PCA results in the Bulge field (A. Saha et al. 2019), which includes many variable stars. We show visits 428030 (left) and 429041 (right) on CCD 28 in the r band, and plot the sources that have PC1 quantile larger than 0.5; the marker opacity is proportional to the PC1 quantile of each source. The corresponding exposure times in MJD are 57115.264 and 57116.403 (the interval is ∼27 hr). We annotate the objects recorded in SIMBAD (M. Wenger et al. 2000). Their stellar types can be identified by name. “OGLE BWC V154” corresponds to “OGLE-BLG-ECL-27776” studied earlier (light curves in Figure 10). “BMB” indicates AGB stars (V. M. Blanco et al. 1984), and “ISOGAL-P J180302.8-295938” is an AGB star (D. K. Ojha et al. 2003) as well. Some short-period stars were also captured because of the timing of their phases, e.g., those names beginning with “OGLE BLG-ECL.” The source detection depends on weather and instrumental conditions. The detected sources without annotation could be noise (especially near CCD edges or saturated stars), or previously uncataloged real objects.