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tokens: Drake et al. 2009 ), retrieved from the Catalina Surveys Data Release 2. Between the WISE and NEOWISE-R epochs, the source dimmed by approximately 1 mag in both W1 and W2 , with further, lower amplitude variability observed between the epochs of each survey independently. In contrast, there is no strong optical variability observed by CRTS. This is consistent with both spectroscopic classifications, as in both an intermediate-type and a type 2 AGN, the optical emission is dominated by the host galaxy. The large drop in mid-IR fluxes suggests that the change in spectroscopic classification is most likely due to a decrease in accretion rate rather than a change in obscuration. Figure 10. Light curve of WISEA J142846.71+172353.1 in the optical from CRTS (green points) and in the WISE bands W1 (purple points) and W2 (red points). All magnitudes are shown in the AB system to limit the dynamic range of the vertical axis. For W1 and W2 , the small circles show the individual frame photometry in the AllWISE and NEOWISE-R surveys. The large circles show the median of each epoch. 5. Comparisons with Other Surveys As mentioned earlier, a number of AGN catalogs already exist in the literature that are similarly as large as ours. In this section, we compare with a number of them in order to characterize how they differ from our R90 and C75 catalogs as well as to assess what the relative completeness and biases are. We consider both mid-IR selected catalogs as well as catalogs selected in different wavelength ranges and, hence, affected by very different systematics. 5.1. Secrest et al. (<xref ref-type="bibr" rid="apjsaaa00abib79">2015</xref>) WISE AGN Catalog Recently, Secrest et al. ( 2015 ) presented an all-sky AGN catalog selected purely on their WISE colors, based on the selection criteria of Mateos et al. ( 2012 ). These criteria require a detection in the W3 band. A13 showed these criteria to be less reliable than the R90 criterion at faint W2 magnitudes, though they are equally reliable at brighter magnitudes. The trade-off is that the Mateos et al. ( 2012 ) selection criteria are more complete at faint W2 magnitudes than the R90 selection. As noted by Jarrett et al. ( 2011 ), requiring a detection in W3 can be particularly useful near the high survey coverage areas at the EPs, where W1 and W2 are confusion limited, and the lower source density W3 band provides robust photometry. However, the lower sensitivity of the W3 band restricts the AGN sample size created using the selection criteria of Mateos et al. ( 2012 ). Additionally, Secrest et al. ( 2015 ) required a 5 σ detection in all three WISE bands, creating a robust catalog at the cost of decreasing the number of sources selected. Indeed, the full catalog presented by Secrest et al. ( 2015 ) consists of 1,354,775 sources, and once we apply the same spatial filters as described in Section 3.1 , the catalog is reduced by 15% to 1,140,022 sources. This is roughly 25% of the sources in our R90