POPULATION PARAMETERS OF INTERMEDIATE-AGE STAR CLUSTERS IN THE LARGE MAGELLANIC CLOUD. III. DYNAMICAL EVIDENCE FOR A RANGE OF AGES BEING RESPONSIBLE FOR EXTENDED MAIN-SEQUENCE TURNOFFS

• Published in: The Astrophysical journal Vol. 737; no. 1; p. jQuery1323905036333='48'
• Main Authors: GOUDFROOIJ, Paul, PUZIA, Thomas H, CHANDAR, Rupali, KOZHURINA-PLATAIS, Vera
• Format: Journal Article
• Language: English
• Published: Bristol IOP 10.08.2011
• Subjects: Age; Astronomy; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; Clusters; DISTRIBUTION; Earth, ocean, space; Escape velocity; Exact sciences and technology; GALAXIES; GIANT STARS; Iron; MAGELLANIC CLOUDS; Population III stars; Red giant stars; SPATIAL DISTRIBUTION; STAR CLUSTERS; STARS; STELLAR ACTIVITY; STELLAR WINDS; VELOCITY; Red giant stars; Stellar winds; Accretion; Radial distribution; Globular clusters; Star clusters; Escape velocity; Star formation; Stellar population; globular clusters: general; Magellanic Clouds; Asymptotic giant branch; Age; Interstellar matter; Large Magellanic Cloud
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/737/1/4

We present a new analysis of 11 intermediate-age (1-2 Gyr) star clusters in the Large Magellanic Cloud based on Hubble Space Telescope imaging data. Seven of the clusters feature main-sequence turnoff (MSTO) regions that are wider than can be accounted for by a simple stellar population, whereas their red giant branches (RGBs) indicate a single value of [Fe/H]. The star clusters cover a range in present-day mass from about 1 X 104 M to 2 X 105 M . We compare radial distributions of stars in the upper and lower parts of the MSTO region, and calculate cluster masses and escape velocities from the present time back to a cluster age of 10 Myr. Our main result is that for all clusters in our sample with estimated escape velocities v esc 15 km s--1 at an age of 10 Myr, the stars in the brightest half of the MSTO region are significantly more centrally concentrated than the stars in the faintest half and more massive RGB and asymptotic giant branch stars. This is not the case for clusters with v esc 10 km s--1 at an age of 10 Myr. We argue that the wide MSTO region of such clusters is caused mainly by a ~200-500 Myr range in the ages of cluster stars due to extended star formation within the cluster from material shed by first-generation stars featuring slow stellar winds. Dilution of this enriched material by accretion of ambient interstellar matter is deemed plausible if the spread of [Fe/H] in this ambient gas was very small when the second-generation stars were formed in the cluster.