Morphology-density relation in two MAMMOTH protoclusters, BOSS1244 (in red) and BOSS1542 (in black). The weighted CANDELS field is shown in blue and the CANDELS stellar mass and SFR sample (CANDELS M_* & SFR lim) is shown in magenta. Top: All detected galaxies brighter than our magnitude threshold (m_F160W ≤ 24.5). Bottom: All detected galaxies brighter than m*+1, where m* is the modeled magnitude of an L^* galaxy at z = 2.246 estimated using EzGal (i.e., m_F160W ≤ 23.36 magnitudes; Mancone & Gonzalez 2012). In each plot, the density measurement is for the entire sample. The value of the fraction of galaxies with n ≥ 2 for each sample is measured by bootstrapping over the measured errors in Sérsic index over 1000 iterations. We found evidence for an internal morphology-density trend in both protoclusters among all galaxies, but no evidence for an enhancement of the early-type fraction relative to the field. The brighter galaxies in each protocluster differed, however, with the denser regions of BOSS1542 having fewer early-type massive galaxies.