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tokens: to estimate the duty cycle and constrain the outburst recurrence time for a large sample of CVs. These properties will help constrain the mass-transfer rate and AML rate in the overall population. Better-constrained AML rates will improve evolutionary models and our understanding of the post-bounce population, and help to reconcile the observed and predicted position of the period minimum. Our catalogue was constructed with a goal towards answering these, and related, questions that require large samples of CV properties to answer. Additionally, it is meant as a reference for individual systems and a means of selecting CVs for targeted campaigns, based on their outburst properties. In Section 2 , we discuss the CRTS survey in detail. Section 3 describes the classification script, and Section 4 outlines the contents of our catalogue. The catalogue is then characterized in Section 5 . 2 CATALINA REAL-TIME TRANSIENT SURVEY The CRTS identifies transients in the data from the Catalina Sky Survey 1 (Larson et al. 1998 , 2003 ) – a photometric survey that searches for Potentially Hazardous Asteroids and Near Earth Objects. Three subsurveys constitute the Catalina Sky Survey, namely the original CSS (Catalina Schmidt Survey), the MLS (Mt Lemmon Survey) based in Arizona, and the SSS (Siding Spring Survey) in Australia, which ended on 2014 July 5. Each has a dedicated telescope with a 4k back-illuminated, unfiltered CCD camera (Djorgovski et al. 2010 ). The field of view and typical limiting magnitude for each survey (at ∼30 s integrations) are 82 and V ∼ 19.5 mag for the CSS, 11 and V ∼ 21.5 mag for the MLS, and 4and V ∼ 19 mag for the SSS. Together these surveys cover 30 000 deg 2 (, see Drake et al. 2014 for more details). The Galactic plane () is avoided due to overcrowding, as are the Magellanic Clouds. Each observation consists of four images (frames) that are separated by ≈10 min. The observing cadence is typically one to four times per lunation (depending on the subsurvey and field). Aperture photometry is performed using SExtractor software (Bertin Arnouts 1996 ) and converted to V -band magnitudes using standard stars as described in Drake et al. ( 2013 ). The CRTS began processing CSS data on 2007 November 8, MLS data on 2009 November 6 and 2010 May 5 for SSS data (Drake et al. 2014 ). Although there is Catalina Sky Survey data preceding these dates, the CRTS only use these data in the transient classification process – any object that was only variable during this time will not have been identified as a CRTS transient. To identify variability, the CRTS makes catalogues of the objects in each image and compare these to previously recorded magnitudes; they do not use image subtraction. An object needs to pass a number of tests to be classified as a transient. In each set of four frames (one epoch), it needs to be positionally coincident in at least three of the frames. This eliminates high proper motion objects (movement of > 0.1 arcmin min