  We present here a reanalysis of the Spitzer Space Telescope phase curves of
the hot Jupiter WASP43 b, using the wavelet pixel-Independent Component
Analysis, a blind signal-source separation method. The data analyzed were
recorded with the InfraRed Array Camera and consisted of two visits at 3.6
$\mu$m, and one visit at 4.5 $\mu$m, each visit covering one transit and two
eclipse events. To test the robustness of our technique we repeated the
analysis on smaller portions of the phase curves, and by employing different
instrument ramp models. Our reanalysis presents significant updates of the
planetary parameters compared to those reported in the original phase curve
study of WASP43 b. In particular, we found (1) higher nightside temperatures,
(2) smaller hotspot offsets, (3) a greater consistency ($\sim$1 $\sigma$)
between the two 3.6~$\mu$m visits, and (4) a greater similarity with the
predictions of the atmospheric circulation models. Our parameter results are
consistent within 1 $\sigma$ with those reported by a recent reanalysis of the
same data sets. For each visit we studied the variation of the retrieved
transit parameters as a function of various sets of stellar limb-darkening
coefficients, finding significant degeneracy between the limb-darkening models
and the analysis output. Furthermore, we performed the analysis of the single
transit and eclipse events, and we examined the differences between these
results with the ones obtained with the whole phase curve. Finally we provide a
formula useful to optimize the trade-off between precision and duration of
observations of transiting exoplanets.
