1997PASP..109.1241T

begin{tex}This paper gives mean spectra and reports orbital periods based on radial velocities taken near minimum light for these dwarf novae, which are all SU UMa stars or candidates. For VZ Pyx I find P_orb = 0.07332 ±0.00003 d (= 105.58 ±0.04 min), for CC Cnc 0.07352 ±0.00005 d (= 105.86 ±0.07 min), and for AH Eri, 0.2391 ±0.0005 d (= 5.738 ±0.012 hr). In AH Eri's case orbital frequencies differing by ±1 cycle d^{-1} are marginally possible. The period for VZ Pyx is similarly ambiguous, but Kato and Nogami's knvz (1997a) superhump period and Remillard et al.'s rem94 (1994) short time base velocity study constrain the alias choice to a single value. For CC Cnc, a preliminary measurement by Munari et al. mun (1991) had indicated a P_orb in the 2 to 3 hour period `gap', but the P_orb found here is well short of the gap. AH Eri had been mentioned in the literature as a possible SU-UMa type dwarf nova; the long period found here makes this classification doubtful. The average spectrum of AH Eri shows molecular absorption bands consistent with an M-type secondary star. With the orbital periods in hand, it would now be interesting to obtain new timeseries photometry aimed at confirming or refuting the candidate ∼40 min photometric modulations in AH Eri and VZ Pyx which have been put forth in the literature.