  In this work we use stacking analysis in \emph{Herschel} PACS to study the
accuracy of several dust-correction factors typically employed to estimate
total star-formation rate (SFR) of high-redshift star-forming (SF) galaxies. We
also analyze what stacking suggests about the relation between SFR and stellar
mass and the redshift evolution of the specific SFR (${\rm sSFR} = {\rm SFR} /
{\rm M_*}$). We find that the dust properties of massive SF galaxies evolve
with redshift, being galaxies at $z \sim 2-3$ more attenuated than at $z \sim
1$ for a given UV continuum slope and stellar mass. As a consequence, a single
IRX-$\beta$ relation can not be used to recover the total SFR of massive SF
galaxies at $0 \lesssim z \lesssim 3$. This might have implications for higher
redshift studies, where a single IRX-$\beta$ relation derived for local
starburst is usually assumed to be valid. However, we find that the local
relation between dust attenuation and stellar mass is valid at least up to $z
\sim 1$, although deviations are found for higher redshift galaxies where only
$\log{\left( M_* / M_\odot \right)} > 10.25-10.50$ galaxies are detected
through stacking. This, therefore, does not rule out the possibility that the
local dust-mass relation can be valid for less massive SF galaxies at $z \sim
2-3$. The SED fitting procedure with stellar population templates gives
over-estimated values (about 0.3--0.5 dex in $\log{\rm SFR}$) of the
dust-corrected SFR at all redshifts studied here. We find that the slope of the
main-sequence of star formation is less steep than previously found in massive
galaxies with $\log{\left( M_* / M_\odot \right)} \geq 10$, and the redshift
evolution of the sSFR reported in previous works in massive is well recovered.
