The 2.4 $\mu$m Galaxy Luminosity Function as Measured Using WISE. II.
  Sample Selection
  The WISE satellite surveyed the entire sky multiple times in four infrared
(IR) wavelengths ($3.4,\ 4.6,\ 12,$ and $22\, \mu$m, Wright et al. 2010). This
all-sky IR photometric survey makes it possible to leverage many of the large
publicly available spectroscopic redshift surveys to measure galaxy properties
in the IR. While characterizing the cross-matching of WISE data to a single
survey is a straightforward process, doing it with six different redshift
surveys takes a fair amount of space to characterize adequately, because each
survey has unique caveats and characteristics that need addressing. This work
describes a data set that results from matching five public redshift surveys
with the AllWISE data release, along with a reanalysis of the data described in
Lake et al. 2012. The combined data set has an additional flux limit of
$80\,\mu$Jy ($19.14$ AB mag) in WISE's W1 filter imposed in order to limit it
to targets with high completeness and reliable photometry in the AllWISE data
set. Consistent analysis of all of the data is only possible if the color bias
discussed in Ilbert et al. (2004) is addressed (for example: the techniques
explored in the first paper in this series Lake et al. 2017b). The sample
defined herein is used in this paper's sequel paper, Lake et al. 2017a), to
measure the luminosity function of galaxies at $2.4\, \mu$m rest frame
wavelength, and the selection process of the sample is optimized for this
purpose.
