  The timing properties of the Z-type low-mass X-ray binaries provide insights
into the emission components involved in producing the unique Z-shaped track in
the hardness-intensity diagrams of these sources. In this work, we investigate
the AstroSat and NICER observations of the GX 340+0 covering the complete
'Z'-track from the horizontal branch (HB) to the extended flaring branch (EFB).
For the first time, we present the Z-track as seen in soft X-rays using the
AstroSat/SXT and NICER (the soft colour is defined as a ratio of 3-6 keV to
0.5-3 keV). The shape of the track is distinctly different in soft X-rays,
strongly suggesting the presence of additional components active in soft
X-rays. The detailed timing analysis revealed significant quasi-periodic
oscillation throughout the HB and the normal branch (NB) using LAXPC and the
first NICER detection of 33.1 +/- 1.1 Hz horizontal branch oscillation (HBO) in
3-6 keV. The oscillations at the HB/NB vertex are observed to have higher
frequencies (41-52 Hz) than the HB oscillations (16-31 Hz) and NB oscillations
(6.2-8 Hz) but significantly lower rms (~1.6%). The HB oscillation is also
limited to the energy range of 3-20 keV, indicating an association of HBO
origin with the non-thermal component. It is also supported by earlier studies
that found the strongest X-ray polarisation during HB.
