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.
引用
收藏
页码:2153 / 2169
页数:17
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