The gravitational self-energy heuristically derived from Penrose's incompatibility measure in (2) has a free parameter . Here, we assumed without discussing that it is valued 1/(8), following Howl, Penrose, and Fuentes. However, if this parameter is incorporated into the mass distribution  (see eq. ( )), it would immediately imply that the Gaussian standard deviation RN should be multiplied by a factor  -1/3 to ensure that the integral over the mass distribution returns the nuclear mass, as expressed in (B.2). For the  = 1/(8), for example, all RN values in Table would be multiplied by 2.9. Any  value below 0.002 would suffice to bring the Gaussian distribution above the lower bound set by Donadi et al. At this point, however, in view of all uncertainties associated with the gravitational self-energy and radiation rate estimates, we believe that it is still too early to rule out the nuclear wave function as the measure of mass distribution width, especially considering that there is no obvious replacement for it.