  We investigate how different mid-infrared (mid-IR) properties of galaxies
trace the environment in which the galaxies are located. For this purpose, we
first study the dependence of galaxy clustering on the absolute magnitude at
3.4 $\mu$m and redshift. Then, we look into the environmental dependence of
mid-IR luminosities and the galaxy properties derived from these luminosities.
We also explore how various infrared galaxy luminosity selections influence the
galaxy clustering measurements. We use a set of W1 (3.4 $\mu$m) absolute
magnitude ($M_\text{W1}$) selected samples from the Galaxy and Mass Assembly
(GAMA) survey matched with mid-IR properties from the Wide-field Infrared
Survey Explorer (WISE) in the redshift range $0.07 \leq z < 0.43$. We compute
the galaxy two-point correlation function (2pCF) and compare the clustering
lengths between subsamples binned in $M_\text{W1}$ and in redshift. We also
measure the marked correlation functions (MCFs) using the luminosities in the
WISE W1 to W4 (3.4 to 22 $\mu$m) bands as marks. Additionally, we compare the
measurements of MCFs with different estimates of stellar mass and star
formation rate used as marks. Finally, we check how different selections
applied to the sample affect the clustering measurements. We show strong
clustering dependence on the W1 absolute magnitude: galaxies brighter in the W1
band are more strongly clustered than their fainter counterparts. We also
observe a lack of significant redshift dependence of clustering in the redshift
range $0.07 \leq z < 0.43$. We show that although W1 and W2 bands are direct
indicators of stellar mass, a galaxy sample selected based on W1 or W2 bands
does not perfectly show the clustering behaviour of a stellar mass selected
sample. Similar is the case with the proxy relation between W3 and W4 bands and
star formation rate.
