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Interstellar lines in stars at high galactic latitudes

Cohen, J. G. (1974) Interstellar lines in stars at high galactic latitudes. Astrophysical Journal, 194 . pp. 37-40. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20190529-161902015

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Abstract

We have measured the velocity and equivalent widths of the optical interstellar lines in a group of southern B stars at high galactic latitudes, as well as additional data for the stars previously discussed by Münch and Zirin. The main peculiarities of the interstellar matter far above the plane seem to be an increase in the ratio of the column density of Ca ii to that of Na i and, less certainly, an excess of Ca ii relative to H i. The gas-to-dust ratio indicates that some of the hydrogen at high galactic latitudes may be ionized.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1086/153219DOIArticle
http://adsabs.harvard.edu/abs/1974ApJ...194...37CADSArticle
ORCID:
AuthorORCID
Cohen, J. G.0000-0002-8039-4673
Additional Information:© American Astronomical Society • Provided by the NASA Astrophysics Data System. Received 1974 May 29; revised 1974 June 13. I am grateful to the night assistants at Cerro Tololo for assistance beyond the call of duty. I thank Dr. C. Heiles for providing detailed velocity distributions of neutral hydrogen at the positions of several of the stars. I am very grateful to Dr. C. Anderson for the loan of the Wisconsin echelle spectrograph to Kitt Peak and for instruction in its use.
Subject Keywords:galactic structure — interstellar matter
Record Number:CaltechAUTHORS:20190529-161902015
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190529-161902015
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95898
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:31 May 2019 15:23
Last Modified:03 Oct 2019 21:17

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