We summarise results for the predicted density and peculiar velocity fields from the PSCz survey , consisting of redshifts for 15,000 IRAS galaxies covering 84 % of the sky to a depth of 25 , 000 { km s } ^ { -1 } .
We have used a generalisation of the Path Interchange Zeldovich Approximation technique to determine the velocity field ; the most remarkable feature being a coherent large-scale flow along the baseline connecting the Local Supercluster , Centaurus and the Shapley Concentration .
Comparison of the predicted and observed bulk flows gives a value of \beta = 0.50 \pm 0.1 .

We re-examine the PSCz dipole , with improved redshift completeness at low-latitudes and using PIZA to estimate real-space distances .
We find the dipole to be stable between 80 and 180 h ^ { -1 } { Mpc } , although there appears to be a significant contribution to the dipole around 200 h ^ { -1 } { Mpc } .
The overall misalignment with the CMB dipole remains at 20 ^ { \circ } .
The implied value of \beta depends on the exact treatment ; we derive values in the range \beta = 0.40 - 0.55 with statistical error \pm 0.1 .

We also present the density field and a preliminary dipole analysis from the almost completed Behind The Plane survey , which extends the PSCz to cover 93 % of the sky including the proposed core of the Great Attractor .
We find a density peak at ( 325 , -5 , 3500 { km s } ^ { -1 } ) , about half as massive as Centaurus or Pavo-Indus , and forming part of a continuous filament linking them across the Plane .
We also find evidence for a much larger ‘ Greater Attractor ’ directly behind the GA , at a distance of 125 h ^ { -1 } { Mpc } , and more massive than the Shapley concentration .

At large distances the dipole direction is in much improved agreement with the CMB : at 250 - 300 h ^ { -1 } { Mpc } , the misalignment is only 5 - 10 ^ { \circ } , and this is consistent with the shot noise errors .
The J _ { 3 } -weighted dipole , which in principal is expected to agree better with the CMB , gives a misalignment of 13 ^ { \circ } .
The dipole direction is somewhat dependent on the corrections made for the redshift incompleteness , and may also be affected by unquantified incompleteness in the BTP survey close to the Galactic Centre .
The dipole amplitude implies a value for the parameter \beta of 0.44 \pm 0.1 .
Values much larger than \beta = 0.5 , while not formally ruled out , cause very unlikely-looking rocket effects .