The Shape of the Bulge from Iras Miras
The number distribution of Miras in the Bulge as a function of distance modulus indicates that the half of the Bulge which is at positive galactic longitude is closer to us than the other half. The observed stellar distribution can be modelled with a triaxial ellipsoidal distribution of stars which we refer to as a ‘bar’ which is tilted at roughly 45° to the line of sight. Furthermore this bar is rotating in a manner consistent with expectations from the kinematics of the galactic centre gas.
KeywordsGlobular Cluster Scale Height Stellar Evolution Interstellar Extinction Distance Modulus
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- Blitz, L. & Spergel, D. N.: 1991. Astrophys. J., in press.Google Scholar
- de Vaucouleurs, G.: 1964. In The Galaxy and the Magellanic Clouds, IAU Sym. 20, Eds. F. J. Kerr & A. W. Rodgers, p. 195.Google Scholar
- Feast, M. W. & Whitelock, P. A.: 1990. In Bulges of Galaxies, ESO-CTIO Workshop, p. 3.Google Scholar
- IRAS Point Source Catalogue: 1985. US Government Publication Office.Google Scholar
- Matsumoto, T., Hayakawa, S., Koizumi, H., Murakami, H., Uyama, K., Yamagami, T. & Thomas, J. A.: 1982. In The Galactic Centre, Eds. G. R. Riegler & R. D. Blandford, p. 48.Google Scholar
- Menzies, J. W.: 1990. In Bulges of Galaxies, ESO-CTIO Workshop, p. 115.Google Scholar
- Whitelock, P. A.: 1990. In: Confrontation of Stellar Evolution and Pulsation Theory, Eds. C. Cacciari & G. Clementini, PASP Conf. Ser. p. 365.Google Scholar