Photometric observations made during the years 2000-2005 are used to determine the pole orientation of (2953) Vysheslavia, a ≃15-km size member of the Koronis family. We find admissible solutions for ecliptic latitude and longitude of the rotation pole P3 : βp = -64° ± 10° and λp = 11° ± 8° or P4: βp = -68° ± 8° and λp = 192° ± 8°. These imply obliquity values γ = 154° ± 14° and γ = 157° ± 11°, respectively. The sidereal rotation period is Psid = 0.2622722 ± 0.0000018 day. This result is interesting for two reasons: (i) the obliquity value between 90° and 180° is consistent with a prediction done by Vokrouhlický et al. [Vokrouhlický, D., Brož, M., Farinella, P., Knežević, Z., 2001. Icarus 150, 78-93] that Vysheslavia might have been transported to its unstable orbit by the Yarkovsky effect, and (ii) with the obliquity close to 180°, Vysheslavia seems to belong to one of the two distinct groups in the Koronis family found recently by Slivan [Slivan, S.M., 2002. Nature 419, 49-51], further supporting the case of dichotomy in the spin axis distribution in this family. We also argue against the possibility that Vysheslavia reached its current orbit by a recent collisional breakup. © 2005 Elsevier Inc. All rights reserved.