Self-interacting dark matter and the delay of supermassive black hole growth

被引:7
|
作者
Cruz, A. [1 ]
Pontzen, A. [2 ]
Volonteri, M. [3 ]
Quinn, T. R. [4 ]
Tremmel, M. [5 ]
Brooks, A. M. [6 ]
Sanchez, N. N. [4 ]
Munshi, F. [7 ]
Di Cintio, A. [8 ,9 ]
机构
[1] Univ Washington, Dept Phys, Seattle, WA 98195 USA
[2] UCL, Dept Phys & Astron, 132 Hampstead Rd, London NW1 2PS, England
[3] Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France
[4] Univ Washington, Dept Astron, Seattle, WA 98195 USA
[5] Yale Ctr Astron & Astrophys, Phys Dept, POB 208120, New Haven, CT 06520 USA
[6] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd Piscataway, Piscataway, NJ 08854 USA
[7] Univ Oklahoma, Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA
[8] Inst Astrofis Canarias, Calle Via Lactea S-N, E-38206 Tenerife, Spain
[9] Univ La Laguna, Avda Astrofis Fco Sanchez, E-38208 Tenerife, Spain
基金
美国国家科学基金会; 美国国家航空航天局; 欧盟地平线“2020”;
关键词
black hole physics; hydrodynamics; galaxies: formation; galaxies: star formation; dark matter; ACTIVE GALACTIC NUCLEI; COSMOLOGICAL SIMULATIONS; DENSITY PROFILES; DWARF GALAXIES; DYNAMICAL FRICTION; MASS MODELS; EVOLUTION; FEEDBACK; HALOES; CORES;
D O I
10.1093/mnras/staa3389
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Using cosmological hydrodynamic simulations with physically motivated models of supermassive black hole (SMBH) formation and growth, we compare the assembly of Milky Way-mass (M-vir approximate to 7 x 10(11)M(circle dot) at z = 0) galaxies in cold dark matter (CDM) and self-interacting dark matter (SIDM) models. Our SIDM model adopts a constant cross-section of 1 cm(2) g(-1). We find that SMBH formation is suppressed in the early Universe due to SIDM interactions. SMBH-SMBH mergers are also suppressed in SIDM as a consequence of the lower number of SMBHs formed. Lack of initial merger-driven SMBH growth in turn delays SMBH growth by billions of years in SIDM compared to CDM. Further, we find that this delayed growth suppresses SMBH accretion in the largest progenitors of the main SIDM galaxies during the first 5Gyr of their evolution. Nonetheless, by z = 0.8 the CDM and SIDM SMBH masses differ only by around 0.2 dex, so that both remain compatible with the MBH-M* relation. We show that the reduced accretion causes the SIDM SMBHs to less aggressively regulate star formation in their host galaxies than their CDM counterparts, resulting in a factor of 3 or more stars being produced over the lifetime of the SIDM galaxies compared to the CDM galaxies. Our results highlight a new way in which SIDM can affect the growth and merger history of SMBHs and ultimately give rise to very different galaxy evolution compared to the classic CDM model.
引用
收藏
页码:2177 / 2187
页数:11
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