A. E. Whitford

M giants in Baade's window: infrared colors, luminosities, and implications for the stellar content of E and S0 galaxies

On presente des observations IR JHKL, [10], CO et H 2 O de 185 geantes M1-9 dans la fenetre de Baade. Les variables de longue periode (VLP) ont des indices et des couleurs IR qui leur donnent des proprietes photometriques distinctes de toutes les autres geantes M de la fenetre de Baade. Toutes les sources IRAS de la fenetre de Baade peuvent etre identifiees avec des geantes M deja connues

Proper motions of bulge stars

Proper motions were measured for K and M giants in the bulge of the Milky Way through Baades window. The proper motions are of sufficient precision for velocity dispersions to be determined. For the entire sample, the motions appear to be very nearly isotropic, with the dispersion in one coordinate just over 100 km/s (for a distance of 7.7 kpc). There is some indication that the more metal-rich stars have a larger dispersion in galactic longitude than in galactic latitude, although this awaits confirmation with a larger sample

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

We have obtained 0.45-2.45 μm spectrophotometry with a resolution λ/Δλ∼1000 of a representative sample of M giants in Baades Window and the solar neighborhood. From an analysis of strong atomic lines of Na I and Ca I in the K band, we derive a mean metallicity of the M giants in Baades Window of =+0.3, comparable to that for the K giants. We demonstrate 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.

Galactic bulge M giants. II. Content and structure of the bulge between b = -3 deg and -12 deg

JHKL colors and CO and H2O indices for a sample of 250 M giants derived from surveys along the minor axis of the Galaxy at latitudes between -3 deg and -12 deg are presented and studied. The bolometric magnitudes for the stars are calculated. The effects of latitude on the colors, magnitudes, and indices are examined. The bolometric luminosity function for each bulge field is provided and the influence of latitude on luminosity is analyzed. Long-period variables in the bulge, the search for IRAS sources in the surveyed fields, and the IR surface brightness of the bulge are discussed. 74 refs.

Photometry of K giants in the nuclear bulge of the galaxy

On presente une photometrie RIJHK de 52 geantes K et M de premier type dans la fenetre de Baade a la latitude galactique de −3°9

THE STELLAR POPULATION OF THE GALACTIC NUCLEAR BULGE.

The stars of the Galactic bulge (GB) are characterized in a survey of observational data, and the results are applied to the evaluation of theoretical models of elliptical galaxies and spiral bulges. The data are presented graphically and discussed in detail, with consideration of population models deduced from analysis of integrated light, the metallicity distribution among the GB K giants, RR Lyr variable, M giants, color-magnitude diagrams, age and mass, and hot blue stars. The GB population is found to have a dominant super-metal-rich (SMR) component, a mildly metal-poor non-SMR component, a maximum Fe/H abundance ratio of about 1.0, and cool M giants like those responsible for the IR signatures of other galaxies, but no very hot stars like those to which the FUV excess of other galaxies is attributed. Since the GB stars are different in mass, age, and metallicity from the giant prototypes of the Local Group, the validity of integrated-light population models of external galaxies based on Local Group giant characteristics is questioned, and the need for extensive studies of the GB population with the aim of constructing new models is indicated.

Dwarf Content of Old Galaxy Populations

Scanner observations of five galaxies in the region near 9910 A showed that the strength of the dwarf-sensitive Wing-Ford band is below the level of detection. This result is at variance with the predictions of strongly dwarf-enriched population models and in accord with the evidence for giant-dominated radiation at 2.3µ reported by Baldwin et al. (1973) on the basis of the strong CO band found in three galaxies. In the absence of any evidence for a power-law mass function, the consequences of a rounded function are examined.