  Stellar bars are common morphological structures in the local Universe;
according to optical and NIR surveys, they are present in about two-thirds of
disc galaxies. These elongated structures are also believed to play a crucial
role in secular evolutionary processes, because they are able to efficiently
redistribute gas, stars, and angular momentum within their hosts, although it
remains unclear as to whether they enhance or suppress star formation. A useful
tool to investigate this ambiguity is the main sequence (MS) relation, which
tightly links stellar mass ($M_{\star}$) and star formation rate (SFR). The
main goal of this work is to explore star-formation processes in barred
galaxies in order to assess the relevance of bars in star-formation quenching
and whether or not they affect the typical log-linear trend of the resolved MS.
To this purpose, we carried out a spatially resolved analysis on subkiloparsec
(subkpc) scales for a sample of six nearby barred galaxies. We collected
multi-wavelength photometric data from far-ultraviolet (FUV) to far-infrared
(FIR) from the DustPedia database and applied a panchromatic spectral energy
distribution (SED) fitting procedure on square apertures of fixed angular size
(8" $\times$ 8") using the magphys code. For each galaxy, we obtain the
distributions of stellar mass and SFR surface density and relate them in the
$\log \Sigma_{\star}$ - $\log \Sigma_{\rm SFR}$ plane, deriving the spatially
resolved MS relation. Although significant galaxy-to-galaxy variations are in
place, we infer the presence of a common anti-correlation track in
correspondence with the bar-hosting region, which shows systematically lower
SFRs. This central quiescent signature can be interpreted as the result of a
bar-driven depletion of gas reservoirs and a consequent halting of star
formation. Our findings appear to support an inside-out quenching scenario.
