  The Black Hole Binary source Swift J175.5-0127 remained in outburst for
$\sim$ 12 years from May 2005 to April 2017. For most part of the outburst, the
source remained in the Low Hard State (LHS) displaying transitions to softer
states only towards the end of the outburst for short periods of time. Quasi
periodic Oscillations (QPOs) were observed in the Power Density Spectrum (PDS)
only during the decay. A soft thermal component was required to model the
spectrum in LHS, which does not conform to the generally accepted disc
truncation theory. In this work, we attempt to obtain a clearer picture of the
accretion disc geometry by studying the QPO variability using frequency
resolved spectroscopy (FRS). We obtain the QPO rms spectrum of the source
during the bright-hard state and model it with physical components. We find
that the QPO rms spectrum can be described only by a Comptonisation component
with no contribution from the thermal disc. This indicates that the variability
observed in the PDS originates in the Comptonisation component and the
evolution of the QPOs is likely to be a result of localization of the
variabilities to different radii of the hot inner flow rather than disc
truncation. The minimal variation in disc parameters also points to the
existence of a stable disc throughout the outburst.
