Modeling high-redshift galaxies: what can we learn from high and ultra-high resolution hydrodynamical simulations?

Devriendt, Julien; Slyz, Adrianne; Powell, Leila C.; Teyssier, Romain

doi:10.1017/s1743921310002863

Cited by 2 publications

(2 citation statements)

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“…The Nut Simulation † is an ultra-high resolution cosmological simulation of a Milky Way like galaxy forming at the intersection of 3 filaments in a ΛCDM cosmology (Slyz et al 2009;Devriendt et al 2010). We perform the simulation with ramses (Teyssier 2002) including cooling, a UV background (Haardt & Madau 1996), SF and SN feedback with metal enrichment (Dubois & Teyssier 2008) achieving a maximum physical spatial resolution of ≈ 0.5pc in the densest regions at all times.…”

Section: Star Formation During Cold-mode Accretion and The Onset Of Amentioning

confidence: 99%

“…SF in the galaxy, its satellites and haloes embedded in the filaments results in many SN explosions, which are individually resolved. The numerous bubbles overlap, creating an extended cavity through which the hot gas escapes the galactic potential in the form of a wind (see Slyz et al 2009;Devriendt et al 2010, for figures illustrating this and additional technical details). By z = 9, when the dark matter halo mass has reached ∼ 10 9 M , the wind extends to ≈ 6r vir , filling the virial sphere with hot, diffuse gas not unlike the shock-heated gaseous halo found in galaxies above the mass threshold for a stable virial shock (e.g.…”

Section: Star Formation During Cold-mode Accretion and The Onset Of Amentioning

confidence: 99%

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Galactic star formation in parsec-scale resolution simulations

et al. 2010

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Abstract. The interstellar medium (ISM) in galaxies is multiphase and cloudy, with stars forming in the very dense, cold gas found in Giant Molecular Clouds (GMCs). Simulating the evolution of an entire galaxy, however, is a computational problem which covers many orders of magnitude, so many simulations cannot reach densities high enough or temperatures low enough to resolve this multiphase nature. Therefore, the formation of GMCs is not captured and the resulting gas distribution is smooth, contrary to observations. We investigate how star formation (SF) proceeds in simulated galaxies when we obtain parsec-scale resolution and more successfully capture the multiphase ISM. Both major mergers and the accretion of cold gas via filaments are dominant contributors to a galaxy's total stellar budget and we examine SF at high resolution in both of these contexts.Keywords. methods: numerical, galaxies: evolution, galaxies: interaction, stars: formation By performing adaptive mesh refinement (AMR) simulations in which we resolve the multiphase ISM and the formation of GMCs, we investigate the nature of galactic SF in two important contexts: major mergers (Section 1) and cold accretion via filaments at high-redshift (Section 2).

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Section: Star Formation During Cold-mode Accretion and The Onset Of Amentioning

confidence: 99%

Section: Star Formation During Cold-mode Accretion and The Onset Of Amentioning

confidence: 99%

Galactic star formation in parsec-scale resolution simulations

et al. 2010

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Black hole–galaxy scaling relations in FIRE: the importance of black hole location and mergers

Çatmabacak

Feldmann

Anglés-Alcázar

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The concurrent growth of supermassive black holes (SMBHs) and their host galaxies remains to be fully explored, especially at high redshift. While often understood as a consequence of self-regulation via AGN feedback, it can also be explained by alternative SMBH accretion models. Here, we expand on previous work by studying the growth of SMBHs with the help of a large suite of cosmological zoom-in simulations (MassiveFIRE) that are part of the Feedback in Realistic Environments (FIRE) project. The growth of SMBHs is modelled in post-processing with different black hole accretion models, placements, and merger treatments, and validated by comparing to on-the-fly calculations. Scaling relations predicted by the gravitational torque driven accretion (GTDA) model agree with observations at low redshift without the need for AGN feedback, in contrast to models in which the accretion rate depends strongly on SMBH mass. At high redshift, we find deviations from the local scaling relations in line with previous theoretical results. In particular, SMBHs are under-massive, presumably due to stellar feedback, but start to grow efficiently once their host galaxies reach M* ∼ 1010M⊙. We analyse and explain these findings in the context of a simple analytic model. Finally, we show that the predicted scaling relations depend sensitively on the SMBH location and the efficiency of SMBH merging, particularly in low-mass systems. These findings highlight the relevance of understanding the evolution of SMBH-galaxy scaling relations to predict the rate of gravitational wave signals from SMBH mergers across cosmic history.

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Modeling high-redshift galaxies: what can we learn from high and ultra-high resolution hydrodynamical simulations?

Cited by 2 publications

References 19 publications

Galactic star formation in parsec-scale resolution simulations

Galactic star formation in parsec-scale resolution simulations

Black hole–galaxy scaling relations in FIRE: the importance of black hole location and mergers

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