On the evolution of galaxy clustering and cosmological N-body simulations

Fall, S. Michael

doi:10.1093/mnras/185.2.165

Cited by 14 publications

(3 citation statements)

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“…Simulations are indispensable tools in the interpretation of astronomical observations of these objects (see for instance Borgani & Kravtsov 2011). Although early N -body simulations only modeled the gravitational evolution of collisionless effects of dark matter (White 1976;Fall 1978;Aarseth, Turner & Gott 1979), these were vital for interpreting galaxy surveys and unveiling the cosmic web of the large scale structure of the Universe. The focus of modern simulations (see e.g.…”

Section: Introductionmentioning

confidence: 99%

nIFTy galaxy cluster simulations – II. Radiative models

Sembolini

Elahi

Pearce

et al. 2016

Mon. Not. R. Astron. Soc.

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We have simulated the formation of a massive galaxy cluster (M crit 200 = 1.1×1015 h −1 M ) in a ΛCDM universe using 10 different codes (RAMSES, 2 incarnations of AREPO and 7 of GADGET), modeling hydrodynamics with full radiative subgrid physics. These codes include Smoothed-Particle Hydrodynamics (SPH), spanning traditional and advanced SPH schemes, adaptive mesh and moving mesh codes. Our goal is to study the consistency between simulated clusters modeled with different radiative physical implementations -such as cooling, star formation and AGN feedback. We compare images of the cluster at z = 0, global properties such as mass, and radial profiles of various dynamical and thermodynamical quantities. We find that, with respect to non-radiative simulations, dark matter is more centrally concentrated, the extent not simply depending on the presence/absence of AGN feedback. The scatter in global quantities is substantially higher than for non-radiative runs. Intriguingly, adding radiative physics seems to have washed away the marked code-based differences present in the entropy profile seen for non-radiative simulations in Sembolini et al. (2015): radiative physics + classic SPH can produce entropy cores. Furthermore, the inclusion/absence of AGN feedback is not the dividing line -as in the case of describing the stellar content-for whether a code produces an unrealistic temperature inversion and a falling central entropy profile. However, AGN feedback does strongly affect the overall stellar distribution, limiting the effect of overcooling and reducing sensibly the stellar fraction.

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Section: Introductionmentioning

confidence: 99%

nIFTy galaxy cluster simulations – II. Radiative models

Sembolini

Elahi

Pearce

et al. 2016

Mon. Not. R. Astron. Soc.

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“…In order to study the spatial correlation of galaxies, the first cosmological N-body simulations were performed in the 1970s using approximately 1000 particles (e.g., Miyoshi & Kihara 1975;Fall 1978;Aarseth et al 1979;Efstathiou 1979). Since then, the development of better simulation algorithms and improvements in the performance of computers allow us to use much larger numbers of particles and have drastically increased the resolution of cosmological simulations.…”

Section: Introductionmentioning

confidence: 99%

The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos

Ishiyama

Rieder

Makino

et al. 2013

ApJ

100

104

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We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048 3 particles. The mass of each particle is 1.28 × 10 5 M , which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ∼10 7 M . We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than −1 at the innermost radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ∼10 8 M . The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ∼10 11 M halos have.

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“…At almost the same time, smaller simulations of cosmological clustering were performed by Haggerty & Janin (1974). This work was followed by numerous studies of the evolution of the two-point correlation function, a measure of galaxy clustering (Miyoshi & Kihara 1975, Groth & Peebles 1976, Fall 1978, Efstathiou 1979. Early work on galaxy formation was reviewed by Gott (1977).…”

Section: Introductionmentioning

confidence: 99%

Simulations of Structure Formation in the Universe

Bertschinger

1998

Annu. Rev. Astron. Astrophys.

276

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Cosmic structure has formed as a result of gravitational amplification of primordial density fluctuations together with the action of other physical processes (adiabatic gas dynamics, radiative cooling, photoionization and recombination, radiative transfer). These complex nonlinear processes, acting over a wide range of length scales (from kiloparsecs to tens of megaparsecs), make this a difficult problem for computation. During the last two decades, significant progress has been made in developing numerical methods and statistical tools for analyzing simulations and data. Combined with observational advances, numerical simulations have led to the demise of several formerly popular models and to an improved understanding of galaxy clusters, quasistellar object (QSO) absorption line systems, and other phenomena. This review summarizes these advances.

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On the evolution of galaxy clustering and cosmological N-body simulations

Cited by 14 publications

References 0 publications

nIFTy galaxy cluster simulations – II. Radiative models

nIFTy galaxy cluster simulations – II. Radiative models

The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos

Simulations of Structure Formation in the Universe

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