Computer Science – Numerical Analysis
Scientific paper
Nov 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...298..528f&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 298, Nov. 15, 1985, p. 528-543.
Computer Science
Numerical Analysis
89
Astronomical Photometry, Galactic Nuclei, Galactic Structure, Spiral Galaxies, Star Distribution, Elliptical Galaxies, Metallicity, Numerical Analysis, Stellar Evolution, Stellar Systems
Scientific paper
Optical and infrared photometry for nineteen late-type spiral galaxies were used to estimate stellar content in the galactic nuclei. Numerical analysis of the UBVJHK colors and CO and H2O indices showed no correlation between the stellar content of the UBV galaxies and the JHK galaxies. Blue stars from the young stellar systems such as the Magellanic cloud clusters of SWB type I-III (less than about 100 Myr) were found to contribute significantly to the optical light of many of the Sc nuclei in the sample. The infrared light was dominated by an older and probably metal-rich stellar population such as in the Magellanic cloud clusters of the SWB type-IV-VI (a few Gyr) and/or elliptical galaxies. The U-V and V-K colors of the Sc nuclei appeared to be much redder than the nuclei of regions farther out. The gradients are attributed to the radial dependence of internal reddening and the relative number of different types of stars. The optical and infrared photometry of the clusters are given in a table.
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