Population structure of the Large Magellanic Cloud bar

Journal Article · Thu Mar 15 04:00:00 EST 1984 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/161826· OSTI ID:7010126

Hardy, E; Buonanno, R; Corsi, C E; Janes, K A; Schommer, R A

We have used a combination of profile-deconvolution and automatized techniques of photographic photometry in crowded fields 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 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.

• Research Organization: Departement de physique and Observatoire du Mont Megantic, Universite Laval
• OSTI ID: 7010126
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 278:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
DATA ANALYSIS
GALAXIES
GIANT STARS
LUMINOSITY
MAGELLANIC CLOUDS
MAIN SEQUENCE STARS
MORPHOLOGY
OPTICAL PROPERTIES
PHOTOMETRY
PHYSICAL PROPERTIES
RED GIANT STARS
STAR ACCRETION
STAR EVOLUTION
STARS