  CONTEXT: The recent discovery of three giant planets orbiting the extremely
metal-poor stars HIP11952 and HIP13044 have challenged theoretical predictions
of the core-accretion model. According to this, the metal content of the
protoplanetary disk from which giant planets are formed is a key ingredient for
the early formation of planetesimals prior to the runaway accretion of the
surrounding gas.
  AIMS: We reanalyzed the original FEROS data that were used to detect the
planets to prove or refute their existence, employing our new reduction and
analysis methods.
  METHOD: We applied the cross-correlation technique to FEROS spectra to
measure the radial velocity variation of HIP13044 and HIP11952. We reached a
typical precision of $\sim$ 35 $ms^{-1}$ for HIP13044 and $\sim$ 25 $ms^{-1}$
for HIP11952, which is significantly superior to the uncertainties presented
previously.
  RESULTS: We found no evidence of the planet orbiting the metal-poor
extragalactic star HIP13044. We show that given our radial velocity precision,
and considering the large number of radial velocity epochs, the probability for
a non-detection of the radial velocity signal recently claimed is lower than
10$^{-4}$. Finally, we also confirm findings that the extremely metal-poor star
HIP11952 does not contain a system of two gas giant planets. These results
reaffirm the expectations from the core-accretion model of planet formation.
