Magnetic CVs in the UCT CCD CV Survey

An overview is given of all the magnetic CVs found in the UCT CCD CV Survey (Woudt & Warner 2001, 2002, 2003a). We have identified eight new candidate Intermediate Polars (IP), of which six are classical novae (RR Cha, DD Cir, AP Cru, V697 Sco, V373 Sct, and RXJ1039.7-0507). The two other candidate IPs are Aqr1 (2236+0052) and RXJ0944.5+0357. In addition, there are two probable Polars, namely V351 Pup (= Nova Puppis 1991) and FIRST J102347.6+003841. 1. The UCT CCD CV Survey The UCT CCD CV Survey is an ongoing high-speed photometric survey of faint Cataclysmic Variable (CV) stars (Woudt & Warner 2001, 2002, 2003a) down to a magnitude limit of V ∼ 21. For this survey, we use the 1.9-m and 1.0-m telescopes of the South African Astronomical Observatory at the Sutherland site, in combination with the University of Cape Town (UCT) CCD camera (O’Donoghue 1995). In the past three years, an intensive observational campaign – mainly focused on old novae – has resulted in new orbital periods for 18 CVs, 12 of which are old southern novae. 2. Candidate Intermediate Polars The objects listed in this section are candidate Intermediate Polars. In these systems we have either seen a second (consistent) photometric period in addition to the orbital modulation, e.g., DD Cir, or we have identified multiple photometric periodicities associated with a spin period (or its harmonic) and its orbital sidebands, e.g., RX J1039.7-0507. In the former case, confirmation of the suspected spin period in X-ray, or optical sidebands, are needed to confirm its classification, whereas in the latter scenario, the orbital sidebands already secure the IP nature of the CV. We will list each of the eight candidate IPs with a short description of their main characteristics, a summary is given in Table 1. Aqr1: Listed in Downes et al. (2001) as Aqr1, this object is also known as 2236+0052 and was identified spectroscopically as a CV by Berg et al. (1992) in a bright QSO survey. We have observed Aqr1 during four nights in 2002 November; the light curves of Aqr1 (for two of the nights) are shown in Fig. 1. The Fourier Transform (FT) of the combined data set, after subtracting the mean