In
astronomy, the
initial mass function (
IMF) is an
empirical function that describes the
distribution of initial masses for a population of stars. The IMF is often given as a
probability distribution function (PDF) for the mass at which a star enters the
main sequence (begins
hydrogen fusion). The distribution function can then be used to construct the
mass distribution (the
histogram of stellar masses) of a population of stars. The properties and evolution of a star are closely related to its mass, so the IMF is an important diagnostic tool for astronomers studying large quantities of stars. For example, the initial mass of a star is the primary factor determining its
colour,
luminosity, and lifetime. The IMF is relatively invariant from one group of stars to another, though some observations suggest that the IMF is different in different environments.