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Metallicities in cosmological simulations with AGN feedback

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Metallicities in cosmological simulations with AGN feedback. / Kobayashi, Chiaki; Taylor, Philip.

In: Proceedings of the International Astronomical Union, Vol. 11, No. S319, 17.08.2016, p. 60-60.

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@article{0bc9bead75f84ac3af313775954ef950,
title = "Metallicities in cosmological simulations with AGN feedback",
abstract = "In our cosmological, chemodynamical simulations, (i) the black hole mass–velocity dispersion relation does not evolve, and black holes actually grow along the relation. (ii) the stellar mass–metallicity relation does not change its shape, while the gas-phase relation has a steeper slope at higher redshifts. (iii) While stellar metallicity gradients are made shallower by galaxy mergers, gas-phase gradients are affected more strongly by AGN feedback.",
keywords = "galaxies: abundances, galaxies: evolution, galaxies: formation",
author = "Chiaki Kobayashi and Philip Taylor",
note = "{\textcopyright} International Astronomical Union 2016.",
year = "2016",
month = aug,
day = "17",
doi = "10.1017/S1743921315010352",
language = "English",
volume = "11",
pages = "60--60",
journal = "Proceedings of the International Astronomical Union",
issn = "1743-9213",
publisher = "Cambridge University Press",
number = "S319",

}

RIS

TY - JOUR

T1 - Metallicities in cosmological simulations with AGN feedback

AU - Kobayashi, Chiaki

AU - Taylor, Philip

N1 - © International Astronomical Union 2016.

PY - 2016/8/17

Y1 - 2016/8/17

N2 - In our cosmological, chemodynamical simulations, (i) the black hole mass–velocity dispersion relation does not evolve, and black holes actually grow along the relation. (ii) the stellar mass–metallicity relation does not change its shape, while the gas-phase relation has a steeper slope at higher redshifts. (iii) While stellar metallicity gradients are made shallower by galaxy mergers, gas-phase gradients are affected more strongly by AGN feedback.

AB - In our cosmological, chemodynamical simulations, (i) the black hole mass–velocity dispersion relation does not evolve, and black holes actually grow along the relation. (ii) the stellar mass–metallicity relation does not change its shape, while the gas-phase relation has a steeper slope at higher redshifts. (iii) While stellar metallicity gradients are made shallower by galaxy mergers, gas-phase gradients are affected more strongly by AGN feedback.

KW - galaxies: abundances

KW - galaxies: evolution

KW - galaxies: formation

U2 - 10.1017/S1743921315010352

DO - 10.1017/S1743921315010352

M3 - Conference article

VL - 11

SP - 60

EP - 60

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

IS - S319

ER -