The structure of the Small Magellanic Cloud. II

Mathewson, D. S.; Ford, V. L.; Visvanathan, N.

doi:10.1086/166772

Cited by 84 publications

(80 citation statements)

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“…There are no direct determinations of the cluster distances along the line of sight, but it is assumed that the SMC has a depth extent of up to 20 kpc (Mathewson et al 1988;Hatzidimitriou et al 1993;Crowl et al 2001;Lah et al 2005;Glatt et al 2008b). The clusters analyzed in our study lie in the central region of the SMC main body.…”

Section: Smcmentioning

confidence: 99%

Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Glatt

Grebel

Koch

2010

A&A

166

213

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Aims. In this paper we discuss the age and spatial distribution of young (age < 1 Gyr) Small Magellanic Cloud (SMC) and Large Magellanic Cloud (LMC) clusters using data from the Magellanic Cloud Photometric Surveys. Luminosities are calculated for all age-dated clusters. Methods. The ages of 324 and 1193 populous star clusters in the SMC and the LMC were determined fitting Padova and Geneva isochrone models to their resolved color-magnitude diagrams. The clusters cover an age range between 10 Myr and 1 Gyr in each galaxy. For the SMC, a constant distance modulus of (m − M) 0 = 18.90 and a metallicity of Z = 0.004 were adopted. For the LMC, we used a constant distance modulus of (m − M) 0 = 18.50 and a metallicity of Z = 0.008. For both galaxies, we used a variable color excess to derive the cluster ages. Results. We find two periods of enhanced cluster formation in both galaxies at 160 Myr and 630 Myr (SMC) and at 125 Myr and 800 Myr (LMC). We present the spatially resolved recent star formation history of both Clouds based on young star clusters. The first peak may have been triggered by a close encounter between the SMC and the LMC. In both galaxies, the youngest clusters reside in the supergiant shells, giant shells, the intershell regions, and toward regions with a high Hα content, suggesting that their formation is related to expansion and shell-shell interaction. Most of the clusters are older than the dynamical age of the supergiant shells. No evidence of cluster dissolution was found. Computed V band luminosities show a trend toward fainter magnitudes with increasing age, as well as a trend toward brighter magnitudes with increasing apparent cluster radii.

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Section: Smcmentioning

confidence: 99%

Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Glatt

Grebel

Koch

2010

A&A

166

213

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“…The binaries are scattered over the whole galaxy, and therefore are likely representative of the galaxy mean distance. It has to be noted that several authors (e.g., Mathewson et al 1988;Hatzidimitriou et al 1993;Crowl et al 2001;Lah et al 2005;Glatt et al 2008b) found that the depth of the SMC can be up to 20 kpc. In the sample of clusters analyzed by Glatt et al (2008b), for example, the closest object has a distance modulus (m − M) 0 = 18.5, while the distance modulus of the farthest system is (m − M) 0 = 19.12.…”

Section: The Agementioning

confidence: 99%

Is the Young Star Cluster NGC 376 Dissolving in the Field of the Small Magellanic Cloud?

Sabbi

Nota

Tosi

et al. 2011

ApJ

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We use deep images acquired with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope in the filters F555W and F814W to characterize the properties of NGC 376, a young star cluster located in the wing of the Small Magellanic Cloud. Using isochrone fitting we derive for NGC 376 an age of 28 ± 7 Myr, in good agreement with previous studies. The high spatial resolution ACS data allow us to determine the center of gravity of the cluster and to construct extended surface brightness and radial density profiles. Neither of these profiles can be fitted with a theoretical model, suggesting that the cluster is not in virial equilibrium. Considering the young age of the cluster, we speculate that the distortion of the radial profiles may be the result of the rapid gas dispersal that follows the initial phase of star formation (SF). The cluster shows clear evidence of dynamical mass segregation. From the properties of the radial profiles and the present-day mass function we conclude that NGC 376 appears to have already lost nearly 90% of its initial stellar mass, probably as a consequence of the sudden gas dispersal that follows the early phase of SF.

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“…In previous studies, a single distance modulus was assumed and applied to the calculations. However, the SMC may have a depth extent of up to 20 kpc (Mathewson et al 1988;Hatzidimitriou et al 1993;Crowl et al 2001;Lah et al 2005). With the exception of NGC 419, for which we used isochrone fitting, we determined the distance modulus for each cluster using the red clump magnitude (Glatt et al 2008a).…”

Section: Comparison Of the Core Radii With Previous Studiesmentioning

confidence: 99%

Structural Parameters of Seven Small Magellanic Cloud Intermediate-Age and Old Star Clusters

Glatt

Grebel

Gallagher

et al. 2009

The Astronomical Journal

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We present structural parameters for the seven intermediate-age and old star clusters NGC 121, Lindsay 1, Kron 3, NGC 339, NGC 416, Lindsay 38, and NGC 419 in the Small Magellanic Cloud (SMC). We fit King profiles and Elson, Fall, and Freeman profiles to both surface-brightness and star-count data taken with the Advanced Camera for Surveys aboard the Hubble Space Telescope. Clusters older than ∼1 Gyr show a spread in cluster core radii that increases with age, while the youngest clusters have relatively compact cores. No evidence for post-core-collapse clusters was found. We find no correlation between core radius and distance from the SMC center, although consistent with other studies of dwarf galaxies, some relatively old and massive clusters have low densities. The oldest SMC star cluster, the only globular NGC121, is the most elliptical object of the studied clusters. No correlation is seen between ellipticity and distance from the SMC center. The structures of these massive intermediate-age (1-8 Gyr) SMC star clusters thus appear to primarily result from internal evolutionary processes.

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The structure of the Small Magellanic Cloud. II

Cited by 84 publications

References 0 publications

Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Is the Young Star Cluster NGC 376 Dissolving in the Field of the Small Magellanic Cloud?

Structural Parameters of Seven Small Magellanic Cloud Intermediate-Age and Old Star Clusters

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