An iterative method for the construction of N-body galaxy models in collisionless equilibrium

Yurin, Denis; Springel, Volker

doi:10.1093/mnras/stu1421

Cited by 106 publications

(108 citation statements)

References 35 publications

(37 reference statements)

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“…6 The public Dropbox link is http://goo.gl/8JzbIJ. 7 MAKEDISK is an earlier realization of a code similar to GALIC (Yurin & Springel 2014). GALIC is publicly available, and its website is http://www.hits.org/tap-software-en/galic-code/.…”

Section: Initial Conditionmentioning

confidence: 99%

The Agora High-Resolution Galaxy Simulations Comparison Project. Ii. Isolated Disk Test

Kim

Agertz

Teyssier

et al. 2016

ApJ

124

142

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Using an isolated Milky Way-mass galaxy simulation, we compare results from 9 state-of-the-art gravitohydrodynamics codes widely used in the numerical community. We utilize the infrastructure we have built for the AGORA High-resolution Galaxy Simulations Comparison Project. This includes the common disk initial conditions, common physics models (e.g., radiative cooling and UV background by the standardized package GRACKLE) and common analysis toolkit yt, all of which are publicly available. Subgrid physics models such as Jeans pressure floor, star formation, supernova feedback energy, and metal production are carefully constrained across code platforms. With numerical accuracy that resolves the disk scale height, we find that the codes overall agree well with one another in many dimensions including: gas and stellar surface densities, rotation curves, velocity dispersions, density and temperature distribution functions, disk vertical heights, stellar clumps, star formation rates, and Kennicutt-Schmidt relations. Quantities such as velocity dispersions are very robust (agreement within a few tens of percent at all radii) while measures like newly-2 J. KIM ET AL. FOR THE AGORA COLLABORATION formed stellar clump mass functions show more significant variation (difference by up to a factor of ∼3). Systematic differences exist, for example, between mesh-based and particle-based codes in the low density region, and between more diffusive and less diffusive schemes in the high density tail of the density distribution. Yet intrinsic code differences are generally small compared to the variations in numerical implementations of the common subgrid physics such as supernova feedback. Our experiment reassures that, if adequately designed in accordance with our proposed common parameters, results of a modern high-resolution galaxy formation simulation are more sensitive to input physics than to intrinsic differences in numerical schemes.

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Section: Initial Conditionmentioning

confidence: 99%

The Agora High-Resolution Galaxy Simulations Comparison Project. Ii. Isolated Disk Test

Kim

Agertz

Teyssier

et al. 2016

ApJ

124

142

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“…where the angle brackets á ñ denote the average over the azimuthal direction (Satoh 1980;Yurin & Springel 2014). 5 Our standard model S1 has k=0.65.…”

Section: Galaxy Modelsmentioning

confidence: 99%

Origin of Non-axisymmetric Features of Virgo Cluster Early-type Dwarf Galaxies. I. Bar Formation and Recurrent Buckling

Kwak

Kim

Rey

et al. 2017

ApJ

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A fraction of early-type dwarf galaxies in the Virgo cluster have a disk component and even possess disk features such as bar, lens, and spiral arms. In this study, we construct 15 galaxy models that resemble VCC856, which is considered to be an infalling progenitor of disk dwarf galaxies, within observational error ranges, and use N-body simulations to study their long-term dynamical evolution in isolation as well as the formation of bar in them. We find that dwarf disk galaxies readily form bars unless they have an excessively concentrated halo or a hot disk. This suggests that infalling dwarf disk galaxies are intrinsically unstable to bar formation, even without any external perturbation, accounting for a population of barred dwarf galaxies in the outskirts of the Virgo cluster. The bars form earlier and stronger in galaxies with a lower fraction of counter-streaming motions, lower halo concentration, lower velocity anisotropy, and thinner disk. Similarly to normal disk galaxies, dwarf disk galaxies also undergo recurrent buckling instabilities. The first buckling instability tends to shorten the bar and to thicken the disk, and drives a dynamical transition in the bar pattern speed as well as mass inflow rate. In nine models, the bars regrow after the mild first buckling instability due to the efficient transfer of disk angular momentum to the halo, and are subject to recurrent buckling instabilities to turn into X-shaped bulges.

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“…Cappellari 2008), which find solutions of the Jeans equations. Clearly there will be existing methods which do not fit neatly in to this categorisation: for example, two particle based methods not based on Syer & Tremaine (1996) are Yurin & Springel (2014) and Rodionov, Athanassoula, & Sotnikova (2009). Each method has its own strengths and can be applied under different conditions.…”

Section: Introductionmentioning

confidence: 99%

Assessing the Jeans Anisotropic Multi-Gaussian Expansion method with the Illustris simulation

Mao

et al. 2015

Mon. Not. R. Astron. Soc.

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We assess the effectiveness of the Jeans-Anisotropic-MGE (JAM) technique with a state-of-the-art cosmological hydrodynamic simulation, the Illustris project. We perform JAM modelling on 1413 simulated galaxies with stellar mass M * > 10 10 M , and construct an axisymmetric dynamical model for each galaxy. Combined with a Markov Chain Monte Carlo (MCMC) simulation, we recover the projected root-mean-square velocity (V rms ) field of the stellar component, and investigate constraints on the stellar mass-to-light ratio, M * /L, and the fraction of dark matter f DM within 2.5 effective radii (R e ). We find that the enclosed total mass within 2.5 R e is well constrained to within 10%. However, there is a degeneracy between the dark matter and stellar components with correspondingly larger individual errors. The 1σ scatter in the recovered M * /L is 30 − 40% of the true value. The accuracy of the recovery of M * /L depends on the triaxial shape of a galaxy. There is no significant bias for oblate galaxies, while for prolate galaxies the JAM-recovered stellar mass is on average 18% higher than the input values. We also find that higher image resolutions alleviate the dark matter and stellar mass degeneracy and yield systematically better parameter recovery.

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An iterative method for the construction of N-body galaxy models in collisionless equilibrium

Cited by 106 publications

References 35 publications

The Agora High-Resolution Galaxy Simulations Comparison Project. Ii. Isolated Disk Test

The Agora High-Resolution Galaxy Simulations Comparison Project. Ii. Isolated Disk Test

Origin of Non-axisymmetric Features of Virgo Cluster Early-type Dwarf Galaxies. I. Bar Formation and Recurrent Buckling

Assessing the Jeans Anisotropic Multi-Gaussian Expansion method with the Illustris simulation

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