Y.M. Bahé
The distribution of atomic hydrogen in EAGLE galaxies: morphologies, profiles, and H I holes
Bahé, Y.M.; Crain, R.A.; Kauffmann, G.; Bower, R.G.; Schaye, J.; Furlong, M.; Lagos, C.; Schaller, M.; Trayford, J.W.; Dalla Vecchia, C.; Theuns, T.
Authors
R.A. Crain
G. Kauffmann
R.G. Bower
J. Schaye
M. Furlong
C. Lagos
M. Schaller
J.W. Trayford
C. Dalla Vecchia
Professor Tom Theuns tom.theuns@durham.ac.uk
Professor
Abstract
We compare the mass and internal distribution of atomic hydrogen (H I) in 2200 present-day central galaxies with Mstar > 1010 M⊙ 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, , agree with observations to better than 0.1 dex for galaxies with Mstar between 1010 and 1011 M⊙. Our fiducial, empirical H2 model based on gas pressure results in galactic H I mass fractions, [Math Processing Error], that agree with observations from the GASS survey to better than 0.3 dex, but the alternative theoretical H2 formula from high-resolution simulations leads to a negative offset in [Math Processing Error] 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 [Math Processing Error] (by a factor of ≲ 2 compared to data from the Bluedisk survey). In the outer region ([Math Processing Error]), the simulated profiles agree quantitatively with observations. Scaled by H I size, the simulated profiles of H I-rich ([Math Processing Error]) and control galaxies ([Math Processing Error]) follow each other closely, as observed.
Citation
Bahé, Y., Crain, R., Kauffmann, G., Bower, R., Schaye, J., Furlong, M., …Theuns, T. (2016). The distribution of atomic hydrogen in EAGLE galaxies: morphologies, profiles, and H I holes. Monthly Notices of the Royal Astronomical Society, 456(1), 1115-1136. https://doi.org/10.1093/mnras/stv2674
Journal Article Type | Article |
---|---|
Acceptance Date | Nov 12, 2015 |
Online Publication Date | Dec 19, 2015 |
Publication Date | Feb 11, 2016 |
Deposit Date | Apr 5, 2016 |
Publicly Available Date | Mar 29, 2024 |
Journal | Monthly Notices of the Royal Astronomical Society |
Print ISSN | 0035-8711 |
Electronic ISSN | 1365-2966 |
Publisher | Royal Astronomical Society |
Peer Reviewed | Peer Reviewed |
Volume | 456 |
Issue | 1 |
Pages | 1115-1136 |
DOI | https://doi.org/10.1093/mnras/stv2674 |
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Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
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