UV dust attenuation as a function of stellar mass and its evolution with
  redshift
  Studying the UV dust attenuation, as well as its relation to other galaxy
parameters such as the stellar mass, plays an important role in
multi-wavelength research. This work relates the dust attenuation to the
stellar mass of star forming galaxies, and its evolution with redshift. A
sample of galaxies with an estimate of the dust attenuation computed from the
infrared excess was used. The dust attenuation vs. stellar mass data, separated
in redshift bins, was modelled by a single parameter linear function, assuming
a nonzero constant apparent dust attenuation for low mass galaxies. But the
origin of this effect is still to be determined and several possibilities are
explored (actual high dust content, variation of the dust-to-metal ratio,
variation of the stars-dust geometry). The best-fitting parameter of this model
is then used to study the redshift evolution of the cosmic dust attenuation and
is found to be in agreement with results from the literature. This work also
gives evidence to a redshift evolution of the dust attenuation - stellar mass
relationship, as is suggested by recent works in the highest redshift range.
