2008/03/21 by Bruce G. Elmegreen, Elmegreen, Bruce G. · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.0803.3154
23 pages, 6 figures, Posted on the conference web page, http://ssc.spitzer.caltech.edu/mtgs/ismevol/, for the 4th Spitzer Science Center Conference, ``The Evolving ISM in the Milky Way and Nearby Galaxies: Recycling in the Nearby Universe;'' December 2-5, 2007 at the Hilton Hotel, Pasadena, California
arxiv created 2008/03/21 · openalex publication_date 2008/03/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The characteristic mass Mc and slope Gamma of the IMF are reviewed for clusters, field regions, galaxies, and regions formed during cosmological times. Local star formation has a somewhat uniform Mc and Gamma. Statistical variations in Gamma are summarized, as are the limitations imposed by these variations. Cosmological star formation appears to have both a higher Mc and a slightly shallower slope at intermediate to high stellar mass. The center of the Milky Way may have a shallow slope too. Field regions have slightly steeper slopes than clusters, but this could be the result of enhanced drift of low mass stars out of clusters and associations. Dwarf galaxies also have steeper slopes. Results from the observation of pre-stellar clumps are reviewed too. Pre-stellar clumps appear to have about the same mass function as stars and are therefore thought to be the main precursors to stars. If this is the case, then the IMF is generally determined by gas-phase processes. Brown dwarf formation also shares many characteristics of star formation, suggesting that they form by similar mechanisms.