  Using VIPERS, we estimated a set of SFR based on photometric and
spectroscopic data. We used, as estimators, photometric bands from ultraviolet
to mid-infrared, and spectral lines. Assuming a reference SFR obtained from the
spectral energy distribution reconstructed with Code Investigating GALaxy
Emission, we estimated the reliability of each band as an SFR tracer. We used
GSWLC to trace the dependence of these SFR calibrators with redshift. The far
and near UV, u-band and 24-$\mu$m bands, as well as $L_{TIR}$, are found to be
good SFR tracers up to $z\sim0.9$ with a strong dependence on the attenuation
prescription used for the bluest bands (scatter of SFR of 0.26, 0.14, 0.15,
0.23, and 0.24dex for VIPERS, and 0.25, 0.24, 0.09, 0.12, and 0.12dex for
GSWLC). The 8-$\mu$m band provides only a rough estimate of the SFR as it
depends on metallicity and polycyclic aromatic hydrocarbon properties (scatter
of 0.23dex for VIPERS). We estimated the scatter of rest-frame luminosity
estimations from CIGALE to be 0.26, 0.14, 0.12, 0.15, and 0.20dex for FUV, NUV,
ugriz, K$_{\mathrm{s}}$, and 8-24$\mu$m-$L_{\mathrm{TIR}}$). At intermediate
redshift, the H$\beta$ line is a reliable SFR tracer (scatter of 0.19dex) and
the [OII] line gives an equally good estimation when the metallicity from the
$R_{23}$ parameter is taken into account (0.17 for VIPERS and 0.20dex for
GSWLC). A calibration based on [OIII] retrieves the SFR only when additional
information such as the metallicity or the ionization parameter of galaxies are
used (0.26 for VIPERS and 0.20dex for GSWLC), diminishing its usability as a
direct SFR tracer. Based on rest-frame luminosities estimated with CIGALE, we
propose our own set of calibrations from FUV, NUV, u-band, 8, 24$\mu$m,
$L_{TIR}$, H$\beta$, [OII], and [OIII].
