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tokens: Lasota (2007) have updated this work, for a sample of ten CVs. The importance of this test was revived by Schreiber Gänsicke (2002) , who pointed out that the HST FGS parallax distance of SS Cyg, the archetypal dwarf nova, led to a revised mass transfer rate that placed this outbursting system in the stable region of the ( R out , Ṁ ) plane. This led to much hand-wringing ( Schreiber Lasota 2007 ; Smak 2010 ) until a radio VLBI parallax distance ( Miller-Jones et al. 2013 ), confirmed with Gaia ( Ramsay et al. 2017 ), firmly placed the system in the unstable region (as anticipated by Lasota 2008 ). Although there are dozens of CVs with relatively well-known binary parameters, a thorough investigation of this test has yet to be performed. Ramsay et al. (2017) proposed to test the DIM by taking the absolute magnitude at a specific stage of a dwarf nova outbursts (at the end of long outbursts or in stand-stills) to compare the derived mass accretion rate to the critical rate for the system, under the assumption that both should be nearly equal. Good agreement was found for the sample of a dozen CVs with distances in the Gaia first data release. Its main advantage is that the required optical magnitude is straightforward to extract from the light curves. However, a major drawback of this approach is that it relies on assumptions on how matter is transported in the disk because one needs to predict when the mass accretion rate happens to be equal to the critical rate during the outburst cycle. Hence, it is a much less fundamental and robust test of the basic premises of the DIM. Indeed, an important difficulty in using the fundamental test is that it requires extracting the average mass transfer rate from CV optical light curves, which in many cases are unevenly, inhomogeneously, and incompletely sampled. The situation is somewhat easier for X-ray binaries, for which the DIM also applies because X-ray monitors provide continuous coverage and X-rays provide a closer measure of the bolometric luminosity in those systems than optical magnitudes do for CVs, which in outburst emit primarily UV radiation. Coriat et al. (2012) were able to derive average mass accretion rates for ~50 X-ray binaries and showed that the DIM, modified to include X-ray irradiation ( van Paradijs 1996 ), separates consistently transients from steady systems. We carry out, for the first time on CVs, a similar analysis to that performed on X-ray binaries by Coriat et al. (2012) to test the fundamental prediction of the DIM: the separation of CVs into stable and unstable systems is determined by the orbital period (a proxy for disk size) of the binary and mass transfer rate from the companion. We use a subsample of the CV light curves gathered by Otulakowska-Hypka et al. (2016) . We consider all types of dwarf nova outbursts, including so-called super-outbursts that are not supposed to be described by the standard version of the DIM (see, e.g., Lasota 2001 , and references