| Abstract
| - We present multicolour CCD photometry of the short-period RS CVn-type binary DV Psc obtained in 2006 September and October. Our observations indicate that GSC0008-789, the comparison star used by Robb et al. in their discovery of DV Psc, is a variable with amplitude exceeding 0.08 mag. Based on the new data, the orbital period of the eclipsing system is revised to 0.308 536 09 d. From the new observations, a set of completely covered B, V and R light curves and a single V-band light curve are formed in two epochs. The radial-velocity curves obtained by Lu, Rucinski & Ogloza are reformed with the newly determined ephemeris and are analysed along with the light curves using the 2003 version of the Wilson-Devinney code. The results show that DV Psc is a detached, near-contact binary system with a mass ratio of 0.693 ± 0.005 and a separation of 2.038 R⊙. The masses and radii for the components are determined as 0.70 ± 0.02 M⊙, 0.68 ± 0.03 R⊙ for the primary, and 0.49 ± 0.01 M⊙, 0.51 ± 0.02 R⊙ for the secondary.
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