NIHAO - XXVIII. Collateral effects of AGN on dark matter concentration and stellar kinematics

Stefan Waterval; Sana Elgamal; Matteo Nori; Mario Pasquato; Andrea V. MacCiò; Marvin Blank; Keri L. Dixon; Xi Kang; Tengiz Ibrayev

doi:10.1093/mnras/stac1191

NIHAO - XXVIII. Collateral effects of AGN on dark matter concentration and stellar kinematics

Stefan Waterval, Sana Elgamal, Matteo Nori, Mario Pasquato, Andrea V. MacCiò, Marvin Blank, Keri L. Dixon, Xi Kang, Tengiz Ibrayev

Physics

Research output: Contribution to journal › Article › peer-review

Abstract

Although active galactic nuclei (AGN) feedback is required in simulations of galaxies to regulate star formation, further downstream effects on the dark matter (DM) distribution of the halo and stellar kinematics of the central galaxy can be expected. We combine simulations of galaxies with and without AGN physics from the Numerical Investigation of a Hundred Astrophysical Objects (NIHAO) to investigate the effect of AGN on the DM profile and central stellar rotation of the host galaxies. Specifically, we study how the concentration-halo mass (c-M) relation and the stellar spin parameter (λR) are affected by AGN feedback. We find that AGN physics is crucial to reduce the central density of simulated massive (≥1012 M⊙) galaxies and bring their concentration to agreement with results from the Spitzer Photometry & Accurate Rotation Curves (SPARC) sample. Similarly, AGN feedback has a key role in reproducing the dichotomy between slow and fast rotators as observed by the ATLAS3D survey. Without star formation suppression due to AGN feedback, the number of fast rotators strongly exceeds the observational constraints. Our study shows that there are several collateral effects that support the importance of AGN feedback in galaxy formation, and these effects can be used to constrain its implementation in numerical simulations.

Original language	English (US)
Pages (from-to)	5307-5319
Number of pages	13
Journal	Monthly Notices of the Royal Astronomical Society
Volume	514
Issue number	4
DOIs	https://doi.org/10.1093/mnras/stac1191
State	Published - Aug 1 2022

Keywords

galaxies: evolution
galaxies: formation
methods: numerical
methods: statistical

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/stac1191

Cite this

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title = "NIHAO - XXVIII. Collateral effects of AGN on dark matter concentration and stellar kinematics",

abstract = "Although active galactic nuclei (AGN) feedback is required in simulations of galaxies to regulate star formation, further downstream effects on the dark matter (DM) distribution of the halo and stellar kinematics of the central galaxy can be expected. We combine simulations of galaxies with and without AGN physics from the Numerical Investigation of a Hundred Astrophysical Objects (NIHAO) to investigate the effect of AGN on the DM profile and central stellar rotation of the host galaxies. Specifically, we study how the concentration-halo mass (c-M) relation and the stellar spin parameter (λR) are affected by AGN feedback. We find that AGN physics is crucial to reduce the central density of simulated massive (≥1012 M⊙) galaxies and bring their concentration to agreement with results from the Spitzer Photometry & Accurate Rotation Curves (SPARC) sample. Similarly, AGN feedback has a key role in reproducing the dichotomy between slow and fast rotators as observed by the ATLAS3D survey. Without star formation suppression due to AGN feedback, the number of fast rotators strongly exceeds the observational constraints. Our study shows that there are several collateral effects that support the importance of AGN feedback in galaxy formation, and these effects can be used to constrain its implementation in numerical simulations.",

keywords = "galaxies: evolution, galaxies: formation, methods: numerical, methods: statistical",

author = "Stefan Waterval and Sana Elgamal and Matteo Nori and Mario Pasquato and MacCi{\`o}, {Andrea V.} and Marvin Blank and Dixon, {Keri L.} and Xi Kang and Tengiz Ibrayev",

note = "Funding Information: We are grateful to the authors of L20 who kindly agreed to share their data with us. This material is based upon work supported by Tamkeen under the NYU Abu Dhabi Research Institute grant CAP 3 (Center for Astro, Particle, and Planetary Physics). The authors gratefully acknowledge the Gauss Centre for Supercomputing e.V. (www.gaus s-centre.eu) for funding this project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (http://www.lrz.de) and the High Performance Computing resources at New York University Abu Dhabi. MP acknowledges financial support from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 896248. Publisher Copyright: {\textcopyright} 2022 The Author(s).",

year = "2022",

month = aug,

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doi = "10.1093/mnras/stac1191",

language = "English (US)",

volume = "514",

pages = "5307--5319",

journal = "Monthly Notices of the Royal Astronomical Society",

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T1 - NIHAO - XXVIII. Collateral effects of AGN on dark matter concentration and stellar kinematics

AU - Waterval, Stefan

AU - Elgamal, Sana

AU - Nori, Matteo

AU - Pasquato, Mario

AU - MacCiò, Andrea V.

AU - Blank, Marvin

AU - Dixon, Keri L.

AU - Kang, Xi

AU - Ibrayev, Tengiz

N1 - Funding Information: We are grateful to the authors of L20 who kindly agreed to share their data with us. This material is based upon work supported by Tamkeen under the NYU Abu Dhabi Research Institute grant CAP 3 (Center for Astro, Particle, and Planetary Physics). The authors gratefully acknowledge the Gauss Centre for Supercomputing e.V. (www.gaus s-centre.eu) for funding this project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (http://www.lrz.de) and the High Performance Computing resources at New York University Abu Dhabi. MP acknowledges financial support from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 896248. Publisher Copyright: © 2022 The Author(s).

PY - 2022/8/1

Y1 - 2022/8/1

N2 - Although active galactic nuclei (AGN) feedback is required in simulations of galaxies to regulate star formation, further downstream effects on the dark matter (DM) distribution of the halo and stellar kinematics of the central galaxy can be expected. We combine simulations of galaxies with and without AGN physics from the Numerical Investigation of a Hundred Astrophysical Objects (NIHAO) to investigate the effect of AGN on the DM profile and central stellar rotation of the host galaxies. Specifically, we study how the concentration-halo mass (c-M) relation and the stellar spin parameter (λR) are affected by AGN feedback. We find that AGN physics is crucial to reduce the central density of simulated massive (≥1012 M⊙) galaxies and bring their concentration to agreement with results from the Spitzer Photometry & Accurate Rotation Curves (SPARC) sample. Similarly, AGN feedback has a key role in reproducing the dichotomy between slow and fast rotators as observed by the ATLAS3D survey. Without star formation suppression due to AGN feedback, the number of fast rotators strongly exceeds the observational constraints. Our study shows that there are several collateral effects that support the importance of AGN feedback in galaxy formation, and these effects can be used to constrain its implementation in numerical simulations.

AB - Although active galactic nuclei (AGN) feedback is required in simulations of galaxies to regulate star formation, further downstream effects on the dark matter (DM) distribution of the halo and stellar kinematics of the central galaxy can be expected. We combine simulations of galaxies with and without AGN physics from the Numerical Investigation of a Hundred Astrophysical Objects (NIHAO) to investigate the effect of AGN on the DM profile and central stellar rotation of the host galaxies. Specifically, we study how the concentration-halo mass (c-M) relation and the stellar spin parameter (λR) are affected by AGN feedback. We find that AGN physics is crucial to reduce the central density of simulated massive (≥1012 M⊙) galaxies and bring their concentration to agreement with results from the Spitzer Photometry & Accurate Rotation Curves (SPARC) sample. Similarly, AGN feedback has a key role in reproducing the dichotomy between slow and fast rotators as observed by the ATLAS3D survey. Without star formation suppression due to AGN feedback, the number of fast rotators strongly exceeds the observational constraints. Our study shows that there are several collateral effects that support the importance of AGN feedback in galaxy formation, and these effects can be used to constrain its implementation in numerical simulations.

KW - galaxies: evolution

KW - galaxies: formation

KW - methods: numerical

KW - methods: statistical

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U2 - 10.1093/mnras/stac1191

DO - 10.1093/mnras/stac1191

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VL - 514

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JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

NIHAO - XXVIII. Collateral effects of AGN on dark matter concentration and stellar kinematics

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