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tokens: in the selection of the most basic data sets, namely, the HJD dates of the midpoints of the X-ray flares and of the peak points of the IR flares that were taken as the events to be analyzed. This is why additional observations and analysis by different people are required in order to strengthen the evidence for the operation of the two pacemakers, or to refute this claim. The numbers S X = 0.1976 (Section 4.1 ) and (Section 6.2.3 ) should be compared with 0.2887, the StD of a rectangular distribution over the [−0.5, 0.5] interval. It seems that the grouping of the X-ray flares, and even more so of the NIR ones, around tick marks of the corresponding pacemakers is not very tight. The model presented in Section 8 suggests that the dispersion of the flare times around the pacemaker tick marks is inherent to the flare phenomenon itself. Rather than being well concentrated around some fixed phase of the pacemaker cycle, the flare events occur within a wide section of it. Therefore, if future observations are to strengthen the evidence for pacemakers in the Sgr A* system, it will not come in the form of diminishing the value of the S parameter as longer series of detected flare times are considered. Further evidence could come from finding in future new independent sets of observations the effect of two pacemakers of the same frequencies F X and F IR , but not necessarily with smaller dispersions. On the theoretical side, the model suggested here relies on post-Newtonian equations applied on a highly relativistic system. Such an approach could be too simplistic. For one thing, there is, so far, no observational hint regarding the rate of rotation of the BH at the center. If it is a fast rotator, the Schwarzschild metric itself is not an appropriate description of spacetime in its vicinity. But even within the context of the Schwarzschild metric it is yet to be proven that the Paczynsky–Witta potential function is an adequate approximation in the extreme conditions of existence of the alleged star. Furthermore, the equations in Table 4 are strictly consistent only for e ≈ 0, implying, according to Table 5 , that M ≅ 4.4. This value lies at the extreme end of the uncertainty in the value of M as estimated by other, more direct measurements. Also, as noted in Section 8.3.2 , P orb must be understood as referring to a mean value of the sidereal orbital cycle of the star, and the NIR pacemaker frequency F IR uncovered in the data is the mark of this mean value. In Equations (5) and (6), the relevant parameter x should represent an instantaneous distance r of the star from the BH that is varying between the extreme values and at the apicyclic frequency. For e > 0, the use of the constant a value in these equations may therefore be a poor approximation. Also for e > 0.02 the orbit leads the star to within the ISCO circle around the BH where the post-Newtonian approximation may break down. It may therefore be that in order to place the model on firmer