Abstract
We present high speed optical, spectroscopic and Swift X-ray observations made during the dwarf nova superoutburst of CC Scl in November 2011. An orbital period of 1.383 h and superhump period of 1.443 h were measured, but the principal new finding is that CC Scl is a previously unrecognised intermediate polar, with a white dwarf spin period of 389.49 s which is seen in both optical and Swift X-ray light curves only during the outburst. In this it closely resembles the old nova GK Per, but unlike the latter has one of the shortest orbital periods among intermediate polars.
Highlights
CC Scl was listed as RX J2315.5−3049 in the ROSAT X-ray catalogue (Voges et al 1999), later identified with a 17.3 mag star, classified as a cataclysmic variable (CV) (Schwope et al 2000), and found in the Edinburgh-Cape Survey where it became EC 23128−3105 [it is in the Two-Micron All-Sky Survey (2MASS) catalogue as 2MASS J23153185−3048476]
The rapid decay phase lasts only about two days, but there is a slow reduction after that to the Catalina Real-time Transient Survey (CRTS) long-term quiescent magnitude of 16.8. These are compatible with the total of nine days recorded by Ishioka et al (2001), and provide a range of outburst of 3.6 mag, so the duration and amplitude are unusually small for a short orbital period superoutbursting CV
To search for any modulation at the known orbital period we look at the quiescent Remote Observatory Atacama Desert (ROAD) photometry (Chile), starting with 11 November
Summary
CC Scl was listed as RX J2315.5−3049 in the ROSAT X-ray catalogue (Voges et al 1999), later identified with a 17.3 mag star, classified as a cataclysmic variable (CV) (Schwope et al 2000), and found in the Edinburgh-Cape Survey where it became EC 23128−3105 [it is in the Two-Micron All-Sky Survey (2MASS) catalogue as 2MASS J23153185−3048476]. Its nature was confirmed when it was seen to rise in an outburst to magnitude 13.4 on 2000 July 8 [see Ishioka et al (2001) for details] followed by another about 100 d later. The latter was observed by Ishioka et al (2001) who suspected two apparent superhumps with a separation of 0.078 d. Ishioka et al (2001) noted that at 9 d duration the apparent superoutburst of CC Scl was unusually brief: ∼14 d is more to be expected of a short orbital period system.
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