The asymptotic giant branch of Magellanic Cloud clusters

• Published in: The Astrophysical journal Vol. 352; no. 1; pp. 96 - 122
• Main Authors: FROGEL, J. A, MOULD, J, BLANCO, V. M
• Format: Journal Article
• Language: English
• Published: Chicago, IL University of Chicago Press 01.03.1990
• Subjects: Astronomy; CARBON STARS; CHEMICAL COMPOSITION; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; COLOR; DIAGRAMS; Earth, ocean, space; ELECTROMAGNETIC RADIATION; Exact sciences and technology; GALAXIES; Giant and subgiant stars; GIANT STARS; HERTZSPRUNG-RUSSELL DIAGRAM; IDENTIFICATION SYSTEMS; INFRARED RADIATION; INTERSTELLAR SPACE; LUMINOSITY; MAGELLANIC CLOUDS; MAIN SEQUENCE STARS; NEAR INFRARED RADIATION; Normal stars (by class): general or individual; OPTICAL PROPERTIES; ORGANOLEPTIC PROPERTIES; PHOTOMETRY; PHYSICAL PROPERTIES; RADIATIONS; SPACE; SPECTROPHOTOMETRY; STAR CLUSTERS; STAR EVOLUTION; Stars; STARS 640102 > Astrophysics & Cosmology > Stars & Quasi-Stellar, Radio & X-Ray Sources; Data analysis; Globular cluster; Color magnitude diagram; Stellar abundance; Stellar evolution; Magellanic clouds; Metallicity; Data table; Carbon star; M star; Asymptotic giant branch; Age; Photometry; Hertzsprung Russel diagram; Late type star; Luminosity function
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/168518

The present search for carbon and M-type asymptotic giant branch (AGB) stars in the 39 clusters of the Magellanic Clouds has yielded identifications and near-IR photometry for about 400 such stars. The Searle et al. (1980) cluster-age-related classification scheme is a basic element of the present analysis of these data. In a C-M diagram, the cluster M stars shift steadily redward as one proceeds from clusters of SWB type I to VI, due to the increasing age of the clusters along the sequence. Luminous carbon stars are present only in SWB IV-VI clusters, and are easily distinguished from M stars by their color and luminosity. 82 refs.