The structure and evolution of rich star clusters in the Large Magellanic Cloud

Elson, Rebecca A. W.

doi:10.1086/191568

Cited by 76 publications

(112 citation statements)

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“…Our NGC 1868 profile seems to systematically include more light beyond R ∼ 5 pc. There are several possible reasons for this small discrepancy such as overestimated sky subtraction in the integral photometry by Elson (1991) or an overcorrection for completeness effects on our data. But given the entirely different photometric methods which led to the profiles shown in the figure, the level of agreement is evidence that there are no strong systematic effects in the photometry, sample selection and background subtraction in either work.…”

Section: Discussionmentioning

confidence: 82%

“…In Fig. 22 we compare the surface brightness profiles obtained by Elson (1991) for four of our clusters with the ones shown in the previous section. Both sets of profiles display a general agreement.…”

Section: Discussionmentioning

confidence: 87%

“…These questions are not easily answered without careful attention to two important issues: a) Derivation of present day mass functions (PDMFs) from luminosity functions require a mass-luminosity relation, which in turn depends on metallicity and age. Thus, this question is intimately related to finding the best fitting isochrones to the cluster CMDs and checking their sensitivity to different Elson (1991), while the solid points are from the present paper evolutionary models. This is currently underway for our clusters CMDs; b) Recovering the IMF from the PDMF requires reconstruction of the dynamical history of the cluster, something more easily done with the help of N -body simulations.…”

Section: Discussionmentioning

confidence: 96%

“…The data in the table were taken from Elson (1991), Corsi et al (1994), Will et al (1995), Mateo (1988) and Johnson et al (2000). …”

Section: Observationsmentioning

confidence: 99%

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Stellar luminosity functions of rich star clusters in the Large Magellanic Cloud

Santiago

Beaulieu

Johnson

et al. 2001

A&A

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Abstract.We show the results of deep V and I HST photometry of 6 rich star clusters in the Large Magellanic Cloud with different ages and metallicities. The number of stars with measured magnitudes in each cluster varies from about 3000 to 10 000 stars. We build stellar density and surface brightness profiles for the clusters and extract half-light radii and other structural parameters for each. We also obtain luminosity functions, Φ(MV ), down to MV 6 (M/M > ∼ 0.9), and investigate their dependence with distance from the cluster centre well beyond their half-light radius. In all clusters we find a systematic increase in the luminosity functions slope, ∆ log Φ(MV )/∆(MV ), with radial distance from the centre. Among the clusters displaying significant mass segregation are the 2 youngest in the sample: NGC 1805, NGC 1818. For these two clusters we obtain present day mass functions. The NGC 1818 mass function is in excellent agreement with that derived by other authors, also using HST data. The young cluster mass function slopes differ, that of NGC 1805 being systematically steeper than NGC 1818. Since these are very young stellar systems (τ < ∼ 40 Myrs), these variations may reflect the initial conditions rather than evolution due to internal dynamics.

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Section: Discussionmentioning

confidence: 82%

Section: Discussionmentioning

confidence: 87%

Section: Discussionmentioning

confidence: 96%

“…The data in the table were taken from Elson (1991), Corsi et al (1994), Will et al (1995), Mateo (1988) and Johnson et al (2000). …”

Section: Observationsmentioning

confidence: 99%

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Stellar luminosity functions of rich star clusters in the Large Magellanic Cloud

Santiago

Beaulieu

Johnson

et al. 2001

A&A

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“…In her analysis of the LMC star clusters, Elson (1991) noted that for clusters of a given age, there appears to exist an upper limit for their core size. Moreover, this limit was found Kontizas et al (1990) 0.28 0.10 0.10 0.23 0.13 · · · 0.23 Geyer et al (1983) 0 .…”

Section: Cluster Evolutionmentioning

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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6.2.4 Clusters in extragalactic systems

Seggewiss¹,

Richtler²

Stars and Star Clusters

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The structure and evolution of rich star clusters in the Large Magellanic Cloud

Cited by 76 publications

References 0 publications

Stellar luminosity functions of rich star clusters in the Large Magellanic Cloud

Stellar luminosity functions of rich star clusters in the Large Magellanic Cloud

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

6.2.4 Clusters in extragalactic systems

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