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Observations of Highly-Ionized Interstellar Iron

Published online by Cambridge University Press:  12 April 2016

L.M. Hobbs
L.M. Hobbs*
Affiliation:
Yerkes Observatory, University of Chicago

Abstract

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The spectra of 24 stars, including 5 at distances d < 200 pc, have been observed in the regions of the coronal [Fe X] λ6375 and [Fe XIV] λ5303 lines at detection limits near an equivalent width of 1 mÅ in the best cases. In general agreement with predictions based on a multi-phase model of the interstellar medium, no absorption which can be attributed to Fe X or Fe XIV ions in hot interstellar gas emitting the soft x-ray background is seen in any of these spectra, except for two. Toward λ Cephei an absorption line near λ6375 is measured with an equivalent width of 8.1 ± 2 mÅ, a width corresponding to 20 ± 5 km s-1 or a temperature T ≤ (0.5 ± 0.25) x 106 °K, and, if it is caused by Fe X ions, a radial velocity of -355 km s-1. On that hypothesis, the hot interstellar gas constitutes at least 63% of the column density of gas along this light path.

Type
Hot Gas in the LISM: Optical, UV, and EUV Wavelengths
Information
International Astronomical Union Colloquium , Volume 81: Local Interstellar Medium , 1984 , pp. 189 - 191
Copyright
Copyright © NASA 1984

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