The population structure of the large Magellanic Cloud bar

Details The population structure of the large Magellanic Cloud bar The population structure of the large Magellanic Cloud bar

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...278..592h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 278, March 15, 1984, p. 592-603. Research supported by the Natural Sciences

Astronomy and Astrophysics

Astrophysics

72

Barred Galaxies, Galactic Structure, Magellanic Clouds, Stellar Evolution, Color-Magnitude Diagram, Main Sequence Stars, Red Giant Stars, Stellar Color, Stellar Magnitude

Scientific paper

A combination of profile-deconvolution and automatized techniques of photographic photometry in crowded fields is used to construct a rich and deep color-magnitude diagram near the NW end of the Large Magellanic Cloud (LMC) bar. The morphology of the diagram and its analysis through the use of luminosity functions and evolutionary models for the core-helium-burning 'clump' red giants indicate that (1) stellar formation continues in the bar areas; (2) an old Population II in the Galaxy sense is not a significant contributor to the observed diagram, although stars of all ages are probably present in the LMC disk; (3) the bulk of star formation, which continues to date, started earlier than about one billion years ago but later than about three billion years ago, although the precise rate of star formation, including the possible presence of bursts, inside such an age range is not known from our data. The observed population is considerably younger and more metal deficient than that of the solar neighborhood.

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