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Observations of Diffuse Emission from the Hot ISM

Published online by Cambridge University Press:  12 April 2016

W.T. Sanders  and
R.J. Edgar
W.T. Sanders
Affiliation:
Department of Physics, University of Wisconsin-Madison, 1150 University Avenue, Madison, WI 53706, USA Space Science & Engineering Center, University of Wisconsin-Madison, 1225 W. Dayton Street, Madison, WI 53706, USA
R.J. Edgar
Affiliation:
Department of Physics, University of Wisconsin-Madison, 1150 University Avenue, Madison, WI 53706, USA Space Science & Engineering Center, University of Wisconsin-Madison, 1225 W. Dayton Street, Madison, WI 53706, USA

Abstract

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The Diffuse X-ray Spectrometer (DXS) is a Bragg-crystal spectrometer designed to obtain spectra of the diffuse x-ray background in the 83–44 Å (150–284 eV) range, with ~ 3 Å spectral resolution (10–25 eV), and ~ 15° angular resolution. It was flown successfully as an attached Shuttle payload on the STS 54 mission of NASA’s Space Shuttle Endeavour in January 1993, and spectra were obtained from the diffuse background along an arc extending roughly along the galactic plane from longitude 150° to longitude 300°. The primary conclusions so far from the analysis of the DXS data are: (1) The spectra of the diffuse background in the 83–44 Å range show emission lines or emission-line blends, indicating that the emission is thermal. Although most models of this emission have assumed that it is of thermal origin, this is the first detection of lines in the diffuse background in this wavelength range. (2) The detected spectra do not resemble the model spectra of cosmic abundance equilibrium plasmas at any temperature in the 105 – 107 K range. This is independent of the particular plasma model used, Raymond & Smith, Mewe & Kaastra, or Monsignori-Fossi & Landini. (3) The detected spectra do not resemble the model spectra of depleted abundance equilibrium plasmas at any temperature in the 105 – 107 K range, for a variety of assumed elemental depletions and the same emission models. This aspect of the analysis is not completed. (4) Tentative line identifications can be made, but other lines predicted to arise from the same ions must be of consistent strength in both the DXS and EUVE data sets.

Type
V. The Interstellar Medium and Diffuse Background
Information
International Astronomical Union Colloquium , Volume 152: Astrophysics in the Extreme Ultraviolet , 1996 , pp. 269 - 275
Copyright
Copyright © Kluwer 1996

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