Galaxy and Mass Assembly (GAMA): Mid-infrared properties as tracers of
  galaxy environment
  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 correlation between various
mid-IR properties and the environment. 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. We
also measure MCFs with different estimates of stellar mass and star formation
rate used as marks and compare the results. 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 W1 and W2 bands closely
follow the stellar mass and W3 and W4 bands closely follow the star formation
rate in tracing the galaxy clustering. We demonstrate the agreement between
different estimates of the stellar mass and the star formation rate in tracing
the environment.
