M Giant Populations and Galactic Structure

Details M Giant Populations and Galactic Structure M Giant Populations and Galactic Structure

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.247..227f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 247, NO.2/NOV15, P. 227, 1990

Astronomy and Astrophysics

Astronomy

53

Scientific paper

JHKL photometry is given for 63 local M giants, for 195 M-giants outside the galactic plane and for 34 M-giants which are known semi-regular variables. Using the (J-H)0-(H-K)0 diagram a comparison is made with recently published models and with the M-giant population in the NGC 6522 Baade window of the Galactic Bulge. The metallicities ([Z/Zsun]) of local M-giants have a root-mean-square (rms) scatter of less than 0.08. If the difference between the Frogel-Whifford bulge sample and the local M giants is due entirely to a metallicity difference, then this is estimated as Δ[Z/Zsun]˜+0.2. There is some evidence for a range of metallicities amongst M giants in the NGC 6522 field. The Frogel-Whitford sample will be biased towards the higher metallicity side of such a spread. Our results show that there are M giants in the extended solar neighbourhood at distances of about 500 pc or more from the galactic plane which lie in the same region of the (J-H)0-(H-K)0 Diagram as the M giants in the NGC 6522 field. This indicates that these stars have similar metallicities to the bulge M giants. Such stars lying out of the galactic plane probably belong to a thick disc or inner halo population and the metal-rich component of the Galactic Bulge can therefore be regarded as the central concentration of this population. The present work gives reasons for supposing the progenitors of Mira variables in the Galactic Bulge and in the extended solar neighbourhood are similar.

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