  Physically unassociated background or foreground objects seen towards
submillimetre sources are potential contaminants of both the studies of young
stellar objects embedded in Galactic dust clumps and multiwavelength
counterparts of submillimetre galaxies (SMGs). We employed the near-infrared
and mid-infrared data from the Wide-field Infrared Survey Explorer (WISE) and
the submillimetre data from the Planck satellite, and uncovered a source,
namely WISE J044232.92+322734.9, whose WISE infrared colours suggest that it is
a star-forming galaxy (SFG), and which is seen in projection towards the
Planck-detected dust clump PGCC G169.20-8.96. We used the MAGPHYS+photo-$z$
spectral energy distribution code to derive the photometric redshift and
physical properties of J044232.92. The redshift was derived to be $z_{\rm
phot}=1.132^{+0.280}_{-0.165}$, while, for example, the stellar mass, IR (8-1
000 $\mu$m) luminosity, and star formation rate were derived to be
$M_{\star}=4.6^{+4.7}_{-2.5}\times10^{11}$ M$_{\odot}$, $L_{\rm
IR}=2.8^{+5.7}_{-1.5}\times10^{12}$ L$_{\odot}$, and ${\rm
SFR}=191^{+580}_{-146}$ ${\rm M}_{\odot}$ yr$^{-1}$. The derived value of
$L_{\rm IR}$ suggests that J044232.92 could be an ultraluminous infrared
galaxy, and we found that it is consistent with a main sequence SFG at a
redshift of 1.132. Moreover, the estimated physical properties of J044232.92
are comparable to those of SMGs. Further observations, in particular
high-resolution (sub-)millimetre and radio continuum imaging, are needed to
better constrain the redshift and physical properties of J044232.92 and to see
if the source really is a galaxy seen through a Galactic dust clump, in
particular an SMG population member at $z\sim1.1$.
