[PDF] Top 20 Young, Massive Star Clusters in the Antennae

... 117 clusters and the two nuclear regions of the ...the Antennae containing active star ...the Antennae and present the first statistical analysis of the differences in cluster age and mass ... See full document

... from clusters 6 and 7 contains a string of smaller H II regions or 30 Doradus/R136-type star clusters, with slightly redder colours than the compact YMCs, which are likely older but otherwise similar ... See full document

... in clusters (Lada & Lada 2003) and disperse into the galactic ...Some star formation sites produce tightly bound clusters, such as the young super-star clusters observed in ... See full document

... of young clusters with N-body simulations of clusters including the effects of rapid gas loss, we argue that young clusters are not in Virial ...the clusters and not related to ... See full document

... most massive star allowed in any cluster is 20 M ...of clusters that have survived any initial gas expulsion phase, and relaxed into a bound ...our clusters at a formal age of zero, really the ... See full document

... Wolf-Rayet star inside this shell, and the possible X-ray discovery of an older population dispersed around Pis 24 (Wang et ...embedded clusters in the molecular cloud south and east of ...multiple ... See full document

... either young or old, however, although older clusters are in general believed to be more spherical than younger ...non-spherical clusters of all ages (van den Bergh 1991; Goodwin 1997), while ... See full document

... many massive stars at all stages of formation and evolution, from embedded molecular cores to post-main-sequence ...central star clusters Danks 1 and Danks 2, using Hubble Space Telescope+NICMOS ... See full document

... of massive stars in the evolution of ga- laxies is ...subsequent star formation. Most massive stars are formed in a clustered environ- ment and are short lived ...investigate young ... See full document

... In order to mimic the process by which a velocity dispersion is measured from the line widths in an integrated spectrum of an ob- served cluster, the distribution of line-of-sight velocities was fitted by a Gaussian of ... See full document

... It is important to note the index is not a measure of local sur- face density – Eq. (5) describes the local spatial distribution of point j. Therefore although the index is proportional to the local point surface density ... See full document

... which are used to derive the final IMF and its uncertainties. In Fig. 7, we show the IMF and the corresponding fits in the power- law form dN/dM ∝ M −α . A Poisson uncertainty is assigned to each fitted data point, but ... See full document

... As part of the ongoing effort to characterize the low-mass ( sub ) stellar population in a sample of massive young clusters, we have targeted the ∼ 2 Myr old cluster NGC 2244. The distance to NGC ... See full document

... 2005). Star clusters form within giant molecular clouds and remain em- bedded in their natal clouds for ∼2–5 Myr before the combined effect of massive stellar winds and supernovae drive out the gas ... See full document

... The shaded area towards the top of Fig. 24 indicates the region of the parameter space where MPC candidates are thought to be found (see Bressert et al. 2012 for details). Comparing the upper end of the observed ... See full document

... Chandra’s sensitivity to point sources is highly dependent on the size of the point spread function, which is itself dependent on the distance from the centre of the observation, known as the off- axis angle. This leads ... See full document

... Vizgin and V. Ya. Frenkel named their article as "Vsevolod Konstantinovich Frederiks as a pioneer of relativity and liquid crystal physics in USSR" [11]. After finishing high school Vsevolod Kostantinovich ... See full document

... with star-formation rate have also been seen in Hα ...of star formation surface ...increasing star formation surface ...individual star formation surface densities and plot the broad-line FWHM ... See full document

... Assuming that luminosity fading dominates the evolution of the FP, its parallel shifting over time traces evolution in M/L (e.g., Treu et al. 2001). For a given cosmology and IMF this constrains the stellar age, and the ... See full document

... the star collapses to a space-time singularity, when the star is sufficiently massive so that no equilibrium state is possible and the gravitational full overcomes all the internal pressures and ... See full document