J/MNRAS/436/136 Ages and masses of LMC clusters (de Grijs+, 2013)
No compelling evidence of significant early star cluster disruption in the
Large Magellanic Cloud.
de Grijs R., Goodwin S.P., Anders P.
<Mon. Not. R. Astron. Soc., 436, 136-149 (2013)>
=2013MNRAS.436..136D 2013MNRAS.436..136D
ADC_Keywords: Magellanic Clouds ; Associations, stellar
Keywords: galaxies: evolution - galaxies: individual: Large Magellanic Cloud -
Magellanic Clouds; galaxies: star clusters: general
Abstract:
Whether or not the rich star cluster population in the Large
Magellanic Cloud (LMC) is affected by significant disruption during
the first few x108yr of its evolution is an open question and the
subject of significant current debate. Here, we revisit the problem,
adopting a homogeneous data set of broad-band imaging observations. We
base our analysis mainly on two sets of self-consistently determined
LMC cluster ages and masses, one using standard modelling and one
which takes into account the effects of stochasticity in the clusters'
stellar mass functions. On their own, the results based on any of the
three complementary analysis approaches applied here are merely
indicative of the physical conditions governing the cluster
population. However, the combination of our results from all three
different diagnostics leaves little room for any conclusion other than
that the optically selected LMC star cluster population exhibits no
compelling evidence of significant disruption - for clusters with
masses, Mcl, of log(Mcl/M☉)≳3.0-3.5 - between the
age ranges of [3-10 and 30-100]Myr, either 'infant mortality' or
otherwise. In fact, there is no evidence of any destruction beyond
that expected from simple models just including stellar dynamics and
stellar evolution for ages up to 1Gyr. It seems, therefore, that the
difference in environmental conditions in the Magellanic Clouds on the
one hand and significantly more massive galaxies on the other may be
the key to understanding the apparent variations in cluster disruption
behaviour at early times.
Description:
We specifically focused on the catalogue of Glatt, Grebel & Koch
(2010, Cat. J/A+A/571/A50), who compiled data of 1193 populous LMC
clusters with ages of up to 1 Gyr based on the most up-to-date and
comprehensive LMC object catalogue of Bica et al. (2008, Cat.
J/MNRAS/389/678). Glatt et al. (2010, Cat. J/A+A/571/A50) used the
optical broad-band photometry from the Magellanic Clouds Photometric
Survey (MCPS; Zaritsky et al., 2004, Cat. J/AJ/128/1606) to construct
colour-magnitude diagrams (CMDs) and subsequently determined ages for
their entire sample based on isochrone fits.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 96 747 LMC cluster positions and derived parameters
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See also:
J/AJ/128/1606 : MCPS: the LMC (Zaritsky+, 2004)
J/MNRAS/389/678 : Extended objects in Magellanic Clouds (Bica+, 2008)
J/A+A/517/A50 : Young SMC/LMC star clusters ages + luminosities (Glatt+ 2010)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh Hour of Right Ascension (J2000)
4- 5 I2 min RAm Minute of Right Ascension (J2000)
7- 11 F5.2 s RAs Second of Right Ascension (J2000)
13 A1 --- DE- Sign of the Declination (J2000)
14- 15 I2 deg DEd Degree of Declination (J2000)
17- 18 I2 arcmin DEm Arcminute of Declination (J2000)
20- 24 F5.2 arcsec DEs Arcsecond of Declination (J2000)
26- 31 F6.3 mag VMAG [-9.8/-1.6] Integrated absolute V-band magnitude
33- 38 F6.3 [yr] logAg.m log of the minimum age
40- 45 F6.3 [yr] logAg.B log of the best age
47- 52 F6.3 [yr] logAg.M log of the maximum age
54- 58 F5.3 [Msun] logM.m log of the minimum mass
60- 64 F5.3 [Msun] logM.B log of the best mass
66- 70 F5.3 [Msun] logM.M log of the maximum mass
72- 96 A25 --- Name Cluster name(s)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 19-Oct-2014