  We report the results from an X-ray and near-infrared observation of the
Galactic black hole binary 4U 1630--47 in the very high state, performed with
{\it Suzaku} and IRSF around the peak of the 2012 September-October outburst.
The X-ray spectrum is approximated by a steep power law, with photon index of
3.2, identifying the source as being in the very high state. A more detailed
fit shows that the X-ray continuum is well described by a multi-color disc,
together with thermal and non-thermal Comptonization. The inner disc appears
slightly truncated by comparison with a previous high/soft state of this
source, even taking into account energetic coupling between the disc and
corona, although there are uncertainties due to the dust scattering correction.
The near-infrared fluxes are higher than the extrapolated disc model, showing
that there is a contribution from irradiation in the outer disk and/or the
companion star at these wavelengths. Our X-ray spectra do not show the Doppler
shifted iron emission lines indicating a baryonic jet which were seen four days
previously in an XMM-Newton observation, despite the source being in a similar
state. There are also no significant absorption lines from highly ionized irons
as are seen in the previous high/soft state data. We show that the increased
source luminosity is not enough on its own to make the wind so highly ionized
as to be undetectable. This shows that the disc wind has changed in terms of
its launch radius and/or density compared to the high/soft state.
