GenetIC—A New Initial Conditions Generator to Support Genetically Modified Zoom Simulations

Stopyra, Stephen; Pontzen, Andrew; Peiris, Hiranya V.; Roth, Nina; Rey, Martin P.

doi:10.3847/1538-4365/abcd94

Cited by 34 publications

(21 citation statements)

References 34 publications

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“…Such approaches were pioneered by Katz et al (1994), Bertschinger (2001), and then extended to higher accuracy and 2LPT perturbation theory using a tree-based approach by Jenkins (2010) which is implemented in a non-public code used by the VIRGO consortium, and using multi-grid techniques by Hahn and Abel (2011) in the publicly available MUSIC-1 code 18 . A recent addition is the GENET-IC code 19 (Stopyra et al 2021) that focuses on the application of constraints (cf. Sect.…”

Section: Zoom Simulationsmentioning

confidence: 99%

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Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

101

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We review the field of collisionless numerical simulations for the large-scale structure of the Universe. We start by providing the main set of equations solved by these simulations and their connection with General Relativity. We then recap the relevant numerical approaches: discretization of the phase-space distribution (focusing on N-body but including alternatives, e.g., Lagrangian submanifold and Schrödinger–Poisson) and the respective techniques for their time evolution and force calculation (direct summation, mesh techniques, and hierarchical tree methods). We pay attention to the creation of initial conditions and the connection with Lagrangian Perturbation Theory. We then discuss the possible alternatives in terms of the micro-physical properties of dark matter (e.g., neutralinos, warm dark matter, QCD axions, Bose–Einstein condensates, and primordial black holes), and extensions to account for multiple fluids (baryons and neutrinos), primordial non-Gaussianity and modified gravity. We continue by discussing challenges involved in achieving highly accurate predictions. A key aspect of cosmological simulations is the connection to cosmological observables, we discuss various techniques in this regard: structure finding, galaxy formation and baryonic modelling, the creation of emulators and light-cones, and the role of machine learning. We finalise with a recount of state-of-the-art large-scale simulations and conclude with an outlook for the next decade.

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Section: Zoom Simulationsmentioning

confidence: 99%

“…A further technique related to constrained realisations has been termed as 'genetic modification' (Roth et al 2016;Stopyra et al 2021). Its main idea is to impose constraints, not in order to be compatible with the Local Universe, but to perform controlled numerical experiments.…”

Section: Real Universes: Constrained Realisationsmentioning

confidence: 99%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

101

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“…Future work that expands the available suite of MW-like simulations (Buch et al in prep. ) and explores modifications to zoom-in initial conditions to engineer MW-like mass accretion histories (e.g., Roth et al 2016;Stopyra et al 2021;Rey & Starkenburg 2021) is therefore compelling.…”

Section: Discussionmentioning

confidence: 99%

The Effects of Dark Matter and Baryonic Physics on the Milky Way Subhalo Population in the Presence of the Large Magellanic Cloud

Nadler,

Banerjee,

Adhikari

et al. 2021

Preprint

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Given recent developments in our understanding of the Large Magellanic Cloud (LMC)'s impact on the Milky Way (MW)'s dark matter subhalo population, we compare the signatures of dark matter and baryonic physics on subhalos in MW systems with realistic LMC analogs. In particular, we study the effects of self-interacting dark matter (SIDM), warm dark matter (WDM), and the Galactic disk on the peak maximum circular velocity (V peak ) function, radial distribution, and spatial distribution of MW and LMC-associated subhalos using cosmological dark matter-only zoom-in simulations of MW-plus-LMC systems. For a fixed abundance of subhalos expected to host dwarf galaxies (V peak 20 km s −1 ), SIDM and WDM can produce a similar mass-dependent suppression of the subhalo V peak function, while disk disruption is mass-independent. Subhalos in the inner regions of the MW are preferentially disrupted by both self-interactions and the disk, while suppression in WDM is radially independent. The relative abundance of LMC-associated subhalos is not strongly affected by disk disruption or WDM, but is significantly suppressed in SIDM due to self-interactions with the LMC at early times and with the MW during LMC infall at late times, erasing spatial anisotropy in the MW subhalo population. These results provide avenues to distinguish dark matter and baryonic physics by combining properties of the MW and LMC subhalo populations probed by upcoming observations of satellite galaxies and stellar streams.

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“…Eridanus II is substantially more extended than any of our reference EDGE dwarfs, with half = 299 ± 12 pc. Using the genetic modification approach (Roth et al 2016;Rey & Pontzen 2018;Stopyra et al 2020), we can create alternative mass accretion histories for a galaxy. Rey et al (2019) modified one of the fiducial resolution EDGE dwarfs, Halo1459, such that it assembled later.…”

Section: Core Formation From Minor Mergersmentioning

confidence: 99%

EDGE: two routes to dark matter core formation in ultra-faint dwarfs

Orkney

Read

Rey

et al. 2021

Monthly Notices of the Royal Astronomical Society

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In the standard Lambda cold dark matter paradigm, pure dark matter simulations predict dwarf galaxies should inhabit dark matter haloes with a centrally diverging density ‘cusp’. This is in conflict with observations that typically favour a constant density ‘core’. We investigate this ‘cusp-core problem’ in ‘ultra-faint’ dwarf galaxies simulated as part of the ‘Engineering Dwarfs at Galaxy formation’s Edge’ project. We find, similarly to previous work, that gravitational potential fluctuations within the central region of the simulated dwarfs kinematically heat the dark matter particles, lowering the dwarfs’ central dark matter density. However, these fluctuations are not exclusively caused by gas inflow/outflow, but also by impulsive heating from minor mergers. We use the genetic modification approach on one of our dwarf’s initial conditions to show how a delayed assembly history leads to more late minor mergers and, correspondingly, more dark matter heating. This provides a mechanism by which even ultra-faint dwarfs ($M_* \lt 10^5\, \text{M}_{\odot }$), in which star formation was fully quenched at high redshift, can have their central dark matter density lowered over time. In contrast, we find that late major mergers can regenerate a central dark matter cusp, if the merging galaxy had sufficiently little star formation. The combination of these effects leads us to predict significant stochasticity in the central dark matter density slopes of the smallest dwarfs, driven by their unique star formation and mass assembly histories.

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GenetIC—A New Initial Conditions Generator to Support Genetically Modified Zoom Simulations

Cited by 34 publications

References 34 publications

Large-scale dark matter simulations

Large-scale dark matter simulations

The Effects of Dark Matter and Baryonic Physics on the Milky Way Subhalo Population in the Presence of the Large Magellanic Cloud

EDGE: two routes to dark matter core formation in ultra-faint dwarfs

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