  We present the results of multicolour $UBVR_{\text{C}}I_{\text{C}}JHK$
photometry, spectroscopic analysis and spectral energy distribution (SED)
modelling for the post-AGB candidate IRAS 02143+5852. We detected Cepheid-like
light variations with the full peak-to-peak amplitude $\Delta V\sim0.9$ mag and
the pulsation period of about 24.9 d. The phased light curves appeared typical
for the W Vir Cepheids. The period-luminosity relation for the Type II Cepheids
yielded the luminosity $\log L/L_{\odot}\sim2.95$. From a low-resolution
spectrum, obtained at maximum brightness, the following atmospheric parameters
were determined: $T_\text{eff}\sim7400$ K and $\log g\sim1.38$. This spectrum
contains the emission lines H$\alpha$, BaII $\lambda$6496.9, HeI $\lambda$10830
and Pa$\beta$. Spectral monitoring performed in 2019-2021 showed a significant
change in the H$\alpha$ profile and appearance of CH and CN molecular bands
with pulsation phase. The metal lines are weak. Unlike typical W Vir variables,
the star shows a strong excess of infrared radiation associated with the
presence of a heavy dust envelope around the star. We modelled the SED using
our photometry and archival data from different catalogues and determined the
parameters of the circumstellar dust envelope. We conclude that IRAS~02143+5852
is a low-luminosity analogue of dusty RV Tau stars.
