We report a multisite photometric campaign for the \beta Cep stars V2052 Oph and V986 Oph .
670 hours of high-quality differential photoelectric Strömgren , Johnson and Geneva time-series photometry were obtained with eight telescopes on five continents during 182 nights .
Frequency analyses of the V2052 Oph data enabled the detection of three pulsation frequencies , the first harmonic of the strongest signal , and the rotation frequency with its first harmonic .
Pulsational mode identification from analysing the colour amplitude ratios confirms the dominant mode as being radial , whereas the other two oscillations are most likely l = 4 .
Combining seismic constraints on the inclination of the rotation axis with published magnetic field analyses we conclude that the radial mode must be the fundamental .
The rotational light modulation is in phase with published spectroscopic variability , and consistent with an oblique rotator for which both magnetic poles pass through the line of sight .
The inclination of the rotation axis is 54 \degr < i < 58 \degr and the magnetic obliquity 58 \degr < \beta < 66 \degr .
The possibility that V2052 Oph has a magnetically confined wind is discussed .
The photometric amplitudes of the single oscillation of V986 Oph are most consistent with an l = 3 mode , but this identification is uncertain .
Additional intrinsic , apparently temporally incoherent , light variations of V986 Oph are reported .
Different interpretations thereof can not be distinguished at this point , but this kind of variability appears to be present in many OB stars .
The prospects of obtaining asteroseismic information for more rapidly rotating \beta Cep stars , which appear to prefer modes of higher l , are briefly discussed .