  This paper presents a physical distance to all radial events in a homogeneous
and isotropic universe as a transform from Friedman-Lemaitre-Robertson-Walker
(FLRW) coordinates, the model that solves the Einstein Field equation for an
ideal fluid. Any well behaved transform is also a solution. The problem is
relating the coordinates of the transform to observables. In the present case
the objective is to find T,R on a stationary frame that has the R be a physical
observable for all distances. We do this by working backwards, assuming the
form of the metric that we desire, with some undetermined coefficients. These
coefficients are then related to the partial derivatives of the transform. The
transformed coordinates T,R are found by the integration of partial
differential equations in the FLRW variables. We show that dR has the same
units as the radial differential of the FLRW metric, which makes it observable.
We develop a criterion for how close the transformed T comes to an observable
time. Close to the space origin at the present time, T also becomes physical,
so that the stationary acceleration becomes Newtonian. We show that a galactic
point on a R,T plot starts close to the space origin at the beginning, moves
out to a physical distance and finite time where it can release light that will
be seen at the origin at the present time. Lastly, because the observable R has
a finite limit at a finite T for t = 0 where the galactic velocity approaches
the light speed, we see that the universe filled with an ideal fluid as seen on
clocks and rulers on the stationary frame has a finite extent like that of an
expanding empty universe, beyond which are no galaxies and no space.
