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tokens: it is as follows: (a) the parameter h eff is sampled, marginalized over the velocity field; (b) the conditional probability of the parameter σ NL is drawn with the other parameters fixed; (c) a constrained realization of the density field is drawn assuming a ΛCDM power spectrum (Hoffman Ribak 1991 ); (d) a new set of distances is established from the sampled constrained realization with probabilities set by the current values of h eff , σ NL , and the velocity field, within priors on the distances. The process is carried through ∼10 3 MCMC steps until convergence. The procedure has been carried out on multiple constrained realizations and mock catalogs. With the current analysis, Graziani et al. ( 2019 ) find h eff = 1.02 ± 0.01 and σ NL = 280 ± 35 km s −1 . The resultant model makes predictions for the morphology and motions of structure locally within the ΛCDM framework and linear perturbations. Our present interest is in voids. It will be asked to what degree the overall model is in agreement with the excellent knowledge we have of the motions of very nearby galaxies. 2. Morphologies of Nearest Voids The Local Void does not have a simple shape. Moreover, as the void is followed to shallower levels it merges with adjacent voids, as part of a continuous network that extends beyond the volume that can currently be mapped. The three-dimensional interplay between complex high- and low-density structures is visually confusing. We should not have the ambition to get into great detail. As a prelude, previous efforts to identify nearby voids can be mentioned, derived from regions of emptiness in maps of the distribution of galaxies in redshift surveys. Among the earliest were the seminal studies of the Boötes Void by Kirshner et al. ( 1981 ) and the void in front of the “Great Wall” Coma and Abell 1367 clusters (Gregory Thompson 1978 ). On very large scales there is the pioneering work by Batuski Burns ( 1985 ) and Einasto et al. ( 1994 ) on the concentrations and absences of rich clusters. More nearby, and pertaining to the distribution of individual galaxies, of note is the work of Kauffmann Fairall ( 1991 ) and Fairall ( 1998 ). The latter gives a list of 33 void-like regions within 8500 km s −1 . Elyiv et al. ( 2013 ) have produced a more quantitatively rigorous catalog of 89 voids within 3000 km s −1 ; spherical regions with no known galaxies brighter than M K = −18.4. Typically these entities are modest in size, with radii ∼6 Mpc. It is well documented that voids network, and their dimensions as constrained by the exclusion of galaxies depend on the intrinsic properties of the galaxy samples. Sparse filaments of dwarf galaxies can snake through regions devoid of bright galaxies. This phenomenon has particularly been noted by Lindner et al. ( 1995 ) and Pustilnik et al. ( 2019 ) within the volume that attracts our attention. The linkage of the region under consideration including the Local Void to very extensive voids has been claimed by