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We have combined the available distances of galaxies to produce a unified view of galaxy motions within the so-called great attractor (GA) region. The current data base includes 253 galaxies that lie within 40ᵈeg^ of the nominal GA center, 3. 5 times the number of galaxies in the original Lynden- Bell et al. survey. The motions of galaxies in all data sets support the basic picture of a high-velocity flow as described by Lynden-Bell et al. and Faber and Burstein. Within 40ᵈeg^ of the center of this region, the flow velocity rises outward from the Local Group, reaching a maximum of ~1000 km s^-1^ at a distance of ~2000 km s^-1^, then decreasing to near zero at a distance of 4500 km s^-1^. This latter distance is close to the centroid of the radial velocity distribution observed for galaxies in this region by Dressler, suggesting that this region can plausibly be equated with the center of mass of the GA. Although the present observations go deeper than the original Lynden-Bell et al. data, an unambiguous signature of infall by galaxies on the backside of the GA has not yet been obtained, possibly because of Malmquist-bias selection effects. A previous model of the Centaurus clusters as two closely interacting clusters is examined in detail using distances to 47 galaxies previously identified as cluster members. Although the existence of two separate clusters is blurred in the present sample, the majority of galaxies are clearly on the near side of the GA center, falling into the GA. Checks are made for systematic errors in the motions of ellipticals that are correlated with cluster richness, structural parameters of the galaxies, or errors in Galactic absorption. Two small effects are found, but neither has a significant effect on the observed large-scale motions. Other evidence strongly supporting the current distance indicators is reviewed, and arguments are presented in favor of the cosmic background radiation defining the correct velocity rest frame. The basic conclusion of this study is therefore to affirm the fundamental correctness of the present body of measured galaxy motions.
Burstein et al. (Tue,) studied this question.