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Observations of interstellar Lyman-α with the Orbiting Astronomical Observatory

Published online by Cambridge University Press:  14 August 2015

B. D. Savage  and
A. D. Code
B. D. Savage
Affiliation:
Space Astronomy Laboratory, Washburn Observatory, University of Wisconsin, Madison, Wis., U.S.A.
A. D. Code
Affiliation:
Space Astronomy Laboratory, Washburn Observatory, University of Wisconsin, Madison, Wis., U.S.A.

Abstract

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The equivalent width of the blended line at Lyman α is given for 48 stars measured with the OAO-A2 scanning spectrometer. This provides an upper limit to the neutral hydrogen column density. In the Orion association these upper limits are significantly lower than the column densities determined from 21-cm emission line measurements. The determination of the Lyman α equivalent width for θ Ori by Carruthers is rediscussed and agreement between 21-cm absorption measures and Lyman α absorption is obtained for a spin temperature in the range of 40–70 K. It is suggested that the most likely explanation for the discrepancies found for the other Orion stars is that the 21-cm emission primarily occurs beyond the Belt stars.

The correlation between the OAO blended equivalent widths and color excess, 4430 Å absorption, and interstellar sodium absorption are examined. Excellent correlation between sodium and hydrogen column densities is found.

Type
Part III: Interstellar Absorption and Emission
Information
Symposium - International Astronomical Union , Volume 36: Ultraviolet Stellar Spectra and Related Ground-Based Observations , 1970 , pp. 302 - 314
Copyright
Copyright © Reidel 1970 

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