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tokens: the UDGs: to −15.5 mag, and M * = 5 × 10 7 to 5 × 10 8 M ⊙ . The slanted solid lines represent the varying surface brightness, = 23, 24, 25, 26, and 27 mag arcsec −2 (from left to right). For given surface brightness, the larger the UDGs are, the brighter (more massive) they are. The stellar masses of the UDGs are much lower than those of the bright red sequence galaxies. Figure 6. Left and middle panels: circularized effective radii vs. r ′-band absolute magnitudes (lower x -axes) and stellar masses (upper x -axes) of the UDGs and other galaxies in Abell S1063, Abell 2744, and the parallel fields. Symbols are the same as in Figure 5 . Solid lines represent isosurface brightness magnitudes of = 23, 24, 25, 26, and 27 mag arcsec −2 from left to right. Right panels: red line histograms are for the UDGs and LSB dwarfs in Abell S1063 and Abell 2744, and gray line histograms are for the UDGs in Coma. The numbers and dotted lines represent mean values of Sérsic index n for UDGs. In the right panels of Figure 6 we plotted the histograms of effective radii for Abell S1063 and Abell 2744 in comparison with that of the Coma UDGs (Yagi et al. 2016 ). The mean values, kpc for Abell S1063 and kpc for Abell 2744, are similar to that of the MW-sized UDGs in Coma, kpc. The histograms of the combined sample of UDGs and LSB dwarfs are similar to those of the large UDGs in Coma. 3.5. Spatial Distributions of the UDGs Figure 7 (left panels) displays the spatial distribution of the UDGs, LSB dwarf galaxies, and bright red sequence galaxies in the Abell S1063 and Abell 2744 fields. The circles in the left panels represent the boundaries of the radial bins used for deriving radial number density profiles. We excluded the central circular region in the UDG survey because of high surface brightness of the central galaxy. Figure 7. Spatial distributions (left panels) and radial number density profiles corrected for detection completeness (right panels) of the UDGs (large red starlets), LSB dwarfs (small red starlets), and bright red sequence galaxies (blue circles) in Abell S1063 and Abell 2744. Black dots denote the compact galaxies with . The circles in the left panels represent the boundaries of the radial bins used for deriving radial number density profiles. The central gray circle denotes the region not used for the UDG survey. Yellow starlets in the right panels are for the sum of the UDGs and LSB dwarfs. Yellow and cyan regions represent the cluster and parallel fields, respectively. We derived the radial number density profiles of the galaxies, subtracting the background contribution using the data for the HXDF. As the center for the radial profiles we adopted the center of the cD galaxy in Abell S1063 and the center of CN-1 in Abell 2744. Note that Lee Jang ( 2016 ) adopted the center of CN-2 at the southeast of CN-1, which is the brightest galaxy in the HST field of Abell 2744, for deriving radial number density profiles of the point sources (mostly