Disentangling age and metallicity effects in the blueish nuclear population of M33, NGC 278 and NGC 404

Details Disentangling age and metallicity effects in the blueish nuclear population of M33, NGC 278 and NGC 404 Disentangling age and metallicity effects in the blueish nuclear population of M33, NGC 278 and NGC 404

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.243..620s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 243, April 15, 1990, p. 620-628. Research supported by

Astronomy and Astrophysics

Astronomy

46

Active Galactic Nuclei, Metallic Stars, Spiral Galaxies, Star Clusters, Stellar Spectra, Astronomical Catalogs, Globular Clusters, Ubv Spectra

Scientific paper

In this study, the authors have applied to the blueish nuclei of the spiral galaxies M33 and NGC 278 and to the dwarf lenticular NGC 404, a population synthesis method relying upon a base of star clusters, over the range 3700-9700 A. The near-infrared spectrum of the nucleus in M33 is very different from that of a metal poor globular cluster. The synthesis indicates that the early type spectrum in the blue arises from young components and that the old, very metal-poor contributions at Z/Z(solar) = -1.5 or less are negligible in this object. The old component with metallicity Z/Z(solar) between -1.0 and -0.5, as well as the intermediate age component, are important. The metallicity of the stellar population in the nucleus, at most, has reached up to the solar value. The nucleus in NGC 278 is dominated by young components, at 500 million yr. The emission-line spectrum suggests that the star formation process is still operating. As for M33, the maximum metallicity in the nucleus is, at most, solar. In NGC 404 the old population with Z/Z(solar) roughly -0.5 is dominant in the nucleus. The young component is weaker than in M33 and in NGC 278.

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