other query modes : |
Identifier query |
Coordinate query |
Criteria query |
Reference query |
Basic query |
Script submission |
TAP |
Output options |
Object types |
Help |
2006MNRAS.366..295D - Mon. Not. R. Astron. Soc., 366, 295-307 (2006/February-2)
How well do we know the age and mass distributions of the star cluster system in the Large Magellanic Cloud?
DE GRIJS R. and ANDERS P.
Abstract (from CDS):
The LMC's cluster formation rate (CFR) has been roughly constant outside of the well-known age gap between ∼3 and 13Gyr, when the CFR was a factor of ∼5 lower. Using a simple approach to derive the characteristic cluster disruption time-scale, we find that log(tdis4/yr) = 9.9±0.1, where tdis=tdis4(Mcl/104M☉)0.62. This long characteristic disruption time-scale implies that we are observing the initial cluster mass function (CMF). We conclude that while the older cluster (sub)samples show CMF slopes that are fully consistent with the α≃-2 slopes generally observed in young star cluster systems, the youngest mass and luminosity-limited LMC cluster subsets show shallower slopes (at least below masses of a few x103M☉), which is contrary to dynamical expectations. This may imply that the initial CMF slope of the LMC cluster system as a whole is not well represented by a power law, although we cannot disentangle the unbound from the bound clusters at the youngest ages.
Abstract Copyright: 2005 The Authors. Journal compilation © 2005 RAS
Journal keyword(s): methods: data analysis - Magellanic Clouds - galaxies: star clusters - galaxies: stellar content
Simbad objects: 9
To bookmark this query, right click on this link: simbad:2006MNRAS.366..295D and select 'bookmark this link' or equivalent in the popup menu