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2005ApJS..161..304M - Astrophys. J., Suppl. Ser., 161, 304-360 (2005/December-0)
Resolved massive star clusters in the Milky way and its satellites: brightness profiles and a catalog of fundamental parameters.
McLAUGHLIN D.E. and VAN DER MAREL R.P.
Abstract (from CDS):
The structural and dynamical parameters are derived from fitting three different models–the modified isothermal sphere of King; an alternate modified isothermal sphere based on the ad hoc stellar distribution function of Wilson; and asymptotic power-law models with constant-density cores–to the surface-brightness profile of each cluster. Surface-brightness data for the LMC, SMC, and Fornax clusters are based in large part on the work of Mackey & Gilmore, but include significant supplementary data culled from the literature and important corrections to Mackey & Gilmore's V-band magnitude scale. The profiles of Galactic globular clusters are taken from Trager et al. We address the question of which model fits each cluster best, finding in the majority of cases that the Wilson models–which are spatially more extended than King models but still include a finite, ``tidal'' cutoff in density–fit clusters of any age, in any galaxy, as well as or better than King models. Untruncated, asymptotic power laws often fit about as well as Wilson models but can be significantly worse. We argue that the extended halos known to characterize many Magellanic Cloud clusters may be examples of the generic envelope structure of self-gravitating star clusters, not just transient features associated strictly with young age.
Abstract Copyright: ∼
Journal keyword(s): Galaxies: Star Clusters - Galaxy: Globular Clusters: General - Galaxies: Magellanic Clouds
VizieR on-line data: <Available at CDS (J/ApJS/161/304): clusters.dat table5.dat table8.dat table10.dat table11.dat table12.dat table13.dat table14.dat>
CDS comments: Table 7: clusters 2MS-GC01, GC02 not identified.
Simbad objects: 225
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