The 388nm CN band (like the better known "G band" of CH) is used in the Sun to locate strong magnetic concentrations. Magnetic network and plage are bright in these molecular bands, since the enhanced chromospheric heating there destroys the molecule, erasing its absorption and allowing the continuum to shine through. We take advantage of this to estimate the filling factor of strong fields in active dwarf stars. CN band depths in active stars can be compared with those of inactive stars of very similar temperature and metallicity, and after an adjustment for line-blanketing, used to estimate a magnetic plage filling factor. We estimate filling factors for a two stars, and compare them to direct Stokes I line-broadening measurements. Limitations, caveats, and future directions are briefly considered.