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Galactic bulge M giants. III - Near-infrared spectra and implications for the stellar content of E and S0 galaxies
Spectra at 0.6-0.9 micron of 320 K and M giants in six low-absorptionfields along the minor axis of the galactic bulge and of an additional60 late-type giants and dwarfs in the solar neighborhood were obtained.Indices of the strength of molecular absorption are combined withprevious infrared and optical photometry to estimate the mean metalabundance of the bulge M giants and to constrain the relativecontribution of late giants and dwarfs to the integrated light of E andS0 galaxies.
| M giants in Baade's window - Infrared colors, luminosities, and implications for the stellar content of E and S0 galaxies
In this paper, 1-10 micron photometric observations of M giants inBaade's window are presented and interpreted. When compared to solarneighborhood M giants, it is found that: (1) bulge giants at the samespectral type have bluer JHK colors but stronger CO indices; (2) thenearly dispersionless H-H, H-K relation for the bulge giants lies on theopposite side of the mean field giant relation from that for globularcluster stars; and (3) bulge M giants are up to two magnitudes fainterthan field giants of the same spectral type, and their luminosityfunction drops precipitously for M(bol) brighter than -4.2. It is arguedthat the near-infrared energy distribution of the bulge giants isstrongly affected by molecular blanketing, particularly from H2O.Long-period variables have infrared colors and indices which give themphotometric properties distinct form all other M giants in Baade'swindow. The observed characteristics of the bulge M giants areconsistent with their being representatives of a population with ametallicity considerably in excess of solar.
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