AN UPDATED CATALOG OF M33 CLUSTERS AND CANDIDATES:<i>UBVRI</i>PHOTOMETRY AND SOME STATISTICAL RESULTS

Ma, Jun

doi:10.1088/0004-6256/144/2/41

Cited by 9 publications

(1 citation statement)

References 43 publications

(156 reference statements)

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“…In this paper, we adopted the reddening values of the sample clusters obtained by Sarajedini et al (1998) and Ma et al (2002). The BVI magnitudes of eight sample clusters are from Ma (2012) and Ma (2013), who presented new UBVRI photometry for 626 star clusters and candidates in M33, including eight sample clusters (except for R12 and R14), using archival images from the Local Group Galaxies Survey . The BVI magnitudes of R12 and R14 are from Christian & Schommer (1988).…”

Section: Halo Gc Sample In M33mentioning

confidence: 99%

Structural Parameters for 10 Halo Globular Clusters in M33

2015

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In this paper, we present the properties of 10 halo globular clusters (GCs) with luminosities L ; 5-7 × 10 5 L e in the Local Group galaxy M33 using images from the Hubble Space Telescope WFPC2 in the F555W and F814W bands. We obtained the ellipticities, position angles, and surface brightness profiles for each GC. In general, the ellipticities of the M33 sample clusters are similar to those of the M31 clusters. The structural and dynamical parameters are derived by fitting the profiles to three different models combined with mass-to-light ratios (M/L values) from population-synthesis models. The structural parameters include core radii, concentration, half-light radii, and central surface brightness. The dynamical parameters include the integrated cluster mass, integrated binding energy, central surface mass density, and predicted line of sight velocity dispersion at the cluster center. The velocity dispersions of the four clusters predicted here agree well with the observed dispersions by Larsen et al. The results here showed that the majority of the sample halo GCs are better fitted by both the King model and the Wilson model than the Sérsic model. In general, the properties of the clusters in M33, M31, and the Milky Way fall in the same regions of parameter spaces. The tight correlations of cluster properties indicate a "fundamental plane" for clusters, which reflects some universal physical conditions and processes operating at the epoch of cluster formation.

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Section: Halo Gc Sample In M33mentioning

confidence: 99%

Structural Parameters for 10 Halo Globular Clusters in M33

2015

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Globular Clusters in the Local Group

Grebel

2014

Proc. IAU

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Only twelve of the > 76 Local Group galaxies contain globular clusters, showing a broad range of specific frequencies. Here we summarize the properties of these globular cluster systems. Many host galaxies contain very old globulars, but in some globular cluster formation may have been delayed. An age range of several Gyr is common. Except for the inner regions of the spirals, old globular clusters tend to be metal-poor. Increasingly, light element variations and hints of multiple stellar populations are being found also in extragalactic globulars. There is ample evidence for globular cluster accretion from dwarfs onto massive galaxies, but its magnitude has yet to be quantified. Caution is needed to avoid overinterpreting indirect evidence.

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Deriving physical parameters of unresolved star clusters

Meulenaer

Narbutis

Mineikis

et al. 2013

A&A

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Context. Stochasticity and physical parameter degeneracy problems complicate the derivation of the parameters (age, mass, and extinction) of unresolved star clusters when using broad-band photometry. Aims. We develop a method to simulate stochasticity and degeneracies and to investigate their influence on the accuracy of derived physical parameters. Then we apply it to star cluster samples of M 31 and M 33 galaxies. Methods. Age, mass, and extinction of observed star clusters are derived by comparing their broad-band U BVRI integrated magnitudes to the magnitudes of a large grid of star cluster models with fixed metallicity Z = 0.008. Masses of stars for a cluster model are randomly sampled from the initial mass function. Models of star clusters from the model grid, which have all of their magnitudes located within 3 observational errors from the magnitudes of the observed cluster, are selected for computing their age, mass, and extinction.Results. In the case of the M 31 galaxy, the extinction range is wide and the age-extinction degeneracy is strong for a fraction of its clusters. Because of a narrower extinction range, the age-extinction degeneracy is weaker for the M 33 clusters. By using artificial cluster sample, we show that age-extinction degeneracy can be reduced significantly if the range of intrinsic extinction within the host galaxy is narrow.

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AN UPDATED CATALOG OF M33 CLUSTERS AND CANDIDATES:UBVRIPHOTOMETRY AND SOME STATISTICAL RESULTS

Cited by 9 publications

References 43 publications

Structural Parameters for 10 Halo Globular Clusters in M33

Structural Parameters for 10 Halo Globular Clusters in M33

Globular Clusters in the Local Group

Deriving physical parameters of unresolved star clusters

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