Galaxy And Mass Assembly (GAMA): $\mathbf{z \sim 0}$ Galaxy Luminosity
  Function down to $\mathbf{L \sim 10^{6}~L_\odot}$ via Clustering Based
  Redshift Inference
  In this study we present a new experimental design using clustering-based
redshift inference to measure the evolving galaxy luminosity function (GLF)
spanning 5.5 decades from $L \sim 10^{11.5}$ to $ 10^6 ~ \mathrm{L}_\odot$. We
use data from the Galaxy And Mass Assembly (GAMA) survey and the Kilo-Degree
Survey (KiDS). We derive redshift distributions in bins of apparent magnitude
to the limits of the GAMA-KiDS photometric catalogue: $m_r \lesssim 23$; more
than a decade in luminosity beyond the limits of the GAMA spectroscopic
redshift sample via clustering-based redshift inference. This technique uses
spatial cross-correlation statistics for a reference set with known redshifts
(in our case, the main GAMA sample) to derive the redshift distribution for the
target ensemble. For the calibration of the redshift distribution we use a
simple parametrisation with an adaptive normalisation factor over the interval
$0.005 < z < 0.48$ to derive the clustering redshift results. We find that the
GLF has a relatively constant power-law slope $\alpha \approx -1.2$ for $-17
\lesssim M_r \lesssim -13$, and then appears to steepen sharply for $-13
\lesssim M_r \lesssim -10$. This upturn appears to be where Globular Clusters
(GCs) take over to dominate the source counts as a function of luminosity. Thus
we have mapped the GLF across the full range of the $z \sim 0$ field galaxy
population from the most luminous galaxies down to the GC scale.
