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Density profile of dark matter haloes and galaxies in the horizon-agn simulation: the impact of AGN feedback
被引:114
作者:
Peirani, Sebastien
[1
,2
,3
,4
,5
]
Dubois, Yohan
[2
,3
]
Volonteri, Marta
[2
,3
]
Devriendt, Julien
[3
,6
,7
]
Bundy, Kevin
[4
]
Silk, Joe
[2
,3
,6
,8
]
Pichon, Christophe
[2
,3
,9
]
Kaviraj, Sugata
[10
]
Gavazzi, Raphael
[2
,3
]
Habouzit, Melanie
[2
,3
,11
]
机构:
[1] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, F-06300 Nice, France
[2] CNRS, UMR 7095, Inst Astrophys Paris, 98 Bis Bd Arago, F-75014 Paris, France
[3] UPMC, 98 Bis Bd Arago, F-75014 Paris, France
[4] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan
[5] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan
[6] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England
[7] Observ Lyon, UMR 5574, 9 Ave Charles Andre, F-69561 St Genis Laval, France
[8] Johns Hopkins Univ, Dept Phys & Astron, Homewood Campus, Baltimore, MD 21218 USA
[9] KIAS, 85 Hoegiro, Seoul 02455, South Korea
[10] Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England
[11] CCA, 160 5th Ave, New York, NY 10010 USA
基金:
新加坡国家研究基金会;
日本学术振兴会;
关键词:
methods: numerical;
galaxies: evolution;
galaxies: haloes;
galaxies: jets;
dark matter;
GALACTIC NUCLEUS FEEDBACK;
CUSP-CORE TRANSFORMATIONS;
SUPERMASSIVE BLACK-HOLE;
HUBBLE-SPACE-TELESCOPE;
MASS-DISTRIBUTION;
COSMOLOGICAL SIMULATIONS;
SIZE EVOLUTION;
DWARF GALAXIES;
STAR-FORMATION;
MINOR MERGERS;
D O I:
10.1093/mnras/stx2099
中图分类号:
P1 [天文学];
学科分类号:
0704 ;
摘要:
Using a suite of three large cosmological hydrodynamical simulations, HORIZON-AGN, HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H-AGN, H-noAGN and H-DM) significantly evolve with time. More specifically, at high redshift (z similar to 5), the mean central density profiles of H-AGN and H-noAGN dark matter haloes tend to be much steeper than their H-DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z similar to 1.5, these mean halo density profiles in H-AGN have flattened, pummelled by powerful AGN activity ('quasar mode'): the integrated inner mass difference gaps with HnoAGN haloes have widened, and those with H-DM haloes have narrowed. Fast forward 9.5 billion years, down to z = 0, and the trend reverses: H-AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ('radio mode'), and the gaps in integrated central mass difference with H-noAGN and H-DM close and broaden, respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations.
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页码:2153 / 2169
页数:17
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