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Interstellar molecular clouds have power-law size L and mass M distributions of the form n(L) dL = L−αL dL and n(M) dM = M−αM dM, where M Lk is also a power law. These relations are shown to resultExpand
Cluster Mass Functions in the Large and Small Magellanic Clouds: Fading and Size-of-Sample Effects
The properties of ~939 star clusters in the Large and Small Magellanic Clouds were determined from ground-based CCD images in UBVR passbands. The areal coverage was extensive, corresponding to 11.0Expand
Evolution of the Bar Fraction in COSMOS: Quantifying the Assembly of the Hubble Sequence
We have analyzed the redshift-dependent fraction of galactic bars over 0:2 < z < 0:84 in 2157 luminous face-on spiral galaxies from the COSMOS 2 deg 2 field. Our sample is an order of magnitudeExpand
Interstellar Turbulence I: Observations and Processes
▪ Abstract Turbulence affects the structure and motions of nearly all temperature and density regimes in the interstellar gas. This two-part review summarizes the observations, theory, andExpand
Star formation from galaxies to globules
The origin of the empirical laws of galactic scale star formation is considered in view of the self-similar nature of interstellar gas and the observation that most local clusters are triggered byExpand
A Universal Formation Mechanism for Open and Globular Clusters in Turbulent Gas
A universal mechanism for cluster formation in all epochs and environments is found to be consistent with the properties and locations of young and old globular clusters, open clusters and unboundExpand
A pressure and metallicity dependence for molecular cloud correlations and the calibration of mass
The correlation of molecular cloud mass with the fourth power of the velocity dispersion, the square of the radius, and the inverse of the density squared is addressed using a modified version of theExpand
Sequential formation of subgroups in OB associations
We reconsider the structure and formation of OB association in view of recent radio and infrared observations of the adjacent molecular clouds. As a result of this reexamination, we propose that OBExpand
The largest molecular cloud complexes in the first galactic quadrant
The CO emission within a few kiloparsecs of the Sun is dominated by a small number of very large molecular complexes, including those associated with the Orion Nebula (Thaddeus 1982), M16 and M17Expand
High-resolution mass models of dwarf galaxies from LITTLE THINGS
We present high-resolution rotation curves and mass models of 26 dwarf galaxies from LITTLE THINGS. LITTLE THINGS is a high-resolution Very Large Array HI survey for nearby dwarf galaxies in theExpand