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 ^ { -1 } 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 M _ { \mbox { \scriptsize { Jup } } } 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 .