How to zoom: bias, contamination and Lagrange volumes in multimass cosmological simulations

Oñorbe, José; Garrison-Kimmel, Shea; Maller, Ariyeh H.; Bullock, James S.; Rocha, Miguel; Hahn, Oliver

doi:10.1093/mnras/stt2020

Cited by 150 publications

(144 citation statements)

References 48 publications

(59 reference statements)

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“…Most of them have been presented in Hopkins et al (2014). The simulations m09 and m10 are isolated dwarfs, constructed using the method from Oñorbe et al (2014). Simulations m10v, m11, m11v, m12q, m12i, and m13 are chosen to match the initial conditions from the AGORA project (Kim et al 2014), which will enable future comparisons with a wide range of simulation codes and physics implementations.…”

Section: Simulation Detailsmentioning

confidence: 99%

The origin and evolution of the galaxy mass–metallicity relation

Ma¹,

Hopkins²,

Faucher-Giguère³

et al. 2015

Mon. Not. R. Astron. Soc.

435

463

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We use high-resolution cosmological zoom-in simulations from the Feedback in Realistic Environment (FIRE) project to study the galaxy mass-metallicity relations (MZR) from z = 0-6. These simulations include explicit models of the multi-phase ISM, star formation, and stellar feedback. The simulations cover halo masses M halo = 10 9 -10 13 M and stellar masses M * = 10 4 -10 11 M at z = 0 and have been shown to produce many observed galaxy properties from z = 0-6. For the first time, our simulations agree reasonably well with the observed mass-metallicity relations at z = 0-3 for a broad range of galaxy masses. We predict the evolution of the MZR from z = 0-6, as log( 04, for gas-phase and stellar metallicity, respectively. Our simulations suggest that the evolution of MZR is associated with the evolution of stellar/gas mass fractions at different redshifts, indicating the existence of a universal metallicity relation between stellar mass, gas mass, and metallicities. In our simulations, galaxies above M * = 10 6 M are able to retain a large fraction of their metals inside the halo, because metal-rich winds fail to escape completely and are recycled into the galaxy. This resolves a long-standing discrepancy between "sub-grid" wind models (and semi-analytic models) and observations, where common sub-grid models cannot simultaneously reproduce the MZR and the stellar mass functions.

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Section: Simulation Detailsmentioning

confidence: 99%

The origin and evolution of the galaxy mass–metallicity relation

Ma¹,

Hopkins²,

Faucher-Giguère³

et al. 2015

Mon. Not. R. Astron. Soc.

435

463

View full text Add to dashboard Cite

show abstract

“…We have taken into account two things: first we wanted them to be cheap in terms of cpu cost and second we wanted them to be representative of the dwarf galaxy halo population. We point to Oñorbe et al (2014) for a full description of the method. Here we just want to show how the properties of our selected halos compare with a realistic sample of dwarf galaxy halos.…”

Section: Appendix A: Dark Matter Properties and Evolution In The Colimentioning

confidence: 99%

Forged in fire: cusps, cores and baryons in low-mass dwarf galaxies

Oñorbe

Boylan-Kolchin

Bullock

et al. 2015

Mon. Not. R. Astron. Soc.

391

414

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We present multiple ultra-high resolution cosmological hydrodynamic simulations of M 10 4−6.3 M dwarf galaxies that form within two M vir = 10 9.5−10 M dark matter halo initial conditions. Our simulations rely on the FIRE implementation of star formation feedback and were run with high enough force and mass resolution to directly resolve structure on the ∼ 200 pc scales. The resultant galaxies sit on the M vs. M vir relation required to match the Local Group stellar mass function via abundance matching. They have bursty star formation histories and also form with half-light radii and metallicities that broadly match those observed for local dwarfs at the same stellar mass. We demonstrate that it is possible to create a large (∼ 1 kpc) constant-density dark matter core in a cosmological simulation of an M 10 6.3 M dwarf galaxy within a typical M vir = 10 10 M halo -precisely the scale of interest for resolving the Too Big to Fail problem. However, these large cores are not ubiquitous and appear to correlate closely with the star formation histories of the dwarfs: dark matter cores are largest in systems that form their stars late (z 2), after the early epoch of cusp building mergers has ended. Our M 10 4 M dwarf retains a cuspy dark matter halo density profile that matches that of a dark-matter only run of the same system. Though ancient, most of the stars in our ultra-faint form after reionization; the UV field acts mainly to suppress fresh gas accretion, not to boil away gas that is already present in the proto-dwarf.

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“…We simulate each galaxy individually using the cosmological "zoom-in" technique (Porter 1985), following the method outlined in Oñorbe et al (2014). We first run several lowerresolution dark-matter-only cosmological simulations at uniform resolution to identify isolated halos of interest.…”

Section: Fire Simulationsmentioning

confidence: 99%

Breathing Fire: How Stellar Feedback Drives Radial Migration, Rapid Size Fluctuations, and Population Gradients in Low-Mass Galaxies

El-Badry

Wetzel

Geha

et al. 2016

ApJ

285

306

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We examine the effects of stellar feedback and bursty star formation on low-mass galaxies (M star =2×10 6 −5×1010 M e ) using the Feedback in Realistic Environments (FIRE) simulations. While previous studies emphasized the impact of feedback on dark matter profiles, we investigate the impact on the stellar component: kinematics, radial migration, size evolution, and population gradients. Feedback-driven outflows/ inflows drive significant radial stellar migration over both short and long timescales via two processes: (1) outflowing/infalling gas can remain star-forming, producing young stars that migrate ∼1 kpc within their first 100 Myr, and (2) gas outflows/inflows drive strong fluctuations in the global potential, transferring energy to all stars. These processes produce several dramatic effects. First, galaxies' effective radii can fluctuate by factors of >2 over ∼200 Myr, and these rapid size fluctuations can account for much of the observed scatter in the radius at fixed M star . Second, the cumulative effects of many outflow/infall episodes steadily heat stellar orbits, causing old stars to migrate outward most strongly. This age-dependent radial migration mixes-and even inverts-intrinsic age and metallicity gradients. Thus, the galactic-archaeology approach of calculating radial star formation histories from stellar populations at z=0 can be severely biased. These effects are strongest at M star ≈10 7-9.6 M e , the same regime where feedback most efficiently cores galaxies. Thus, detailed measurements of stellar kinematics in low-mass galaxies can strongly constrain feedback models and test baryonic solutions to small-scale problems in ΛCDM.

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How to zoom: bias, contamination and Lagrange volumes in multimass cosmological simulations

Cited by 150 publications

References 48 publications

The origin and evolution of the galaxy mass–metallicity relation

The origin and evolution of the galaxy mass–metallicity relation

Forged in fire: cusps, cores and baryons in low-mass dwarf galaxies

Breathing Fire: How Stellar Feedback Drives Radial Migration, Rapid Size Fluctuations, and Population Gradients in Low-Mass Galaxies

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