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tokens: the point sources matched between the two shortest wavelength IRAC bands. To illustrate the locations of detected sources in our catalog, we present in Figs. 5 through 9 the 3.6 m image of each galaxy with the positions of detected sources overplotted, followed by an image of the galaxy without sources shown. For each galaxy, red points denote the location of point sources not likely to be associated with the galaxy, while green points demarcate the regions inside isophotes for the Kron radius for all galaxies but NGC 2366, where the isophote described in de Vaucouleurs et al. (1991) was used. Consequently, the green points are more probably actual sources associated with each galaxy. Figures 10 through 14 show color-magnitude diagrams (CMDs) of [3.6] versus [3.6][4.5] for each galaxy. The points follow the color scheme from the images showing each galaxy, with green points representing sources within the isophotes for with each galaxy, and red points sources in the field of each galaxy. For each magnitude bin, the average uncertainty was computed for both the [3.6] magnitude and [3.6][4.5] color, and is plotted as an ellipse on the left hand side of the plot. For reference, lines are drawn to show the completeness limit of mag and the color [3.6][4.5] = 0, where most stars lie in the plot. In terms of absolute magnitudes, the [3.6] limit corresponds to detections of all objects brighter than in every galaxy. One other interesting feature in the plot was explained by Khan et al. (2015c) . For both NGC 55 and NGC 253, the two galaxies with the most sources of those studied in this work, one can see a “break” at about the same magnitude as the completeness limit. This feature is representative of the two different populations in the photometry, one physically associated with the galaxy, and another simply sharing the same region of sky. Khan et al. (2015c) calls the second population “contaminants”. This population contains foreground stars near the [3.6][4.5] color of 0, some Milky Way Halo late-type giants and unresolved background galaxies in other regions of the CMD. Red supergiants (RSGs) have been empirically shown to exist in the region of negative color space ( Bonanos et al. 2009 , 2010 ). This is due to a suppression of the flux in the 4.5 m photometry owing to molecular bands, most prominently CO ( Verhoelst et al. 2009 ). However, spectroscopic investigations into the individual stellar components of Local Group dwarf irregular galaxies have discovered 15% of new RSGs at positive colors in CMDs for those galaxies ( Britavskiy et al. 2014 , 2015 ). Fig. 10 Colormagnitude diagram for sources in the field of NGC 55. All photometrically measured sources are marked with a red dot, while those residing within the isophotal limits of the galaxy are represented by green dots. Overplotted are lines denoting the limiting magnitude of 18.0 and a [3.6][4.5] color of 0. On the left are ellipses corresponding to the average uncertainty for