  We present Fabry-Perot absorption-line spectroscopy of the SB0 galaxy NGC
7079. This is the first use of Fabry-Perot techniques to measure the
two-dimensional stellar kinematics of an early-type disk galaxy. We scan the
infrared CaII line using the Rutgers Fabry-Perot (RFP), to obtain kinematic
data extending to $I$-band surface brightness $\mu_I \simeq 21$ mag./arcsec^-2,
in a field of radius $\sim 40\arcsec$. The kinematic data, consisting of
line-of-sight velocities and velocity dispersions, are in good agreement with
data obtained along the major axis of the disk with standard slit spectroscopy.
Comparison of the exposure times required for slit and RFP spectroscopy to
reach the same limiting magnitude shows that the RFP is significantly more
efficient for mapping absorption-line galaxy kinematics. We use the velocity
data, together with our own deep broad-band photometry,to measure the bar
pattern speed, $\Omega_p$, of NGC 7079 with the model-independent
Tremaine-Weinberg (TW) method. We find $\Omega_p = 8.4 \pm 0.2$ km/s/arcsec;
this is the best-constrained pattern speed ever measured for a bar using the TW
method. From the rotation curve, corrected for asymmetric drift, we calculate
the co-rotation radius and find that the bar ends just inside this radius. The
two-dimensional character of these data allow us to show that the TW method is
sensitive to errors in the position angle (PA) of the disk. For example, a PA
error of $2\degrees$ can give errors $\sim \pm 25%$ in $\Omega_p$.
