Four phases of angular-momentum buildup in high-z galaxies: from cosmic-web streams through an extended ring to disc and bulge

Danovich, Mark; Dekel, Avishai; Hahn, Oliver; Ceverino, Daniel; Primack, Joel R.

doi:10.1093/mnras/stv270

Cited by 293 publications

(436 citation statements)

References 113 publications

(174 reference statements)

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“…In particular, the simulations are denser by a factor ∼2 at z < 2. One possible explanation is that the baryons in the simulations loses angular momentum during its collapse, as described in Danovich et al (2014). In fact, found in the same simulations used here a systematic trend ofλ with redshift (see their Figure 12).…”

Section: Evolution Of the Surface Density Within Resupporting

confidence: 54%

Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers

Ceverino

Dekel

Tweed

et al. 2015

Monthly Notices of the Royal Astronomical Society

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101

100

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We address the formation of massive stellar spheroids between redshifts z = 4 and 1 using a suite of AMR hydro-cosmological simulations. The spheroids form as bulges, and the spheroid mass growth is partly driven by violent disc instability (VDI) and partly by mergers. A kinematic decomposition to disc and spheroid yields that the mass fraction in the spheroid is between 50% and 90% and is roughly constant in time, consistent with a cosmological steady state of VDI discs that are continuously fed from the cosmic web. The density profile of the spheroid is typically "classical", with a Sersic index n = 4.5 ± 1, independent of whether it grew by mergers or VDI and independent of the feedback strength. The disc is characterized by n = 1.5±0.5, and the whole galaxy by n = 3±1. The high-redshift spheroids are compact due to the dissipative inflow of gas and the high universal density. The stellar surface density within the effective radius of each galaxy as it evolves remains roughly constant in time after its first growth. For galaxies of a fixed stellar mass, the surface density is higher at higher redshifts.

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Section: Evolution Of the Surface Density Within Resupporting

confidence: 54%

Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers

Ceverino

Dekel

Tweed

et al. 2015

Monthly Notices of the Royal Astronomical Society

Self Cite

101

100

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“…with the goal of studying in more detail the dependence and constrain seed black hole scenarios. We note that (Danovich et al 2015, and references therein) have studied in detail the angular-momentum buildup in high − z massive galaxies using high-resolution zoom cosmological simulations and have explicitly studied the link with early disc formation and tidal field theory. In our work we illustrate that black hole formation and angular momentum buildup can be understood within the same context.…”

Section: Discussionmentioning

confidence: 99%

The origin of the most massive black holes at high-z: BlueTides and the next quasar frontier

Matteo

Croft

Feng

et al. 2017

Monthly Notices of the Royal Astronomical Society

109

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The growth of the most massive black holes in the early universe, consistent with the detection of highly luminous quasars at z > 6 implies sustained, critical accretion of material to grow and power them. Given a black hole seed scenario, it is still uncertain which conditions in the early Universe allow the fastest black hole growth. Large scale hydrodynamical cosmological simulations of structure formation allow us to explore the conditions conducive to the growth of the earliest supermassive black holes. We use the cosmological hydrodynamic simulation BlueTides, which incorporates a variety of baryon physics in a (400h −1 Mpc) 3 volume with 0.7 trillion particles to follow the earliest phases of black hole critical growth. At z = 8 the most massive black holes (a handful) approach masses of 10 8 M with the most massive (with M BH = 4 × 10 8 M ) being found in an extremely compact spheroid-dominated host galaxy. Examining the large-scale environment of hosts, we find that the initial tidal field is more important than overdensity in setting the conditions for early BH growth. In regions of low tidal fields gas accretes 'cold' onto the black hole and falls along thin, radial filaments straight into the center forming the most compact galaxies and most massive black holes at earliest times. Regions of high tidal fields instead induce larger coherent angular momenta and influence the formation of the first population of massive compact disks. The extreme early growth depends on the early interplay of high gas densities and the tidal field that shapes the mode of accretion. Mergers play a minor role in the formation of the first generation, rare massive BHs.

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“…Cosmological hydrodynamic simulations have shown that the angular momentum of the gas is not conserved during infall (Kimm et al 2011;Danovich et al 2015). However, even though Eq.…”

Section: Disc Radii and Rotation Speedsmentioning

confidence: 99%

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

Cattaneo

Blaizot

Devriendt

et al. 2017

Monthly Notices of the Royal Astronomical Society

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GalICS 2.0 is a new semianalytic code to model the formation and evolution of galaxies in a cosmological context. N-body simulations based on a Planck cosmology are used to construct halo merger trees, track subhaloes, compute spins and measure concentrations. The accretion of gas onto galaxies and the morphological evolution of galaxies are modelled with prescriptions derived from hydrodynamic simulations. Star formation and stellar feedback are described with phenomenological models (as in other semianalytic codes). GalICS 2.0 computes rotation speeds from the gravitational potential of the dark matter, the disc and the central bulge. As the rotation speed depends not only on the virial velocity but also on the ratio of baryons to dark matter within a galaxy, our calculation predicts a different Tully-Fisher relation from models in which v rot ∝ v vir . This is why GalICS 2.0 is able to reproduce the galaxy stellar mass function and the Tully-Fisher relation simultaneously. Our results are also in agreement with halo masses from weak lensing and satellite kinematics, gas fractions, the relation between star formation rate (SFR) and stellar mass, the evolution of the cosmic SFR density, bulge-to-disc ratios, disc sizes and the Faber-Jackson relation.

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Four phases of angular-momentum buildup in high-z galaxies: from cosmic-web streams through an extended ring to disc and bulge

Cited by 293 publications

References 113 publications

Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers

Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers

The origin of the most massive black holes at high-z: BlueTides and the next quasar frontier

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

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