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Physically unassociated background or foreground objects seen towardssubmillimetre sources are potential contaminants of both the studies of youngstellar objects embedded in Galactic dust clumps and multiwavelengthcounterparts of submillimetre galaxies (SMGs). We employed the near-infraredand mid-infrared data from the Wide-field Infrared Survey Explorer (WISE) andthe submillimetre data from the Planck satellite, and uncovered a source,namely WISE J044232.92+322734.9, whose WISE infrared colours suggest that it isa star-forming galaxy (SFG), and which is seen in projection towards thePlanck-detected dust clump PGCC G169.20-8.96. We used the MAGPHYS+photo-$z$spectral energy distribution code to derive the photometric redshift andphysical properties of J044232.92. The redshift was derived to be $z_{\rmphot}=1.132^{+0.280}_{-0.165}$, while, for example, the stellar mass, IR (8-1000 $\mu$m) luminosity, and star formation rate were derived to be$M_{\star}=4.6^{+4.7}_{-2.5}\times10^{11}$ M$_{\odot}$, $L_{\rmIR}=2.8^{+5.7}_{-1.5}\times10^{12}$ L$_{\odot}$, and ${\rmSFR}=191^{+580}_{-146}$ ${\rm M}_{\odot}$ yr$^{-1}$. The derived value of$L_{\rm IR}$ suggests that J044232.92 could be an ultraluminous infraredgalaxy, and we found that it is consistent with a main sequence SFG at aredshift of 1.132. Moreover, the estimated physical properties of J044232.92are comparable to those of SMGs. Further observations, in particularhigh-resolution (sub-)millimetre and radio continuum imaging, are needed tobetter constrain the redshift and physical properties of J044232.92 and to seeif the source really is a galaxy seen through a Galactic dust clump, inparticular an SMG population member at $z\sim1.1$.

WISE J044232.92+322734.9: A star-forming galaxy at redshift 1.1 seen through a Galactic dust clump?