Hostname: page-component-848d4c4894-m9kch Total loading time: 0 Render date: 2024-06-08T09:34:05.584Z Has data issue: false hasContentIssue false
  • English
  • Français

The Galactic Distribution and Kinematics of OH Stars (A Preliminary Discussion)

Published online by Cambridge University Press:  25 April 2016

P.F. Bowers
P.F. Bowers*
Affiliation:
Astronomy Program, University of Maryland
Get access Rights & Permissions [Opens in a new window]

Extract

The majority of OH/IR stars have been identified as M-type Mira variables, but there are a few cases where the stars have been identified as M supergiants or late-type semi-regular variables. A large number of OH sources have also been discovered with the 1612 MHz OH characteristics of OH/IR stars but no apparent optical or infrared counterparts. In several cases the velocities of these unidentified sources (OH stars) have been outside the velocity range of the neutral hydrogen distribution, suggesting that some of these sources may represent a population with a higher velocity dispersion than Population I objects (Kerr and Bowers 1974a, b). The lack of infrared and optical counterparts may indicate that the sources are quite distant, since identified OH/IR stars are often bright infrared objects. A large-scale 1612 MHz sky survey has therefore been initiated to study the galactic distribution and kinematics of the OH stars and to investigate the possibility that they may represent an older population of stars (Bowers et al. 1974).

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 2 , Issue 6 , October 1975 , pp. 362 - 363
Copyright
Copyright © Astronomical Society of Australia 1975

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Altenhoff, W.J., Downes, D., Goad, L., Maxwell, A., and Rinehart, K., Astron. Astrophys. Suppl. Ser., 1, 319 (1970).Google Scholar
Bowers, P.F., Simonson, S.C., and Kerr, F.J., Bull. Am. Astron. Soc., 6, 426 (1974).Google Scholar
Caswell, J.L., and Haynes, R.F., Mon. Not. R. Astron. Soc, (in press) (1975).Google Scholar
Kerr, F.J., Aust. J. Phys. Astrophys. Suppl., No. 9, 1 (1969).Google Scholar
Kerr, F.J., and Bowers, P.F., in ‘Galactic Radio Astronomy’ (IAU Symp. No.60) (Eds. Kerr, F. J. and Simonson, S. C. III) p.459 D. Reidel, Dordrecht, Holland (1974a).Google Scholar
Kerr, F.J., and Bowers, P.F., Astron. Astrophys., 36, 225 (1974b).Google Scholar
Mezger, P.G., Wilson, T.L., Gardner, F.F., and Milne, D.K., Astron. Astrophys., 4, 96 (1970).Google Scholar
Winnberg, A., Goss, W.M., Höglund, B., and Johansson, L.E.B., Astrophys. Lett., 13, 125 (1973).Google Scholar