  We present the complete results of the planet search program carried out at
the ESO Coude Echelle Spectrometer (CES) on La Silla, using the Long Camera
from Nov. 1992 to April 1998. The CES survey has monitored 37 late-type (F8V -
M5V) stars in the southern hemisphere for variations in their differential
radial velocities (RV) in order to detect Doppler reflex motions caused by
planetary companions. This led to the discovery of the first extrasolar planet
in an Earth-like orbit around the young (ZAMS) and active G0V star iota
Horologii (Kuerster et al. 2000). Here we present the RV results for all survey
stars and perform a statistical examination of the whole data-set. Each star is
tested for RV variability, RV trends (linear and non-linear) and significant
periodic signals. Beta Hyi and eps Ind are identified as long-term,
low-amplitude RV variables. Furthermore, for 30 CES survey stars we determine
quantitative upper mass-limits for giant planets based on our long-term RV
results. We find that the CES Long Camera survey would have detected
short-period (51 Peg-type) planets around all 30 stars but no planets with m
sin i < 1 M_Jup at orbital separations larger than 2 AU. Finally, we
demonstrate that the CES planet search can be continued without applying
velocity corrections to the RV results coming from the currently installed Very
Long Camera at the CES.
