  We present the results obtained from an X-ray timing study of the new black
hole candidate (BHC) Swift J1727.8-1613. The work is based on Hard X-ray
Modulation Telescope (Insight-HXMT) observations carried out during the 2023
outburst. Prominent type-C low-frequency Quasi-periodic Oscillations (LFQPOs)
are detected throughout the observations. With the substantial effective area
of the Insight-HXMT at high energies, we examine the energy dependence of
various parameters, including the centroid frequency, fractional rms, and phase
lags of the type-C QPOs. Our findings align closely with those observed in
high-inclination systems. During the initial stage of the outburst, a peaked
noise component is also detected, the frequency of which is highly correlated
with the LFQPO frequency, aligning with the Psaltis-Belloni-van der Klis (PBK)
relation. By assuming that the peaked noise originates from the precession of
the accretion disc, the spin of this source can be constrained. Our results
suggest that this source may possess a high spin.
