The UV radiation is considered to be one of the best tracers of star formation rate (SFR), but it only gives an incomplete picture of the star formation activity. A big fraction of the UV emission produced by stars does not manage to escape the dust in the star forming regions. There are proposed methods to correct the star formation rate for the dust absorption. These relations, calibrated in the local universe and then applied to surveys at higher redshifts, are under the scanner recently.
The questions that arise now are : whether these relations evolve as we trace back the history of the universe? And whether (or not) these relations keep their functional form as the ensemble properties of galaxies change? In this work we try to answer these questions using UV data from XMM-Newton Optical/UV Monitor telescope (XMM-OM) and FIR data from the five Herschel bands. We stack the UV sources on the FIR maps from Herschel PACS and SPIRE instruments to produce average estimates of the FIR luminosities coming from the UV selected star-forming galaxies. The dust attenuation relation is constrained using the IRX ratio in the redshift range 0.6 - 1.2 which corresponding to the epoch just after the peak of the star formation activity in the universe.