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

The return to the hard state of GX 339-4 as seen by Suzaku