  Far-infrared observations from the \textit{Herschel Space Observatory} are
used to estimate the infrared (IR) properties of ultraviolet-selected galaxies.
We stack the PACS (100, 160 $\mu \mathrm{m}$) and SPIRE (250, 350 and 500$\mu
\mathrm{m}$) maps of the Chandra deep field south (CDFS) on a source list of
galaxies selected in the rest-frame ultraviolet (UV) in a redshift range of
$0.6-1.2$. This source list is created using observations from the XMM-OM
telescope survey in the CDFS using the UVW1 (2910 {\AA}) filter. The stacked
data are binned according to the UV luminosity function of these sources, and
the average photometry of the UV-selected galaxies is estimated. By fitting
modified black bodies and IR model templates to the stacked photometry, average
dust temperatures and total IR luminosity are determined. The
luminosity-weighted average temperatures are consistent with a weak trend of
increasing temperature with redshift found by previous studies. Infrared
excess, unobscured, and obscured star formation rate (SFR) values are obtained
from the UV and IR luminosities. We see a trend in which dust attenuation
increases as UV luminosity decreases. It remains constant as a function of IR
luminosities at fixed redshift across the luminosity range of our sources. In
comparison to local luminous infrared galaxies with similar SFRs, the higher
redshift star-forming galaxies in the sample show a lesser degree of dust
attenuation. Finally, the inferred dust attenuation is used to correct the
unobscured SFR density in the redshift range $0.6-1.2$. The dust-corrected SFR
density is consistent with measurements from IR-selected samples at similar
redshifts.
