NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-18 T01:00:00 PDT
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For refcode 2016MNRAS.456.1115B:
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Copyright by Royal Astronomical Society. 2016MNRAS.456.1115B The distribution of atomic hydrogen in EAGLE galaxies: morphologies, profiles, and H I holes Bahe, Yannick M.; Crain, Robert A.; Kauffmann, Guinevere; Bower, Richard G.; Schaye, Joop; Furlong, Michelle; Lagos, Claudia; Schaller, Matthieu; Trayford, James W.; Dalla Vecchia, Claudio; Theuns, Tom Abstract. We compare the mass and internal distribution of atomic hydrogen (H I) in 2200 present-day central galaxies with M_star_ > 10^10^ M_sun_ from the 100 Mpc EAGLE 'Reference' simulation to observational data. Atomic hydrogen fractions are corrected for self-shielding using a fitting formula from radiative transfer simulations and for the presence of molecular hydrogen using an empirical or a theoretical prescription from the literature. The resulting neutral hydrogen fractions, M_{H_I+H_2}_ / M_star, agree with observations to better than 0.1 dex for galaxies with M_star_ between 10^10^ and 10^11^ M_sun_. Our fiducial, empirical H_2_ model based on gas pressure results in galactic H I mass fractions, M_{H I/ M_star, that agree with observations from the GASS survey to better than 0.3 dex, but the alternative theoretical H_2_ formula from high-resolution simulations leads to a negative offset in M_{H I}_/ M_star of up to 0.5 dex. Visual inspection of mock H I images reveals that most H I discs in simulated H I-rich galaxies are vertically disturbed, plausibly due to recent accretion events. Many galaxies (up to 80 per cent) contain spuriously large H I holes, which are likely formed as a consequence of the feedback implementation in EAGLE. The H I mass-size relation of all simulated galaxies is close to (but 16 per cent steeper than) observed, and when only galaxies without large holes in the H I disc are considered, the agreement becomes excellent (better than 0.1 dex). The presence of large H I holes also makes the radial H I surface density profiles somewhat too low in the centre, at Sigma_{H I}_ > 1 M_{sun}_ pc^{-2} (by a factor of <~ 2 compared to data from the Bluedisk survey). In the outer region (Sigma_{H I}_ < 1 M_{sun}_ pc^{-2}), the simulated profiles agree quantitatively with observations. Scaled by H I size, the simulated profiles of H I-rich (M_{H I}_> 10^{9.8} M_{sun}_) and control galaxies (10^{9.1} M_{sun}_> M_{H I}_ > 10^{9.8} M_{sun}_) follow each other closely, as observed. Key words: methods: numerical, galaxies: formation, galaxies: ISM, galaxies: structure
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