2005MNRAS.363.1279G


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.31CET12:41:04

2005MNRAS.363.1279G - Mon. Not. R. Astron. Soc., 363, 1279-1289 (2005/November-2)

Near-infrared surface brightness fluctuations and optical colours of Magellanic star clusters.

GONZALEZ-LOPEZLIRA R.A., ALBARRAN M.Y., MOUHCINE M., LIU M.C., BRUZUAL G.A. and DE BATZ B.

Abstract (from CDS):

This work continues our efforts to calibrate model surface brightness fluctuation luminosities for the study of unresolved stellar populations, through a comparison with the data of Magellanic Cloud star clusters. We present here the relation between absolute Ks-band fluctuation magnitude and (V-I) integrated colour, using data from the Two-Micron All-Sky Survey (2MASS) and the Deep Near-Infrared Southern Sky Survey (DENIS), and from the literature. We compare the star cluster sample with the sample of early-type galaxies and spiral bulges studied by Liu et al. We find that intermediate-age to old star clusters lie along a linear correlation with the same slope, within the errors, of that defined by the galaxies in the versus (V-I) diagram. While the calibration by Liu et al. was determined in the colour range 1.05 < (V-IC)0< 1.25, ours holds in the interval. This implies, according to Bruzual-Charlot and Mouhcine-Lanon models, that the star clusters and the latest star formation bursts in the galaxies and bulges constitute an age sequence. At the same time, a slight offset between the galaxies and the star clusters [the latter are ∼0.7 mag fainter than the former at a given value of (V-I)], caused by the difference in metallicity of roughly a factor of 2, confirms that the versus (V-I) plane may contribute to break the age-metallicity degeneracy in intermediate-age and old stellar populations. The confrontation between models and galaxy data also suggests that galaxies with Ks fluctuation magnitudes that are brighter than predicted, given their (V-I) colour, might be explained in part by longer lifetimes of thermally pulsing asymptotic giant branch stars. A preliminary comparison between the H 2MASS data of the Magellanic star clusters and the sample of 47 early-type galaxies and spiral bulges observed by Jensen et al. through the F160WHubble Space Telescope filter leads to the same basic conclusions: galaxies and star clusters lie along correlations with the same slope, and there is a slight offset between the star cluster sample and the galaxies, caused by their different metallicities. Magellanic star clusters are single populations, while galaxies are composite stellar systems; moreover, the objects analysed live in different environments. Therefore, our findings mean that the relationship between fluctuation magnitudes in the near-infrared, and (V-I) might be a fairly robust tool for the study of stellar population ages and metallicities, could provide additional constraints on star formation histories, and aid in the calibration of near-infrared surface brightness fluctuations for cosmological distance measurements.

Abstract Copyright: 2005 The Authors. Journal compilation © 2005 RAS

Journal keyword(s): stars: AGB and post-AGB - Magellanic Clouds - galaxies: star clusters - galaxies: stellar content - infrared: galaxies - infrared: stars

Simbad objects: 30

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Number of rows : 30

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9566 1
2 NGC 299 Cl* 00 53 24.74 -72 11 47.6 11.71 12.05 11.73   10.67 ~ 37 0
3 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5766 1
4 NGC 1389 GiP 03 37 11.7424496792 -35 44 45.871664087 12.80 12.39 11.50 10.99   ~ 175 1
5 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1568 0
6 NGC 1419 GiG 03 40 42.120 -37 30 39.09   13.56   12.07   ~ 114 0
7 NGC 1727 HII 04 52 13.0 -69 20 20           ~ 51 0
8 LHA 120-N 79E HII 04 52 17.2 -69 20 13           ~ 43 0
9 NGC 1777 Cl* 04 55 48 -74 17.0   13.40 12.80     ~ 41 0
10 NGC 1786 Cl* 04 59 07.470 -67 44 45.44   10.1       ~ 134 0
11 OGLE-CL LMC 318 Cl* 05 17 48.270 -69 38 53.08   12.89 12.32     ~ 27 0
12 IC 2127 EmO 05 22 12.532 -67 58 31.92     11.60     ~ 91 1
13 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15001 1
14 KMHK 879 As* 05 25 26 -67 28.4     11.75     ~ 38 0
15 NGC 1953 Cl* 05 25 29.060 -68 50 16.54   11.97 11.74     ~ 36 0
16 NGC 1951 Cl* 05 26 05.410 -66 35 51.56   10.67 10.58     ~ 29 0
17 KMHK 911 OpC 05 26 23.680 -71 41 45.98   12.77 12.70     ~ 14 0
18 NGC 1986 Cl* 05 27 37.930 -69 58 29.94   11.31 11.07     ~ 19 0
19 NGC 2001 As* 05 29 10 -68 44.8           ~ 25 0
20 NGC 2014 As* 05 32 24 -67 41.3   9.17 8.97     ~ 73 0
21 NAME Hodge 4 GlC 05 32 25.0 -64 44 11     13.33     ~ 47 0
22 NGC 2074 As* 05 39 03 -69 29.9           ~ 59 0
23 ESO 86-22 Cl* 05 42 29.090 -65 21 46.33     13.8     ~ 37 0
24 ESO 121-3 Cl* 06 02 02.0 -60 31 20   14.91 14.04     ~ 104 0
25 NGC 2193 Cl* 06 06 17 -65 05.9   14.13 13.42     ~ 46 0
26 ESO 86-61 Cl* 06 08 15 -62 59.3   14.94 14.15     ~ 34 0
27 ESO 86-66 Cl* 06 10 53 -65 02.6           ~ 13 0
28 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5909 0
29 NGC 4489 GiG 12 30 52.240 +16 45 31.31   13.2       ~ 241 0
30 NAME Local Group GrG ~ ~           ~ 7076 0

    Equat.    Gal    SGal    Ecl

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2020.10.31-12:41:04

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