Infrared Spectra of Low-Temperature Stars
- Creators
- McCammon, D.
- Münch, G.
- Neugebauer, G.
Abstract
Spectra of stars of types M, N(R), and S, as well as of NML objects in Cygnus and Taurus, are presented in the regions ⋋⋋l 5-1.8 μ and ⋋⋋l 9-2 5 μ. In M stars the absorption due to stellar H_2O is apparent from the wings of the bands at ⋋l.4, ⋋l.9, and ⋋2.7 μ Stars of N and S types show weaker H_2O absorption. The Δv = 2 and Δv = 3 vibration-rotation band sequences of CO appear well marked in all stars, being somewhat weaker in the M types than in other stars. The late N stars Y CVn and U Hyd show a sharp discontinuity or band head at ⋋l.76 μ not present in other stars. The entire spectra of Y CVn and U Hyd shortward of this discontinuity appears veiled, the Δv = 3 CO band sequence being conspicuously weak. The spectra of the NML objects in Cygnus and Taurus have spectral characteristics resembling the carbon more than the M stars.
Additional Information
© 1967 American Astronomical Society. The spectrometer has been loaned to us by the Space Sciences Division of the Jet Propulsion Laboratory. We thank all the members of the California Institute of Technology infrared astronomy group, but especially E. Becklin and C. Spencer, for their efforts supporting this work. We are indebted to Dr. Aert Schadee for calculating the absorption coefficient of the rotation-vibration bands of CO and to M. Katz for her help in reducing the data. We thank Dr. William S. Benedict for a helpful discussion.Attached Files
Published - 1967ApJ___147__575M.pdf
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Additional details
- Eprint ID
- 74588
- Resolver ID
- CaltechAUTHORS:20170228-101154975
- Created
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2017-02-28Created from EPrint's datestamp field
- Updated
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2021-11-11Created from EPrint's last_modified field