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tokens: complex structure within the overall galaxy mass functions. For instance, in increasingly higher halo mass regimes, we observe high-mass drop-offs that occur at higher galaxy mass. These drop-offs mark the natural boundary in the largest central galaxy mass for a given halo mass, as seen in Figure 5 (b). Figure 13. Breakdown of RESOLVE-B (top row), L r ,tot -limited RESOLVE-B (middle row), and ECO (bottom row) SMF and BMF into different group halo mass regimes. The four group halo mass regimes are M halo 10 11.4 M ⊙ (low-mass groups, often solo centrals, blue), M halo between 10 11.4 and 10 12 M ⊙ (intermediate-mass groups, green), M halo between 10 12 and 10 13.5 M ⊙ (large group, orange), and M halo > 10 13.5 M ⊙ (cluster, red, ECO only). The dark gray marks the overall SMF or BMF for each data set, and the gray hash-marked region denotes the incomplete regions for each mass function. The conditional mass functions are much more complex than the overall mass function, with pronounced bumps and dips. In both the RESOLVE-B and ECO intermediate (green) and large (orange) group halo mass regimes, we observe a peak in the SMF and BMF. For intermediate group halos, this peak occurs at ∼10 10.2 M ⊙ , right between the gas-richness threshold and bimodality mass scales. For large group halos, the peak occurs at ∼10 10.8 M ⊙ , above the bimodality mass scale and also near the knee of the overall mass functions. The peak in the large group halo regime appears to be causing the pronounced “bump” seen in the overall RESOLVE-B SMF and BMF. While the ECO data set also has this characteristic peak in its large group halo regime mass functions, the more gradual decline in the overall SMF and BMF for large galaxy masses seems to be due to the cluster galaxy population in ECO. The cluster population makes up 17% of galaxies with M star > 10 10.5 M ⊙ and 31% of galaxies with M star > 10 11 M ⊙ for ECO. The RESOLVE-B “bump,” meanwhile, may be emphasized by the lack of a cluster galaxy population and the overabundance of halos in this large group halo regime, as shown in Figure 5 (a). It is clear that the low-mass slopes of the SMF and BMF in these different halo mass regimes are very different. In the cluster halo mass regime, the rise is quite smooth, although the slope appears to flatten out at lower masses, at least in part due to incompleteness in galaxy counts around the clusters caused by high fiber collision rates and by missing ultradiffuse galaxies like those recently found in the Coma and Virgo clusters (Mihos et al. 2015 ; van Dokkum et al. 2015 ). We note that Yamanoi et al. ( 2012 ) found a fairly flat slope for the Coma cluster LF down to galaxy magnitudes of M R = −14.0, with a steep upturn for galaxies below our luminosity limit. Also, not all previous studies of cluster LFs have found steep slopes, and many cluster LF studies have relied on using statistical counts to remove background galaxies (e.g., Dressler 1978 and Goto et al. 2002 ).