Context : KUV 05134+2605 is one of the 21 pulsating DB white dwarfs ( V777 Her or DBV variables ) known so far .
The detailed investigation of the short-period and low-amplitude pulsations of these relatively faint targets requires considerable observational efforts from the ground , long-term single-site or multisite observations .
The observed amplitudes of excited modes undergo short-term variations in many cases , which makes the determination of pulsation modes difficult .

Aims : We aim to determine the pulsation frequencies of KUV 05134+2605 , find regularities between the frequency and period components , and perform its asteroseismic investigation for the first time .

Methods : We re-analysed the data already published , and collected new measurements .
We compared the frequency content of the different datasets from the different epochs and performed various tests to check the reliability of the frequency determinations .
The mean period spacings were investigated with linear fits to the observed periods , Kolmogorov-Smirnov and Inverse Variance significance tests , and Fourier analysis of different period sets , including a Monte Carlo test simulating the effect of alias ambiguities .
We employed fully evolutionary DB white dwarf models for the asteroseismic investigations .

Results : We identified 22 frequencies between 1280 and 2530 \mu Hz .
These form 12 groups , which suggests at least 12 possible frequencies for the asteroseismic investigations .
Thanks to the extended observations , KUV 05134+2605 joined the group of rich white dwarf pulsators .
We identified one triplet and at least one doublet with a \approx 9 \mu Hz frequency separation , from which we derived a stellar rotation period of 0.6 d. We determined the mean period spacings of \approx 31 and 18 s for the modes we propose as dipole and quadrupole , respectively .
We found an excellent agreement between the stellar mass derived from the \ell = 1 period spacing and the period-to-period fits , all providing M _ { * } = 0.84 - 0.85 M _ { \odot } solutions .
Our study suggests that KUV 05134+2605 is the most massive amongst the known V777 Her stars .

Conclusions :