefGoogle Scholar
Raymond, J. C., and Smith, B. W. 1987, private communication (update to Raymond and Smith 1977).Google Scholar