LEAST ACTION SOLUTION OF LARGE SCALE \\STRUCTURE
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**Session 13 -- Large Scale Structure**
*Oral presentation, Monday, 10:30-12:00, Zellerbach Playhouse Room*

## [13.03] LEAST ACTION SOLUTION OF LARGE SCALE \\STRUCTURE

*E.J. Shaya (U of Maryland), P.J.E. Peebles (U. of Princeton), R.B. Tully (U. of Hawaii)*
Techniques for using the Least Action Principle for calculating the
orbits of many hundred of groups of galaxies from the Big Bang to the
present will be described. Complications in finding a robust best fit
analysis leads us to solve for the positions of all groups given the
present recessional velocities and then calculate a Chi-square on
resulting distances to determine best input parameters. Using distance
indicators within 3,000 km/s and the mass distribution of the Nearby
Galaxy Catalog our results thus far indicate best fit with bias
parameter b = 3.0 $\Omega_0^{0.6}$, that is b = 3.0 if $\Omega_0$ = 1.0
and $\Omega_0$ = 0.16 if b = 1.0. This assumes the relation of M/L$_B$
ratio = 1270 h $\Omega_0$. The Chi-square is remarkably flat along this
($\Omega_0$, bias) trajectory. The effects of adding Abell Cluster
catalogs and IRAS maps to describe the mass distribution at larger
distances will also be described.

**Monday
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