We report optical spectroscopy and high-speed photometry and polarimetry of the INTE-GRAL source IGRJ14536-5522 (=Swift J1453.4-5524). The photometry, polarimetry and spectroscopy are modulated on an orbital period of 3.1564(1) h. Orbital circularly polarized modulations are seen from ∼0 to ∼ −18 per cent, unambiguously identifying IGRJ14536-5522 as a polar. The negative circular polarization is seen over ∼95 per cent of the orbit, which is consistent (as viewed from the Earth) with a single-pole accretor. We estimate some of the system parameters by modelling the polarimetric observations. Some of the high-speed photometric data show modulations that are consistent with quasiperiodic oscillations (QPOs) on the order of 5-6 min. Furthermore, for the first time, we detect the (5-6) min QPOs in the circular polarimetry. We discuss the possible origins of these QPOs. In addition, we note that the source undergoes frequent changes between different accretion states.We also include details of HIgh-speed Photo-POlarimeter (HIPPO), a new high-speed photopolarimeter, used for some of our observations. This instrument is capable of high-speed, multi-filtered, simultaneous all-Stokes observations. It is therefore ideal for investigating rapidly varying astronomical sources such as magnetic cataclysmic variables.

We describe briefly the properties of the recently completed Southern African Large Telescope (SALT), along with its first light imager SALTICAM. Using this instrument, we present 4.3 h of high‐speed unfiltered photometric observations of the eclipsing polar SDSS J015543.40+002807.2 with time‐resolution as short as 112 ms, the highest‐quality observations of this kind of any polar to date. The system was observed during its high‐luminosity state. Two accreting poles are clearly seen in the eclipse light curve. The binary system parameters have been constrained: the white dwarf mass is at the low end of the range expected for cataclysmic variables. Correlations between the positions of the accretion regions on or near the surface of the white dwarf and the binary system parameters were established. The sizes of the accretion regions and their relative movement from eclipse to eclipse were estimated: they are typically 4°–7° depending on the mass of the white dwarf. The potential of these observations will only fully be realized when low‐state data of the same kind are obtained and the contact phases of the eclipse of the white dwarf are measured.

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