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

被引:7
作者
Waterval, Stefan [1 ,2 ]
Elgamal, Sana [1 ,2 ]
Nori, Matteo [1 ,2 ]
Pasquato, Mario [1 ,2 ,3 ,4 ]
Maccio, Andrea, V [1 ,2 ,5 ]
Blank, Marvin [1 ,2 ,6 ]
Dixon, Keri L. [1 ,2 ]
Kang, Xi [7 ,8 ]
Ibrayev, Tengiz [1 ]
机构
[1] New York Univ Abu Dhabi, POB 129188, Abu Dhabi, U Arab Emirates
[2] New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, POB 129188, Abu Dhabi, U Arab Emirates
[3] Univ Padua, Phys & Astron Dept Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy
[4] Univ Montreal, Dept Phys, Montreal, PQ H3T 1J4, Canada
[5] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
[6] Christian Albrechts Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24118 Kiel, Germany
[7] Zhejiang Univ, Zhejiang Univ Purple Mt Observ Joint Res Ctr Astr, Hangzhou 310027, Peoples R China
[8] Purple Mt Observ, 10 Yuan Hua Rd, Nanjing 210034, Peoples R China
基金
欧盟地平线“2020”;
关键词
methods: numerical; methods: statistical; galaxies: evolution; galaxies: formation; ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATES; EARLY-TYPE GALAXIES; BLACK-HOLES; COSMOLOGICAL SIMULATIONS; ATLAS(3D) PROJECT; DENSITY PROFILES; ANGULAR-MOMENTUM; INNER STRUCTURE; SAURON PROJECT;
D O I
10.1093/mnras/stac1191
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 (lambda(R)) are affected by AGN feedback. We find that AGN physics is crucial to reduce the central density of simulated massive (greater than or similar to 10(12) M-circle dot) 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 ATLAS(3D) 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.
引用
收藏
页码:5307 / 5319
页数:13
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