Example Survey Parameters for a 100 hr project to map 90 sq. degrees
|2.4mm||9.5 arcseconds||0.17 mJy rms|
|1.4mm||6.3 arcseconds||0.23 mJy rms|
|1.1 mm||5 arcseconds||0.26 mJy rms|
The stellar IMF is the fundamental basis of many astrophysical phenomena, from star formation rates and supernova in galaxies to the frequency of habitable planets. Despite much empirical characterization, theories for the origin of the IMF remain very poorly constrained. One current set of theories postulates that the distribution of stellar masses is inherited from the distribution of gas. This survey will map over a dozen giant molecular clouds in their entirety with sufficient depth to detect 0.05 Mʘ pre-stellar cores in all three TolTEC bands, and sufficient statistics to characterize the CMF to <0.1 Mʘ for many clouds beyond Gould’s Belt and test this theory. The substantial range of cloud properties within 2 kpc will enable the detection of any environmental effects on the CMF turnoff mass and power law index to be robustly constrained. With FWHM=5” resolution, the survey will resolve individual pre-stellar cores out to distances of 2 kpc, providing a strong statistical base for the first time to address fundamental questions such as: What is the origin of the stellar IMF? Is there an intimate link between the CMF and the IMF? Is the CMF universal?