Using an IDL program I created, I plotted all of my galaxies as a function of Galactic Longitude and Latitude. The three graphs below represent a single block of GLIMPSE 3D data.It is important to note that in these graphs, the sizes of the ellipses were enlargened  for easier viewing . These galaxies are really not that big!

Conclusions

• Twelve square degrees of GLIMPSE 3-D data were searched for galaxies, resulting in 114  galaxy candidates (9.5 per square degree) and 159 other interesting objects.

• We  note that in our galaxy position graphs, we observe a galaxy detection gradient. As we move away from the galactic equator, we find more galaxies. So Galaxy detection is dependent on galactic latitude increasing from 4 per square degrees at b=1º to 12 per square degrees at b =3º.

• A silimar survey was conducted on 2MASS data. In comparison to their detection rate of 1-2 galaxies per square degree for galaxies brighter than 12.1 mag, our detection rate is two to four times as many galaxies per unit area.

• The 8 micron band was very intrusmental in finding these galaxies. Without it, I would approximate that we would have found only 50% of  our current galaxy candidates. In future observations, only the 3.6 and 4.5 micron bands will be at work. These bands may be able to recover some galaxies, but as we have discovered, galaxies tend to be most distinct in the 8 micron band.
  

• Automated searches for galaxies may not yield as many galaxies as was found by hand. We found that the process involved scaling the sky search segments several times, in an effort to reveal any hidden galaxies. We also had to make many judgement calls to differentiate galaxy candidates and other objects such as stars. Without the human factor, and automated galaxy search would yield irrelevant data.