Multi-wavelength study of 14000 star-forming galaxies from the Sloan
  Digital Sky Survey
  (abridged) We studied a large sample of ~14000 dwarf star-forming galaxies
with strong emission lines selected from the Sloan Digital Sky Survey (SDSS)
and distributed in the redshift range of z~0-0.6. We modelled spectral energy
distributions (SED) of all galaxies which were based on the SDSS spectra in the
visible range of 0.38-0.92 micron and included both the stellar and ionised gas
emission. These SEDs were extrapolated to the UV and mid-infrared ranges to
cover the wavelength range of 0.1-22 micron. The SDSS spectroscopic data were
supplemented by photometric data from the GALEX, SDSS, 2MASS, WISE, IRAS, and
NVSS all-sky surveys. We derived global characteristics of the galaxies, such
as their element abundances, luminosities, and stellar masses. The luminosities
and stellar masses range within the sample over ~5 orders of magnitude, thereby
linking low-mass and low-luminosity blue compact dwarf (BCD) galaxies to
luminous galaxies, which are similar to high-redshift Lyman-break galaxies
(LBGs). The luminosity L(Hbeta) of the Hbeta emission line, a characteristic of
the youngest stellar population with an age of a few Myr, is correlated with
luminosities in other wavelength ranges. This implies that the most recent
burst of star formation makes a significant contribution to the emission in the
visible range and dominates in other wavelength ranges. We found 20 galaxies
with very red WISE mid-infrared m(3.4micron)-m(4.6micron) colour (>2 mag),
which suggests the important contribution of the hot (with a temperature of
several hundred degree) dust emission in these galaxies. Our analysis of the
balance between the luminosity in the WISE bands that covered a wavelength
range of 3.4-22 micron and the luminosity of the emission absorbed at shorter
wavelengths showed that the luminosity of the hot dust emission is increased
with increasing L(Hbeta) and EW(Hbeta).
