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Methods to measure masses of PG1159 stars in order to test evolutionaryscenarios are currently based on spectroscopic masses or asteroseismologicalmass determinations. SDSSJ212531.92-010745.9, a recently discovered PG1159 starin a close binary system, may finally allow the first dynamical massdetermination, and has so far been analysed on the basis of one SDSS spectrumand photometric monitoring.  In order to be able to phase radial velocity measurements of the systemSDSSJ212531.92-010745.9, we have followed up the photometric monitoring of thissystem. New white light time series of the brightness variation ofSDSSJ212531.92-010745.9 with the Tuebingen 80cm and Goettingen 50cm telescopesextend the monitoring into a second season (2006). We give the improvedephemeris for the orbital motion of the system, based on a sine fit which nowresults in a period of 6.95573(5)h.  In 2007, we have obtained a series of phase-resolved medium-resolutionspectra with the TWIN spectrograph at the 3.5m telescope at Calar Alto, whichwill allow us to derive the radial velocity curves for both components of thesystem, and to perform spectral analyses of the irradiating and irradiatedcomponents at different phases. We briefly describe the newly obtained spectra.The light curve and radial velocities combined will allow us to carry out amass determination.

New Light Curves and Spectra of the close PG1159 Binary System SDSSJ212531.92-010745.9