Journal
ASTROPHYSICAL JOURNAL
Volume 872, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aafb74
Keywords
cosmology: observations; galaxies: abundances; galaxies: evolution; galaxies: halos; intergalactic medium; quasars: absorption lines
Categories
Funding
- NASA [NAS 5-26555, HST-AR-12854]
- Space Telescope Science Institute [HST-GO-13846]
- NSF [AST-1615296]
- NASA Astrophysical Data Analysis Program (ADAP) [NNX16AF52G, AST-1212012]
- NASA Keck PI Data Award
- NASA ADAP grants [NNX16AF52G, NNX10AE84G]
- W. M. Keck Foundation
- Notre Dame Center for Research Computing
- NASA [NNX16AF52G, 904913] Funding Source: Federal RePORTER
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We present the results from our COS circumgalactic medium (CGM) compendium (CCC), a survey of the CGM at z less than or similar to 1 using H I-selected absorbers with 15 < logN(H I) < 19. We focus here on 82 partial Lyman limit systems (pLLSs, 16.2 <= logN(H I) < 17.2) and 29 LLSs (17.2 <= logN(H I) < 19). Using Bayesian techniques and Markov Chain Monte Carlo sampling of a grid of photoionization models, we derive the posterior probability distribution functions (PDFs) for the metallicity of each absorber in CCC. We show that the combined pLLS metallicity PDF at z less than or similar to 1 has two main peaks at [X/H] similar or equal to -1.7 and -0.4, with a strong dip at [X/H] similar or equal to -1. The metallicity PDF of the LLSs might be more complicated than a unimodal or bimodal distribution. The pLLSs and LLSs probe a similar range of metallicities -3 less than or similar to [X/H] less than or similar to +0.4, but the fraction of very metal-poor absorbers with [X/H] less than or similar to -1.4 is much larger for the pLLSs than the LLSs. In contrast, absorbers with logN(H I) >= 19 have mostly -1 less than or similar to [X/H] less than or similar to 0 at z less than or similar to 1. The metal-enriched gas probed by pLLSs and LLSs confirms that galaxies that have been enriching their CGM over billions of years. Surprisingly, despite this enrichment, there is also abundant metal-poor CGM gas (41%-59% of the pLLSs have [X/H] less than or similar to -1.4), representing a reservoir of near-pristine gas around z less than or similar to 1 galaxies. We compare our empirical results to recent cosmological zoom simulations, finding some discrepancies, including an overabundance of metal-enriched CGM gas in simulations.
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