2007A&A...462..139K


C.D.S. - SIMBAD4 rel 1.7 - 2019.07.21CEST11:47:43

2007A&A...462..139K - Astronomy and Astrophysics, volume 462, 139-156 (2007/1-4)

Physical parameters of 15 intermediate-age LMC clusters from modelling of HST colour-magnitude diagrams.

KERBER L.O., SANTIAGO B.X. and BROCATO E.

Abstract (from CDS):

We analyzed HST/WFPC2 colour-magnitude diagrams (CMDs) of 15 populous Large Magellanic Cloud (LMC) stellar clusters with ages between ∼0.3Gyr and ∼3Gyr. These (V, B-V) CMDs are photometrically homogeneous and typically reach V∼22. Accurate and self-consistent physical parameters (age, metallicity, distance modulus and reddening) were extracted for each cluster by comparing the observed CMDs with synthetic ones. These determinations involved simultaneous statistical comparisons of the main-sequence fiducial line and the red clump position, offering objective and robust criteria to determine the best models. The models explored a regular grid in the parameter space covered by previous results found in the literature. Control experiments were used to test our approach and to quantify formal uncertainties. In general, the best models show a satisfactory fit to the data, constraining well the physical parameters of each cluster. The age-metallicity relation derived by us presents a lower spread than similar results found in the literature for the same clusters. Our results are in accordance with the published ages for the oldest clusters, but reveal a possible underestimation of ages by previous authors for the youngest clusters. Our metallicity results in general agree with the ones based on spectroscopy of giant stars and with recent works involving CMD analyses. The derived distance moduli implied by the most reliable solutions, correlate with the reddening values, as expected from the non-negligible three-dimensional distribution of the clusters within the LMC. The inferred spatial distribution for these clusters is roughly aligned with the LMC disk, being also more scattered than recent numerical predictions, indicating that they were not formed in the LMC disk. The set of ages and metallicities homogeneously derived here can be used to calibrate integrated light studies applied to distant galaxies.

Abstract Copyright:

Journal keyword(s): galaxies: star clusters - Magellanic Clouds - Hertzsprung-Russell (HR) and C-M diagrams

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 8999 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5301 1
3 NGC 1651 GlC 04 37 32.530 -70 35 08.71   12.99 12.28     ~ 106 0
4 NGC 1718 Cl* 04 52 25.040 -67 03 08.50   13.01 12.25     ~ 66 0
5 NGC 1777 Cl* 04 55 48 -74 17.0   13.40 12.80     ~ 41 0
6 NGC 1818 GlC 05 04 13.300 -66 26 05.47   9.7       ~ 231 0
7 NGC 1831 GlC 05 06 17.4 -64 55 11   11.52 11.18     ~ 151 0
8 NGC 1856 Cl* 05 09 30.290 -69 07 45.08   10.40 10.06     ~ 134 0
9 NGC 1868 GlC 05 14 36 -63 57.3   12.02 11.57     ~ 113 0
10 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14185 1
11 2MASX J05283953-7337514 GlC 05 28 39.531 -73 37 51.45   14.14 13.42     ~ 47 0
12 ESO 86-22 Cl* 05 42 29.090 -65 21 46.33     13.8     ~ 36 0
13 NGC 2121 Cl* 05 48 13.190 -71 28 52.00   13.21 12.37     ~ 110 0
14 NGC 2173 GlC 05 57 58 -72 58.7   12.74 11.88     ~ 129 0
15 NGC 2155 Cl* 05 58 32.070 -65 28 38.62   13.41 12.60     ~ 90 0
16 NGC 2162 GlC 06 00 31 -63 43.3   13.38 12.70     ~ 75 0
17 ESO 121-3 Cl* 06 02 02.0 -60 31 20   14.91 14.04     ~ 103 0
18 NGC 2209 GlC 06 08 34 -73 50.5   13.58 13.15     ~ 106 0
19 NGC 2213 Cl* 06 10 42.000 -71 31 43.99   13.09 12.38     ~ 87 0
20 NGC 2249 GlC 06 25 49 -68 55.2   12.66 12.23     ~ 62 0

    Equat.    Gal    SGal    Ecl

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2019.07.21-11:47:43

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