simba: Cosmological simulations with black hole growth and feedback

Davé, Romeel; Anglés-Alcázar, Daniel; Narayanan, Desika; Li, Qi; Rafieferantsoa, Mika; Appleby, Sarah

doi:10.1093/mnras/stz937

Cited by 832 publications

(1,009 citation statements)

References 166 publications

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“…Assuming this type of prescription has the advantage that it is a relatively simple parametrisation of black hole accretion. In addition, this type of accretion is commonly assumed in almost every state-of-the-art cosmological simulation (e.g., in EAGLE (Schaye et al 2015), HORIZON-AGN (Dubois et al 2014),ILLUSTRIS-TNG (Weinberger et al 2017), MASSIVE-BLACK (Di Matteo et al 2012), BLUE-TIDES (Feng et al 2016)) with the exception of the SIMBA simulations (Davé et al 2019). This allows us to connect our results with other studies.…”

Section: Numerical Setupsupporting

confidence: 58%

How AGN feedback drives the size growth of the first quasars

Vlugt

Costa

2019

Monthly Notices of the Royal Astronomical Society

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Quasars at z = 6 are powered by accretion onto supermassive black holes with masses M BH ∼ 10 9 M . Their rapid assembly requires efficient gas inflow into the galactic nucleus, sustaining black hole accretion at a rate close to the Eddington limit, but also high central star formation rates. Using a set of cosmological 'zoom-in' hydrodynamic simulations performed with the moving mesh code Arepo, we show that z = 6 quasar host galaxies develop extremely tightly bound stellar bulges with peak circular velocities 300 − 500 km s −1 and half-mass radii ≈ 0.5 kpc. Despite their high binding energy, we find that these compact bulges expand at z < 6, with their half-mass radii reaching ≈ 5 kpc by z = 3. The circular velocity drops by factors ≈ 2 from their initial values to 200 − 300 km s −1 at z ≈ 3 and the stellar profile undergoes a cusp-core transformation. By tracking individual stellar populations, we find that the gradual expansion of the stellar component is mainly driven by fluctuations in the gravitational potential induced by bursty AGN feedback. We also find that galaxy size growth and the development of a cored stellar profile does not occur if AGN feedback is ineffective. Our findings suggest that AGN-driven outflows may have profound implications for the internal structure of massive galaxies, possibly accounting for their size growth, the formation of cored ellipticals as well as for the saturation of the M BH − σ seen at high velocity dispersions σ .

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Section: Numerical Setupsupporting

confidence: 58%

How AGN feedback drives the size growth of the first quasars

Vlugt

Costa

2019

Monthly Notices of the Royal Astronomical Society

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“…Recent studies (e.g. Bekki 2013;Mancini et al 2016;McKinnon et al 2016McKinnon et al , 2017McKinnon et al , 2018Aoyama et al 2017;Hirashita et al 2018;Gjergo et al 2018;Davé et al 2019;Hou et al 2019) have implemented mechanisms for tracking dust production and destruction in hydrodynamical simulations. McKinnon et al (2016McKinnon et al ( , 2017 implemented a simplified dust model in the moving mesh code AREPO to investigate dust formation in a diverse sample of galaxies, accounting for thermal sputtering of grains.…”

Section: Previous Modellingmentioning

confidence: 99%

Detailed dust modelling in the L-Galaxies semi-analytic model of galaxy formation

Vijayan

Clay

Thomas

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We implement a detailed dust model into the L-Galaxies semi-analytical model which includes: injection of dust by type II and type Ia supernovae (SNe) and AGB stars; grain growth in molecular clouds; and destruction due to supernova-induced shocks, star formation, and reheating. Our grain growth model follows the dust content in molecular clouds and the inter-cloud medium separately, and allows growth only on pre-existing dust grains. At early times, this can make a significant difference to the dust growth rate. Above z ∼ 8, type II SNe are the primary source of dust, whereas below z ∼ 8, grain growth in molecular clouds dominates, with the total dust content being dominated by the latter below z ∼ 6. However, the detailed history of galaxy formation is important for determining the dust content of any individual galaxy. We introduce a fit to the dust-to-metal (DTM) ratio as a function of metallicity and age, which can be used to deduce the DTM ratio of galaxies at any redshift. At z 3, we find a fairly flat mean relation between metallicity and the DTM, and a positive correlation between metallicity and the dust-to-gas (DTG) ratio, in good agreement with the shape and normalisation of the observed relations. We also match the normalisation of the observed stellar mass -dust mass relation over the redshift range of 0 − 4, and to the dust mass function at z = 0. Our results are important in interpreting observations on the dust content of galaxies across cosmic time, particularly so at high redshift.

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“…As for AGN feedback, the commonly pursued approaches consist in providing the feedback energy to the surrounding medium in the form of thermal or kinetic energy (e.g. Springel et al 2005;Sijacki et al 2007;Dubois et al 2010;Barai et al 2016), or with a combination of the two (Davé et al 2019). The recently pursued direction of investigation aims at simulating the effect of the radiative power of the AGN via the injection of thermal energy, while modelling the outcome of the mechanical power of the AGN by means of outflows in the form of kinetic feedback (e.g.…”

Section: Introductionmentioning

confidence: 99%

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

Valentini

Murante

Borgani

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present simulations of galaxy formation, based on the GADGET-3 code, in which a sub-resolution model for star formation and stellar feedback is interfaced with a new model for AGN feedback. Our sub-resolution model describes a multiphase ISM, accounting for hot and cold gas within the same resolution element: we exploit this feature to investigate the impact of coupling AGN feedback energy to the different phases of the ISM over cosmic time. Our fiducial model considers that AGN feedback energy coupling is driven by the covering factors of the hot and cold phases. We perform a suite of cosmological hydrodynamical simulations of disc galaxies (M halo, DM 2 · 10 12 M , at z = 0), to investigate: (i) the effect of different ways of coupling AGN feedback energy to the multiphase ISM; (ii) the impact of different prescriptions for gas accretion (i.e. only cold gas, both cold and hot gas, with the additional possibility of limiting gas accretion from cold gas with high angular momentum); (iii) how different models of gas accretion and coupling of AGN feedback energy affect the coevolution of supermassive BHs and their host galaxy. We find that at least a share of the AGN feedback energy has to couple with the diffuse gas, in order to avoid an excessive growth of the BH mass. When the BH only accretes cold gas, it experiences a growth that is faster than in the case in which both cold and hot gas are accreted. If the accretion of cold gas with high angular momentum is reduced, the BH mass growth is delayed, the BH mass at z = 0 is reduced by up to an order of magnitude, and the BH is prevented from accreting below z 2, when the galaxy disc forms.

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simba: Cosmological simulations with black hole growth and feedback

Cited by 832 publications

References 166 publications

How AGN feedback drives the size growth of the first quasars

How AGN feedback drives the size growth of the first quasars

Detailed dust modelling in the L-Galaxies semi-analytic model of galaxy formation

Impact of AGN feedback on galaxies and their multiphase ISM across cosmic time

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