  A recent reanalysis of archival data has lead several authors to arrive at
strikingly different conclusions for a number of planet-hosting candidate
stars. In particular, some radial velocities measured using FEROS spectra have
been shown to be inaccurate, throwing some doubt on the validity of a number of
planet detections. Motivated by these results, we have begun the Reanalysis of
Archival FEROS specTra (RAFT) program and here we discuss the first results
from this work. We have reanalyzed FEROS data for the stars HD 11977, HD 47536,
HD 70573, HD 110014 and HD 122430, all of which are claimed to have at least
one planetary companion. We have reduced the raw data and computed the radial
velocity variations of these stars, achieving a long-term precision of $\sim$
10 m/s on the known stable star tau Ceti, and in good agreement with the
residuals to our fits. We confirm the existence of planets around HD 11977, HD
47536 and HD 110014, but with different orbital parameters than those
previously published. In addition, we found no evidence of the second planet
candidate around HD 47536, nor any companions orbiting HD 122430 and HD 70573.
Finally, we report the discovery of a second planet around HD 110014, with a
minimum mass of 3.1 Mjup and a orbital period of 130 days. Analysis of activity
indicators allow us to confirm the reality of our results and also to measure
the impact of magnetic activity on our radial velocity measurements. These
results confirm that very metal-poor stars down to [Fe/H]$\sim$ -0.7 dex, can
indeed form giant planets given the right conditions.
