tokens: It can be seen that it agrees well with the other methods tested. The three methods, whilst not in exact concurrence, are in good agreement. Thus, to separate spirals and ellipticals in our sample, we use the parameter, both because it gives the intermediate values for fraction of spirals and ellipticals, and because it is more reliable and less computationally expensive when computed for a very large number of galaxies. We also present numerical results from our tests using g r band luminosity as the divide between spiral and elliptical galaxies, with a cut defined by equation ( A1 ) (Figs A2 and A3 ). Figure A2. Similar to Fig. A1 , but here galaxies are split based on the cutoff in g r band luminosity from equation ( A1 ). Figure A3. Distribution of ETGs in the R plane, as in Fig. 3 , but using g r luminosity, rather than as the cutoff between spirals and ellipticals. We find a smaller number of ellipticals by the same selection criteria, roughly half those in the ATLAS 3D survey, and a similar distribution, with a slightly higher fraction of highly elongated or fast-spinning galaxies compared to that found with a cutoff. We also experimented with making a cutoff between star-forming and quiescent galaxies based on their magnitude in the g and r bands. Galaxies for which g r is large are redder with little star formation and these quiescent galaxies are often ellipticals, whilst smaller g r colours characterize bluer, star-forming galaxies, which in observational surveys correspond well with the population of spirals (Kormendy 2016 ). We define a cut between star-forming galaxies as those below the line and quiescent galaxies as those above, motivated by the distribution of the whole sample of galaxies in Illustris (Vogelsberger etal. 2014 ). The luminosities are found by summing the individual luminosity of all stellar particles in the galaxy. The fraction of quiescent to star-forming galaxies, by mass, is in line with observations (Muzzin etal. 2013 ) over the whole mass range examined (down to haloes with stellar mass of 10 10 M ). Fig. A3 is a comparison with the galaxy population found in the ATLAS 3D survey, as presented in Section 3.1 using a cutoff defined by . We find less galaxies classified as ellipticals in the same volume, roughly half the previous number, with a wider spread in the distribution. There are more, faster spinning galaxies included though still few as rapidly rotating as in the ATLAS 3D survey. The population of high-mass galaxies is essentially unchanged, still with particularly elongated high-mass SRs as mentioned in Section 3.1 . Fig. A2 shows the stellar mass function derived using a colour cut. Whilst the results are more in line with the observed stellar mass function at low masses, we believe that this is due to the dependence of both on galaxy mass, rather than any strong link between luminosity and kinematic behaviour. Bottrell etal. ( 2017 ) performed similar analysis on carefully constructed mock
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