Context : Aims : We present an asteroseismological study on the two high-gravity pulsating PG1159 ( GW Vir or DOV ) stars , PG 2131+066 and PG 1707+427 , and on the pulsating [ WCE ] star NGC 1501 . All of these stars have been intensively scrutinized through multi-site observations , so they have well resolved pulsation spectra . Methods : We compute adiabatic g -mode pulsation periods on PG1159 evolutionary models with stellar masses ranging from 0.530 to 0.741 M _ { \odot } . These models take into account the complete evolution of progenitor stars , through the thermally pulsing AGB phase , and born-again episode . We constrain the stellar mass of PG 2131+066 , PG 1707+427 , and NGC 1501 by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings . We also employ the individual observed periods in search of representative seismological models for each star . Results : We derive a stellar mass of 0.627 M _ { \odot } for PG 2131+066 , 0.597 M _ { \odot } for PG 1707+427 , and 0.571 M _ { \odot } for NGC 1501 from a comparison between the observed period spacings and the computed asymptotic period spacings , and a stellar mass of 0.578 M _ { \odot } for PG 2131+066 , 0.566 M _ { \odot } for PG 1707+427 , and 0.576 M _ { \odot } for NGC 1501 by comparing the observed period spacings with the average of the computed period spacings . We also find , on the basis of a period-fit procedure , asteroseismological models representatives of PG 2131+066 and PG 1707+427 . These best-fit models are able to reproduce the observed period patterns of these stars with an average of the period differences of \overline { \delta \Pi _ { i } } = 1.57 s and \overline { \delta \Pi _ { i } } = 1.75 s , respectively . The best-fit model for PG 2131+066 has an effective temperature T _ { eff } = 102 100 K , a stellar mass M _ { * } = 0.589 M _ { \odot } , a surface gravity \log g = 7.63 , a stellar luminosity and radius of \log ( L _ { * } / L _ { \odot } ) = 1.57 and \log ( R _ { * } / R _ { \odot } ) = -1.71 , respectively , and a He-rich envelope thickness of M _ { env } = 1.6 \times 10 ^ { -2 } M _ { \odot } . We derive a seismic distance d \sim 830 pc and a parallax \pi \sim 1.2 mas . The best-fit model for PG 1707+427 , on the other hand , has T _ { eff } = 89 500 K , M _ { * } = 0.542 M _ { \odot } , \log g = 7.53 , \log ( L _ { * } / L _ { \odot } ) = 1.40 , \log ( R _ { * } / R _ { \odot } ) = -1.68 , and M _ { env } = 2.5 \times 10 ^ { -2 } M _ { \odot } , and the seismic distance and parallax are d \sim 730 pc and \pi \sim 1.4 mas . Finally , we have been unable to find an unambiguous best-fit model for NGC 1501 on the basis of a period-fit procedure . Conclusions : This work closes our short series of asteroseismological studies on pulsating pre-white dwarf stars . Our results demonstrate the usefulness of asteroseismology for probing the internal structure and evolutionary status of pre-white dwarf stars . In particular , asteroseismology is able to determine stellar masses of PG1159 stars with an accuracy comparable or even better than spectroscopy .