Thousands of star clusters in M51 with HST/ACS

  title={Thousands of star clusters in M51 with HST/ACS},
  author={Remco Scheepmaker and Mark Gieles and Marcel Richard Haas and Nate Bastian and S. Larsen and Hjglm Lamers},
We study the entire star cluster population in the disk of M51 by using radius measurements, and we see evidence for a universal preferred radius for both young and old cluster populations and for an increased cluster formation rate at a galactocentric distance of ∼6 kpc, which is similar to the corotation radius. 
How Initial Size Governs Core Collapse in Globular Clusters
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Star formation rates (SFRs) larger than 1000 Myr −1 are observed in extreme starbursts. This leads to the formation of star clusters with masses >10 6 Min which crowding of the pre-stellar cores may
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Essentially all stars form in giant molecular clouds (GMCs). However, inside GMCs, most of the gas does not participate in star formation; rather, denser gas accumulates in clumps in the GMC, with


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ACS imaging of star clusters in M 51. I. Identification and radius distribution
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A detailed description is given of the data analysis leading to the discovery of young massive star clusters (YMCs) in a sample of 21 nearby galaxies. A new useful tool, ishape , for the derivation
Observational evidence for a truncation of the star cluster initial mass function at the high mass end
We present the luminosity function (LF) of star clusters in M51 based on HST/ACS observations taken as part of the Hubble Heritage project. The clusters are selected based on their size and with the
Diameters of Galactic globular clusters
All published aperture photometry of Galactic globular clusters has been used to derive total magnitudes, V(t), and values of the diameter containing half the cluster light in projection, D(0.5). For
Galactic Dynamics
Two of the world’s leading astrophysicists, James Binney and Scott Tremaine, here present a comprehensive review of the theory of galactic dynamics at a level suitable for both graduate students and
  • ApJ
  • 2005
Gieles et al: A&A (in prep
  • Gieles et al: A&A (in prep
  • 2006