  We propose a technique for estimation of the mass m of the young stellar
population and the starburst age T in luminous compact galaxies (LCGs). For
this purpose we use LCG H{\alpha} emission line luminosities from the Sloan
Digital Sky Survey (SDSS) spectra and Galaxy Evolution Explorer (GALEX) FUV and
NUV continuum luminosities. The method is intended for quick estimation of m
and T in large galaxy samples and does not require spectral energy distribution
(SED) fitting. Estimated m and T for the sample of about 550 LCGs are compared
with the same values derived from the SED fitting in the wavelength range
\lambda\lambda 3800 -- 9200\AA. We obtain the average differences in log m and
T of 0.27 and 0.87 Myr, respectively. This technique could be used for
selection of galaxies with desired ranges of m and T or for reducing a range of
parameter variations in SED fitting.
