Color and metallicity gradients in E and S0 galaxies

Details Color and metallicity gradients in E and S0 galaxies Color and metallicity gradients in E and S0 galaxies

Mar 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...204..684s&link_type=abstract

Astrophysical Journal, vol. 204, Mar. 15, 1976, pt. 1, p. 684-693.

Astronomy and Astrophysics

Astrophysics

78

Astronomical Photometry, Galactic Evolution, Giant Stars, Light Curve, Metallic Stars, Ubv Spectra, Broadband, Elliptical Galaxies, Galactic Mass, Galactic Nuclei, Globular Clusters, K Stars, M Stars, Main Sequence Stars, Spiral Galaxies, Star Distribution

Scientific paper

Plots of (U-B), (B-V), and (V-K) color indices against distance along both the major and minor axes are presented for the galaxies NGC 3115 (S0), NGC 3377 (E5), NGC 3379 (E0), and NGC 4762 (S0). Advantages of using the wide-band (V-K) color index as a measure of metallicity are noted along with some characteristics of the galaxies studied. It is found that the galaxies generally become bluer in all three color indices as distance from the nucleus increases and that the color gradients for the flattened systems are steeper along the minor axes. A population synthesis based on two crude galaxy models is performed to calibrate the (V-K) colors in terms of metallicity. The results are shown to suggest that the (V-K) light from the four galaxies is dominated by contributions from M and K giants and that the color changes seem to depend on the metal-to-hydrogen ratio. The derived metallicity gradients are compared with those predicted from theoretical models, and very good agreement is obtained outside the nuclear regions. It is concluded that M/L ratios in excess of 50 are ruled out if late M dwarfs are the major low-luminosity component of the galactic mass.

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