Metallicities in cosmological simulations with AGN feedback

Chiaki Kobayashi; Philip Taylor

doi:10.1017/S1743921315010352

Metallicities in cosmological simulations with AGN feedback

Research output: Contribution to journal › Conference article › peer-review

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.

Original language	English
Pages (from-to)	60-60
Number of pages	1
Journal	Proceedings of the International Astronomical Union
Volume	11
Issue number	S319
DOIs	https://doi.org/10.1017/S1743921315010352
Publication status	E-pub ahead of print - 17 Aug 2016

Keywords

galaxies: abundances
galaxies: evolution
galaxies: formation

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Cite this

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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.",

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author = "Chiaki Kobayashi and Philip Taylor",

note = "{\textcopyright} International Astronomical Union 2016.",

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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

SN - 1743-9213

VL - 11

SP - 60

EP - 60

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

IS - S319

ER -

Metallicities in cosmological simulations with AGN feedback

Abstract

Keywords

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