Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-30T23:24:19.751Z Has data issue: false hasContentIssue false
  • English
  • Français

Do the OH/IR stars within 100 pc of the Galactic Center belong to the disk population?

Published online by Cambridge University Press:  07 August 2017

A.E. Whitford
A.E. Whitford*
Affiliation:
Lick Observatory, University of California Santa Cruz, California 95064 USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The 135 OH/IR stars within 0.8 deg (∼ 100 pc) of the Galactic Center (GC) identified in a search with the VLA (Lindqvist et al. 1991) are in rapid rotation about the center with a regression line showing a velocity gradient of 1.2±0.1 km s−1, equivalent to 178 km s—1 deg−1 for Ro = 8.5 kpc (Lindqvist et al. 1992). This is of the same order as the inward extrapolation of the Galactic rotation curve derived from the terminal velocities of HI for l < 2 deg (Burton and Gordon 1978) and the general trend of the velocities of the CO clouds in the equatorial disk mapped by Dame et al. (1987) (Fig. 1b). These OH/IR stars are located along the ridge of highest projected CO density. This spatial location and the flat configuration argue for assignment to the disk population, a possibility suggested by Feast (1989). The VLA objects are not in general supergiants (Blommaert et al. 1992). On a K-band map of an area 1×2 deg around the GC, Catchpole et al. (1990) found a number of stars brighter than (mK)o = 5. On the assumption that BCK = 3.3, (Frogel and Whitford 1987), and Ro = 8.5 kpc, Mbol < — 6.3, i.e., in the supergiant range.

Type
Contributed Papers
Information
Symposium - International Astronomical Union , Volume 153: Galactic Bulges , 1993 , pp. 339 - 340
Copyright
Copyright © Kluwer 1993 

References

Blommaert, J.A.D.L., van Langenvelde, H.J., Habing, H. J., van der Veen, W.E.C.J., and Epchtein, N. 1992, Feast Symposium, preprint.Google Scholar
Burton, W. B., and Gordon, M. A. 1978, A&A, 63, 7.Google Scholar
Carney, B.W., Latham, D.W., and Laird, J.B. 1990, in Bulges of Galaxies, Jarvis, B. and Terndrup, D., eds. (Garching: ESO), p. 127.Google Scholar
Catchpole, R.M., Whitelock, P.A., and Glass, I.S., 1990, MNRAS, 247, 479.Google Scholar
Dame, T. M., Ungerechts, H., Cohen, R. S., de Geus, E. J., Grenier, I. A., May, J., Murphy, D. C., Nyman, L.-A., and Thaddeus, P. 1987, ApJ, 322, 706.Google Scholar
Feast, M. W. 1989, in The Gravitational Forces Perpendicular to the Galactic Plane, Davis, A. G., and Lu, P. K. eds. (Schenectady: L. Davis Press), p. 210.Google Scholar
Frogel, J. A., and Whitford, A.E., 1987, ApJ, 320, 199.CrossRefGoogle Scholar
Kormendy, J., and Illingworth, G. 1982, ApJ, 256, 460.Google Scholar
Lewis, J. R., and Freeman, K. C. 1989, AJ, 97, 139.Google Scholar
te Lintel Hekkert, P., Caswell, J. L., Habing, H. J., Haynes, R. F. and Norris, R. F. 1991, A&AS, 90, 327.Google Scholar
Lindqvist, M., Winnberg, A., Habing, H. J., and Matthews, H. E. 1992, A&AS, 92, 43.Google Scholar
Lindqvist, M., Habing, H. J., and Winnberg, A. 1992, A&A, 259, 118.Google Scholar
Menzies, J. W. 1990, in Bulges of Galaxies, Jarvis, B. and Terndrup, D., eds. (Garching: ESO), p. 115.Google Scholar
Minitti, D., White, S. D.M., Olzewski, E. W., and Hill, J. M. 1992, ApJ Lett., 393, L47.CrossRefGoogle Scholar
van der Veen, W.E.C.J., and Habing, H.J. 1990, A&A, 231, 404.Google Scholar
Wielen, R., Dettbarn, C., Fuchs, B. Jahreiss, H., and Radons, G. 1992, in The Stellar Populations of Galaxies, Barbuy, B. and Renzini, A., eds., (Dordrecht: Kluwer), p. 81 CrossRefGoogle Scholar