Introduction
This Python module is for calculating K-corrections of galaxies in the ultraviolet, optical, and near-infrared. The method, as well as results from an earlier version of the software, are described in a paper in the Astronomical Journal.
The primary class is Kcorrect, which fits very restricted spectral
energy distribution models to galaxy photometry. These fits are based
on stellar population synthesis models and may also be interpreted
physically (e.g. in terms of stellar masses or mass-to-light ratios),
with a somewhat limited accuracy.
Of potential additional use are: