Browsing by Author "Kannappan, Sheila J."

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    The resolved and eco g3 initiative: drivers of h i content and x-ray emission in galaxy groups
    (Institute of Physics, 2025) Baker, Andrew J.; Hutchens, Zackary L.; Kannappan, Sheila J.
    Adding to the RESOLVE and ECO Gas in Galaxy Groups (G3) initiative, we examine possible drivers of group-integrated H i-to-halo mass ratios (MHI,grp/Mhalo) and group X-ray emission, including group halo mass (Mhalo), virialization as probed by crossing time (tcross), presence of active galactic nuclei (AGN), and group-integrated fractional stellar mass growth rate (FSMGRgrp). G3 groups span Mhalo = 1011−1014.5 M⊙ with comprehensive H i gas and AGN information, which we combine with X-ray stacking of ROSAT All-Sky data. We detect hot gas emission exceeding AGN and X-ray binary backgrounds confidently for Mhalo = 1012.6−1014 M⊙ and unambiguously for Mhalo > 1014 M⊙, reflecting an inverse dependence of MHI,grp/Mhalo and hot gas emission on halo mass. At fixed halo mass, MHI,grp/Mhalo transitions to greater spread below tcross ∼ 2 Gyr. Dividing groups across this transition, lower-tcross groups show elevated X-ray emission compared to higher-tcross groups for Mhalo > 1013.3 M⊙, but this trend reverses for Mhalo = 1012.6−1013.3 M⊙. Additionally, AGN-hosting halos below Mhalo ∼ 1012.1 M⊙ exhibit a broad, ∼0.25 dex deep valley in MHI,grp/Mhalo compared to non-AGN-hosting halos with correspondingly reduced FSMGRgrp. When diluted by non-AGN-hosting halos, this valley becomes shallower and narrower, falling roughly between M halo = 10 11.5 M ⊙ and M halo = 10 12.1 M ⊙ in the overall MHI,grp/Mhalo vs. Mhalo relation. We may also detect a second, less easily interpreted valley at Mhalo ∼ 1013 M⊙. Neither valley matches theoretical predictions of a deeper valley located at or above M halo = 10 12.1 M ⊙ .