@misc{bahe2016origin,
  abstract = {Observations of galaxies in the local Universe have shown that both the
ionized gas and the stars of satellites are more metal-rich than of equally
massive centrals. To gain insight into the connection between this metallicity
enhancement and other differences between centrals and satellites, such as
their star formation rates, gas content, and growth history, we study the
metallicities of >3600 galaxies with M_star > 10^10 M_sun in the cosmological
hydrodynamical EAGLE 100 Mpc `Reference' simulation, including ~1500 in the
vicinity of galaxy groups and clusters (M_200 >= 10^13 M_sun). The simulation
predicts excess gas and stellar metallicities in satellites consistent with
observations, except for stellar metallicities at M_star <~ 10^10.2 M_sun where
the predicted excess is smaller than observed. The exact magnitude of the
effect depends on galaxy selection, aperture, and on whether the metallicity is
weighted by stellar mass or luminosity. The stellar metallicity excess in
clusters is also sensitive to the efficiency scaling of star formation
feedback. We identify stripping of low-metallicity gas from the galaxy
outskirts, as well as suppression of metal-poor inflows towards the galaxy
centre, as key drivers of the enhancement of gas metallicity. Stellar
metallicities in satellites are higher than in the field as a direct
consequence of the more metal-rich star forming gas, whereas stripping of stars
and suppressed stellar mass growth, as well as differences in accreted vs.
in-situ star formation between satellites and the field, are of secondary
importance.},
  added-at = {2016-09-13T10:34:04.000+0200},
  author = {Bahe, Yannick M. and Schaye, Joop and Crain, Robert A. and McCarthy, Ian G. and Bower, Richard G. and Theuns, Tom and McGee, Sean L. and Trayford, James W.},
  biburl = {https://www.bibsonomy.org/bibtex/24bc5e6af81d3638dee6d9db4403e7b07/miki},
  description = {[1609.03379] The origin of the enhanced metallicity of satellite galaxies},
  interhash = {ac6c1f292b5a7b5e6854460040177b75},
  intrahash = {4bc5e6af81d3638dee6d9db4403e7b07},
  keywords = {environment simulations satellite metallicity},
  note = {cite arxiv:1609.03379Comment: 22 pages, 15 figures; accepted by MNRAS},
  timestamp = {2016-09-13T10:34:16.000+0200},
  title = {The origin of the enhanced metallicity of satellite galaxies},
  url = {http://arxiv.org/abs/1609.03379},
  year = 2016
}

{"_id":"3eEwxEHQXq3qbwyko","bibbaseid":"bahe-schaye-crain-mccarthy-bower-theuns-mcgee-trayford-theoriginoftheenhancedmetallicityofsatellitegalaxies-2016","author_short":["Bahe, Y. M.","Schaye, J.","Crain, R. A.","McCarthy, I. G.","Bower, R. G.","Theuns, T.","McGee, S. L.","Trayford, J. W."],"bibdata":{"bibtype":"misc","type":"misc","abstract":"Observations of galaxies in the local Universe have shown that both the ionized gas and the stars of satellites are more metal-rich than of equally massive centrals. To gain insight into the connection between this metallicity enhancement and other differences between centrals and satellites, such as their star formation rates, gas content, and growth history, we study the metallicities of >3600 galaxies with M_star > 10^10 M_sun in the cosmological hydrodynamical EAGLE 100 Mpc `Reference' simulation, including  1500 in the vicinity of galaxy groups and clusters (M_200 >= 10^13 M_sun). The simulation predicts excess gas and stellar metallicities in satellites consistent with observations, except for stellar metallicities at M_star <  10^10.2 M_sun where the predicted excess is smaller than observed. The exact magnitude of the effect depends on galaxy selection, aperture, and on whether the metallicity is weighted by stellar mass or luminosity. The stellar metallicity excess in clusters is also sensitive to the efficiency scaling of star formation feedback. We identify stripping of low-metallicity gas from the galaxy outskirts, as well as suppression of metal-poor inflows towards the galaxy centre, as key drivers of the enhancement of gas metallicity. Stellar metallicities in satellites are higher than in the field as a direct consequence of the more metal-rich star forming gas, whereas stripping of stars and suppressed stellar mass growth, as well as differences in accreted vs. in-situ star formation between satellites and the field, are of secondary importance.","added-at":"2016-09-13T10:34:04.000+0200","author":[{"propositions":[],"lastnames":["Bahe"],"firstnames":["Yannick","M."],"suffixes":[]},{"propositions":[],"lastnames":["Schaye"],"firstnames":["Joop"],"suffixes":[]},{"propositions":[],"lastnames":["Crain"],"firstnames":["Robert","A."],"suffixes":[]},{"propositions":[],"lastnames":["McCarthy"],"firstnames":["Ian","G."],"suffixes":[]},{"propositions":[],"lastnames":["Bower"],"firstnames":["Richard","G."],"suffixes":[]},{"propositions":[],"lastnames":["Theuns"],"firstnames":["Tom"],"suffixes":[]},{"propositions":[],"lastnames":["McGee"],"firstnames":["Sean","L."],"suffixes":[]},{"propositions":[],"lastnames":["Trayford"],"firstnames":["James","W."],"suffixes":[]}],"biburl":"https://www.bibsonomy.org/bibtex/24bc5e6af81d3638dee6d9db4403e7b07/miki","description":"[1609.03379] The origin of the enhanced metallicity of satellite galaxies","interhash":"ac6c1f292b5a7b5e6854460040177b75","intrahash":"4bc5e6af81d3638dee6d9db4403e7b07","keywords":"environment simulations satellite metallicity","note":"cite arxiv:1609.03379Comment: 22 pages, 15 figures; accepted by MNRAS","timestamp":"2016-09-13T10:34:16.000+0200","title":"The origin of the enhanced metallicity of satellite galaxies","url":"http://arxiv.org/abs/1609.03379","year":"2016","bibtex":"@misc{bahe2016origin,\n abstract = {Observations of galaxies in the local Universe have shown that both the\r\nionized gas and the stars of satellites are more metal-rich than of equally\r\nmassive centrals. To gain insight into the connection between this metallicity\r\nenhancement and other differences between centrals and satellites, such as\r\ntheir star formation rates, gas content, and growth history, we study the\r\nmetallicities of >3600 galaxies with M_star > 10^10 M_sun in the cosmological\r\nhydrodynamical EAGLE 100 Mpc `Reference' simulation, including ~1500 in the\r\nvicinity of galaxy groups and clusters (M_200 >= 10^13 M_sun). The simulation\r\npredicts excess gas and stellar metallicities in satellites consistent with\r\nobservations, except for stellar metallicities at M_star <~ 10^10.2 M_sun where\r\nthe predicted excess is smaller than observed. The exact magnitude of the\r\neffect depends on galaxy selection, aperture, and on whether the metallicity is\r\nweighted by stellar mass or luminosity. The stellar metallicity excess in\r\nclusters is also sensitive to the efficiency scaling of star formation\r\nfeedback. We identify stripping of low-metallicity gas from the galaxy\r\noutskirts, as well as suppression of metal-poor inflows towards the galaxy\r\ncentre, as key drivers of the enhancement of gas metallicity. Stellar\r\nmetallicities in satellites are higher than in the field as a direct\r\nconsequence of the more metal-rich star forming gas, whereas stripping of stars\r\nand suppressed stellar mass growth, as well as differences in accreted vs.\r\nin-situ star formation between satellites and the field, are of secondary\r\nimportance.},\n added-at = {2016-09-13T10:34:04.000+0200},\n author = {Bahe, Yannick M. and Schaye, Joop and Crain, Robert A. and McCarthy, Ian G. and Bower, Richard G. and Theuns, Tom and McGee, Sean L. and Trayford, James W.},\n biburl = {https://www.bibsonomy.org/bibtex/24bc5e6af81d3638dee6d9db4403e7b07/miki},\n description = {[1609.03379] The origin of the enhanced metallicity of satellite galaxies},\n interhash = {ac6c1f292b5a7b5e6854460040177b75},\n intrahash = {4bc5e6af81d3638dee6d9db4403e7b07},\n keywords = {environment simulations satellite metallicity},\n note = {cite arxiv:1609.03379Comment: 22 pages, 15 figures; accepted by MNRAS},\n timestamp = {2016-09-13T10:34:16.000+0200},\n title = {The origin of the enhanced metallicity of satellite galaxies},\n url = {http://arxiv.org/abs/1609.03379},\n year = 2016\n}\n\n","author_short":["Bahe, Y. 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