Abstract
Based on the observations of M giant stars in the north galactic polar objective-prism survey of Upgren (1960) and the data summarized by Blanco (1965) the overall space density of all M-type giants as a function of distance from the galactic plane at the position of the sun can be approximated by,
where z is in kpc and ρ(z) is the number of stars per 106pc3. This relationship is derived from the observed fall-off in space densities up to a distance of about 2 kpc.
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References
Blanco, V.M.: 1965, Stars and Stellar Systems, 5, 241.
Kinman, T.D., Wirtanen, C.A. and Janes, K.A.: 1966, Ap. J. Supp. 13, 379
Luyten, W.J.: 1968, Monthly Notices Roy. Astron. Soc. 139, 221.
Luyten, W.J.: 1976, Proper Motion Survey with the 48-Inch Schmidt Telescope XLVI, Univ. of Minnesota Press, Minneapolis.
Sanduleak, N.: 1965, “The Luminosity Function of the M Dwarf Stars”, Case Institute of Technology, Cleveland (Ph.D. Thesis).
Sanduleak, N.: 1976, Astron. J. 81, 350.
Upgren, A.R.: 1960, Astron. J. 65, 644.
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Sanduleak, N. (1977). The Frequency of Faint M Giant Stars at High Galactic Latitudes. In: Müller, E.A. (eds) Highlights of Astronomy. International Astronomical Union / Union Astronomique Internationale, vol 4-2. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-1250-8_10
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DOI: https://doi.org/10.1007/978-94-010-1250-8_10
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