Galactic bulge M giants. IV - 0.5-2.5 micron spectrophotometry and abundances for stars in Baade's Window

Details Galactic bulge M giants. IV - 0.5-2.5 micron spectrophotometry and abundances for stars in Baade's Window Galactic bulge M giants. IV - 0.5-2.5 micron spectrophotometry and abundances for stars in Baade's Window

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...378..742t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 378, Sept. 10, 1991, p. 742-755.

Astronomy and Astrophysics

Astrophysics

65

Abundance, Galactic Bulge, Giant Stars, Late Stars, M Stars, Opacity, Stellar Spectrophotometry, Absorption Spectra, Carbon Monoxide, Color-Magnitude Diagram, Infrared Photometry, Infrared Spectroscopy, Line Spectra, Water

Scientific paper

Spectrophotometric observations of bulge and local M giants from 0.45 to 2.5 microns at a resolution of about 1000 are presented. From an analysis of strong atomic lines of Na I and Ca I in the K band, a mean metallicity of the M giants in Baade's Window is derived. It is demonstrated that J-K is a good temperature indicator for both the field and bulge nonvariable M giants, and that the relationship between the two quantities is the same for both types of stars. In addition, there is no difference in the surface gravity between bulge and field giants of the same J-K color (i.e., temperature). A major difference in the overall spectral energy distributions of bulge and local M giants is that the classical H-band bump attributed to the opacity minimum of the H(-) ion near 1.6 microns is considerably reduced in many of the bulge stars.

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