Simulating Brown Dwarf Observations for Various Mass Functions, Birthrates, and Lowmass Cutoffs
Abstract
After decades of brown dwarf discovery and followup, we can now infer the functional form of the mass distribution within 20 pc, which serves as a constraint on star formation theory at the lowest masses. Unlike objects on the main sequence that have a clear luminositytomass correlation, brown dwarfs lack a correlation between an observable parameter (luminosity, spectral type, or color) and mass. A measurement of the brown dwarf mass function must therefore be procured through proxy measurements and theoretical models. We utilize various assumed forms of the mass function, together with a variety of birthrate functions, lowmass cutoffs, and theoretical evolutionary models, to build predicted forms of the effective temperature distribution. We then determine the best fit of the observed effective temperature distribution to these predictions, which in turn reveals the most likely mass function. We find that a simple power law (
 Publication:

The Astrophysical Journal
 Pub Date:
 October 2024
 DOI:
 10.3847/15384357/ad62fc
 arXiv:
 arXiv:2406.09690
 Bibcode:
 2024ApJ...974..222R
 Keywords:

 Stellar mass functions;
 Initial mass function;
 Brown dwarfs;
 Star formation;
 Solar neighborhood;
 1612;
 796;
 185;
 1569;
 1509;
 Astrophysics  Solar and Stellar Astrophysics;
 Astrophysics  Earth and Planetary Astrophysics
 EPrint:
 13 pages, 14 figures, 1 table, accepted to ApJ