  In this paper we report on Expanded Very Large Array radio and Chandra and
Swift X-ray observations of the outburst decay of the transient black hole
candidate MAXI J1659-152 in 2011. We discuss the distance to the source taking
the high inclination into account and we conclude that the source distance is
probably 6+-2 kpc. The lowest observed flux corresponds to a luminosity of
2x10^31 (d/6 kpc)^2 erg/s This, together with the orbital period of 2.4 hr
reported in the literature, suggests that the quiescent X-ray luminosity is
higher than predicted on the basis of the orbital period -- quiescent X-ray
luminosity relationship. The relation between the accretion and ejection
mechanisms can be studied using the observed correlation between the radio and
X-ray luminosities as these evolve over an outburst. We determine the behaviour
of MAXI J1659-152 in the radio -- X-ray diagram at low X-ray luminosities using
the observations reported in this paper and at high X-ray luminosities using
values reported in the literature. At high X-ray luminosities the source lies
closer to the sources that follow a correlation index steeper than 0.6-0.7.
However, when compared to other sources that follow a steeper correlation
index, the X-ray luminosity in MAXI J1659-152 is also lower. The latter can
potentially be explained by the high inclination of MAXI J1659-152 if the X-ray
emission comes from close to the source and the radio emission is originating
in a more extended region. However, it is probable that the source was not in
the canonical low-hard state during these radio observations and this may
affect the behaviour of the source as well. At intermediate X-ray luminosities
the source makes the transition from the radio underluminous sources in the
direction of the relation traced by the 'standard' correlation similar to what
has been reported for H1743-322. (abridged)
