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The similarity in physical conditions in winds of low-mass post-asymptoticgiant branch stars and evolved massive stars leads to the appearance of aninteresting phenomenon of spectral mimicry. Due to that the discovery of everynew star with Wolf--Rayet spectrum requires special study of its evolutionarystatus before it may be included in the list of Galactic Wolf--Rayet (WR)stars. A couple of years ago LAMOST J040901.83+323955.6 (hereafter J0409+3239)was selected as a WR star in LAMOST spectroscopic database by machine learningmethods. In this work we investigated its evolutionary status. Analyzing thespatial location of J0409+3239, in the Galaxy and its position in thecolor-magnitude diagram we concluded what J0409+3239, is instead a low massobject with WR phenomenon. Its luminosity is $L*=1000 L_\odot$ and effectivetemperature $T_{\rm eff}$=40,000 K. Using new and archival photometric data wedetected irregular variability on time scales from hours to tens of days withamplitude up to $\approx0.2$ mag. Comparison of the spectrum obtained in 2022with the one from 2014 also shows an evidence of spectral variability. Theabsence of clearly detected circumstellar nebula does not allow to classifyJ0409+3239, as [WR], i.e. a central star of planetary nebula (CSPN). However,its position in Hertzsprung--Russell diagram suggests that J0409+3239, is a lowmass star caught in rare transitional phase to CSPN. Estimation of J0409+3239,mass based on evolutionary tracks shows that it is less than $0.9~M_\odot$, andthus the age of the Galaxy is barely enough for the star to evolve to itscurrent stage.

LAMOST J040901.83+329355.6 -- a new Galactic star with Wolf--Rayet characteristics on a post-AGB to CSPN transitional stage