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We analyze spatially resolved and co-added SDSS-IV MaNGA spectra withsignal-to-noise ~100 from 2200 passive central galaxies (z~0.05) to understandhow central galaxy assembly depends on stellar mass (M*) and halo mass (Mh). Wecontrol for systematic errors in Mh by employing a new group catalog fromTinker (2020a,b) and the widely-used Yang et al. (2007) catalog. At fixed M*,the strength of several stellar absorption features varies systematically withMh. Completely model-free, this is one of the first indications that thestellar populations of centrals with identical M* are affected by theproperties of their host halos. To interpret these variations, we applied fullspectral fitting with the code alf. At fixed M*, centrals in more massive halosare older, show lower [Fe/H], and have higher [Mg/Fe] with 3.5 sigmaconfidence. We conclude that halos not only dictate how much M* galaxiesassemble, but also modulate their chemical enrichment histories. Turning to ouranalysis at fixed Mh, high-M* centrals are older, show lower [Fe/H], and havehigher [Mg/Fe] for Mh>10^{12}Msun/h with confidence > 4 sigma. While massivepassive galaxies are thought to form early and rapidly, our results are amongthe first to distinguish these trends at fixed Mh. They suggest that high-M*centrals experienced unique early formation histories, either through enhancedcollapse and gas fueling, or because their halos were early-forming and highlyconcentrated, a possible signal of galaxy assembly bias.

SDSS-IV MaNGA: How the stellar populations of passive central galaxies depend on stellar and halo mass