SDSS-IV MaNGA: How the stellar populations of passive central galaxies depend on stellar and halo mass
| Autor: | Oyarzun, Grecco A., Bundy, Kevin, Westfall, Kyle B., Tinker, Jeremy L., Belfiore, Francesco, Argudo-Fernandez, Maria, Zheng, Zheng, Conroy, Charlie, Masters, Karen L., Wake, David, Law, David R., McDermid, Richard M., Aragon-Salamanca, Alfonso, Parikh, Taniya, Yan, Renbin, Bershady, Matthew, Sanchez, Sebastian F., Andrews, Brett H., Fernandez-Trincado, Jose G., Lane, Richard R., Bizyaev, D., Boardman, Nicholas Fraser, Lacerna, Ivan, Brownstein, J. R., Drory, Niv, Zhang, Kai |
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| Rok vydání: | 2022 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| DOI: | 10.3847/1538-4357/ac7048 |
| Popis: | We analyze spatially resolved and co-added SDSS-IV MaNGA spectra with signal-to-noise ~100 from 2200 passive central galaxies (z~0.05) to understand how central galaxy assembly depends on stellar mass (M*) and halo mass (Mh). We control for systematic errors in Mh by employing a new group catalog from Tinker (2020a,b) and the widely-used Yang et al. (2007) catalog. At fixed M*, the strength of several stellar absorption features varies systematically with Mh. Completely model-free, this is one of the first indications that the stellar populations of centrals with identical M* are affected by the properties of their host halos. To interpret these variations, we applied full spectral fitting with the code alf. At fixed M*, centrals in more massive halos are older, show lower [Fe/H], and have higher [Mg/Fe] with 3.5 sigma confidence. We conclude that halos not only dictate how much M* galaxies assemble, but also modulate their chemical enrichment histories. Turning to our analysis at fixed Mh, high-M* centrals are older, show lower [Fe/H], and have higher [Mg/Fe] for Mh>10^{12}Msun/h with confidence > 4 sigma. While massive passive galaxies are thought to form early and rapidly, our results are among the first to distinguish these trends at fixed Mh. They suggest that high-M* centrals experienced unique early formation histories, either through enhanced collapse and gas fueling, or because their halos were early-forming and highly concentrated, a possible signal of galaxy assembly bias. Comment: Accepted for publication in ApJ. 28 pages and 12 figures |
| Databáze: | arXiv |
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