Lauer and Postman ,  presented distances of the Brightest Cluster Galaxies (BCG's) of a sample of 119 Abell ,  clusters to cz < 15,000 km s-1. Following work of  and , they found that the luminosity L of these galaxies within an aperture of radius 10 h-1kpc correlated with the logarithmic slope of the surface brightness profile . This yields a distance indicator with an error of 15 - 20%, depending on the value of . Their sample was full-sky (or as much so as the zone of avoidance would allow) and volume-limited, and great effort was taken to obtain and reduce the data as uniformly as possible.
To their great surprise, the sample showed a strong signature of bulk flow, with an amplitude of 764 ± 160 km s-1 , towards l = 341°, b = +49°. This was much larger than one might expect, given the effective depth of the sample of 8000 km s-1; indeed,  and  both showed that a bulk flow with the statistical significance of that of Lauer-Postman ruled out a whole series of cosmological models at the > 95% confidence level.
As a follow-up to this survey, Tod Lauer, Marc Postman and I are extending the sample to cz = 24, 000 km s-1. The sample now consists of 529 BCG's, an increase of more than a factor of 4 from the original l19 (the Abell cluster catalog has the beautiful feature of being volume-limited, at least to moderate redshifts, and this increase in number of clusters is almost exactly the increase in volume). The photometry for this sample is all in hand, and redshifts for all BCG's are nearly complete. Barring unseen systematic effects (which we've worked very hard to minimize), we should be able to measure the bulk flow on these scales to 130 km s-1 or so. We have also measured velocity dispersions for the BCG's, with preliminary indications that this reduces the scatter in the L - relation, in analogy to the Dn - relation. The sky distribution of this sample is shown in Fig. 4a.
Figure 4. a. The BCG sample with z < 0.08. The substantial region devoid of clusters in the general direction of the Galactic center is due to the difficulty in finding clusters in regions of high stellar density, and is a general feature of the Abell catalogue. b. The sky distribution in Galactic coordinates of galaxies in the Sb, Sc shell sample at cz 6000 km s-1.
As Fig. 3, and the controversy that the Lauer-Postman result have engendered, make clear, the comparison of various measurements of bulk flows with one another is non-trivial.
The velocity field has components on all scales; it is not purely dipolar in nature. The geometry of any given sample couples to various multipoles of the velocity field (the sparser the sampling is, the larger the extent to which this is true), and therefore not all bulk flow measurements measure the same quantity . Thus  published a bulk flow analysis of 13 Type 1a supernovae, which appear to be standard candles to an accuracy of ~ 5% . Their results were inconsistent with that found by Lauer & Postman at the 99% confidence level, assuming that the velocity field was describable by a pure bulk flow plus small-scale incoherent noise. However, the two surveys sample space really very differently, and therefore are very differently sensitive to components of the velocity field on scales smaller than the dipole. Watkins & Feldman  calculated the expectation value of the dot product of the bulk flows each measured, normalized by the expectation value of each bulk flow separately:
This quantity, a sort of dimensionless covariance between the two bulk flow measurements, would be close to unity if these two surveys were indeed measuring the same quantity. The results depend on the power spectrum assumed. If one assumes "realistic" power spectra, the quantity is of the order of 10%, but as mentioned above, the Lauer-Postman result is inconsistent with most ordinary power spectra. Watkins & Feldman thus also consider a power spectrum with a huge bump at large scales; in such a model, the relative importance of small-scale components of the velocity field is reduced, but the quantity is still only 35%.