  The microquasar GX 339-4 was observed by Suzaku five times, spaced by a few
days, during its transition back to the hard state at the end of its 2010-2011
outburst. The 2-10 keV source flux decreases by a factor ~10 between the
beginning and the end of the monitoring. Simultaneous radio and OIR
observations highlighted the re-ignition of the radio emission just before the
beginning of the campaign, the maximum radio emission being reached between the
two first Suzaku pointings, while the IR peaked a few weeks latter. A
fluorescent iron line is always significantly detected. Fits with a gaussian or
Laor profiles give statistically equivalent results. In the case of a Laor
profile, fits of the five data sets simultaneously agree with a disk
inclination angle of ~20 degrees. The disk inner radius is <10-30 R_g in the
first two observations but almost unconstrained in the last three. A soft X-ray
excess is also present in these two first observations. Fits with a multicolor
disk component give disk inner radii in agreement with those obtained with the
iron line fits. The use of a physically more realistic model, including a
blurred reflection component and a comptonization continuum, give some hints of
the increase of the disk inner radius but the significances are always weak.
Interestingly, the addition of warm absorption significantly improves the fit
of OBS1 while it is not needed in the other observations. The radio-jet
re-ignition occurring between OBS1 and OBS2, these absorption features may
indicate the natural evolution from a disk wind and a jet. The comparison with
a long 2008 Suzaku observation of GX 339-4 in a persistent faint hard state
where a narrow iron line clearly indicates a disk recession, is discussed.
