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Visible colors (BVRI) are a reasonable proxy for real spectra of Centaurs andKuiper Belt Objects, which are rather linear in this range. Colors providelimited information but remain the best tool to study the bulk surfaceproperties. We explore recurrent effects in the study of visible colors: i) howa correlation could be missed or weakened as a result of the data error bars,ii) the "risk" of missing an existing trend because of low sampling, and thepossibility of making quantified predictions on the sample size needed todetect a trend at a given significance level, iii) the use of partialcorrelations to distinguish the mutual effect of two or more parameters, andiv) the sensitivity of the "reddening line" tool to the central wavelength ofthe filters used. We have compiled the visible colors of about 370 objectsavailable in the literature and carried out an analysis per dynamical family.Our results show how a) data error bars impose a limit on the detectablecorrelations regardless of sample size and that therefore, once that limit isachieved, it is important to diminish the error bars, but it is pointless toenlarge the sampling with the same or larger errors; b) almost all dynamicalfamilies still require larger samplings to ensure the detection of correlationsstronger than 0.5; c) the correlation strength between (V-R) vs. (R-I) issystematically lower than the one between (B-V) vs. (V-R) and is not relatedwith error-bar differences between these colors; d) it is statisticallyequivalent to use any of the different flavors of orbital excitation orcollisional velocity parameters regarding the color-inclination correlation ofclassical KBOs whereas the inclination and Tisserand parameter relative toNeptune cannot be separated from one another; and e) classical KBOs are theonly dynamical family that shows neither (B-V) vs. (V-R) nor (V-R) vs. (R-I)correlations.

Reanalyzing the visible colors of Centaurs and KBOs: what is there and what we might be missing