  We report new observations of the central star of the planetary nebula VV 47
carried out to verify earlier assertions that the short-period pulsation modes
detected in the star are driven by the $\epsilon$ mechanism. In our data, VV 47
was not variable up to a limit of 0.52 mmag in the Fourier amplitude spectrum
up to the Nyquist frequency of 21.7 mHz. Given this null result we re-analyzed
the data set in which oscillations were claimed. After careful data reduction,
photometry, extinction correction, and analysis with a conservative criterion
of S/N $\geq$ 4 in the Fourier amplitude spectrum, we found that the star was
not variable during the original observations. The oscillations reported
earlier were due to an over-optimistic detection criterion. We conclude that VV
47 did not pulsate during any measurements at hand; the observational detection
of $\epsilon$-driven pulsations remains arduous.
