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tokens: those in A2, but there are too few points in A3. Statistically, the difference in the slope between A2 and A3 is not significant, although, neither is that between A1 and A3. 5. DISCUSSION The galactic conformity is very marginal in the central area of the Virgo Cluster (A1), which seems to be similar to the result in WHL J085910.0+294957 from Lee et al. ( 2014 ). Since the analysis in Lee et al. ( 2014 ) was limited to the central area within 500 kpc radius, the two clusters (Virgo and WHL J085910.0+294957) commonly show only weak signals of small-scale conformity in their central areas (∼2 σ significance). On the other hand, the signal of small-scale conformity in A2 appears to be more obvious, showing significance close to 3 σ . In the case of the outermost area A3, as mentioned in the previous section, the signal is very weak due to the insufficient size of the sample. It is noted that the correlation coefficient in A3 is as large as 0.44, which is similar to the value in A2, while that in A1 is only 0.27. This is not a decisive evidence of small-scale conformity in A3, but it shows a possibility that a clearer signal of conformity may be detected if a larger sample is available. In this paper, however, because the uncertainty for the result in A3 is too large, we will focus on the results in A1 and A2. These results show that small-scale conformity is weak or somewhat ambiguous in the inner region (roughly within the virial radius), while it seems to be more obvious in the outer region of the Virgo Cluster. Note that, in Section 3.1 , the average standard deviation of color indices in faint companions around a given bright galaxy is 0.116. This value is only approximately one fourth of the distribution over the entire sample, which ranges from 0.25 to 0.70. This small value of the average standard deviation of color indices implies that the faint companion galaxies in a possible group tend to have similar properties rather than have randomly mixed properties, which is consistent with the expected small-scale conformity. Lee et al. ( 2014 ) suggested three scenarios regarding the origin of the small-scale galactic conformity in a cluster. The first is the “tidal dwarfs” scenario, in which the massive galaxies are partially torn out by tidal interactions with many other galaxies (harassment) or the cluster potential itself, forming many low-mass galaxies that may be the faint companions we observe. The properties of these low-mass galaxies must be similar to their host massive galaxy because they have been a single galaxy. If this scenario is correct, the conformity may be detected better in the inner region than in the outer region of a cluster, because the tidal force by a cluster is stronger in the inner region and more numerous massive galaxies exist in the inner region of a typical cluster, which may cause stronger harassment. However, this does not agree with our results that show an exactly opposite trend. Furthermore, the