Metallicities in cosmological simulations with AGN feedback

Chiaki Kobayashi; Philip Taylor

doi:10.1017/S1743921315010352

Metallicities in cosmological simulations with AGN feedback

Chiaki Kobayashi, Philip Taylor

Research output: Contribution to journal › 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
Number of pages	1
Journal	Proceedings of the International Astronomical Union
Volume	11
DOIs	https://doi.org/10.1017/S1743921315010352
Publication status	Published - 2015

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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.",

keywords = "galaxies: abundances, galaxies: evolution, galaxies: formation",

author = "Chiaki Kobayashi and Philip Taylor",

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

year = "2015",

doi = "10.1017/S1743921315010352",

language = "English",

volume = "11",

pages = "60",

journal = "Proceedings of the International Astronomical Union",

issn = "1743-9213",

publisher = "Cambridge University Press",

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AU - Kobayashi, Chiaki

AU - Taylor, Philip

PY - 2015

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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

UR - http://www.scopus.com/inward/record.url?scp=84983268319&partnerID=8YFLogxK

U2 - 10.1017/S1743921315010352

DO - 10.1017/S1743921315010352

M3 - Article

SN - 1743-9213

VL - 11

SP - 60

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

ER -

Metallicities in cosmological simulations with AGN feedback

Abstract

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