The correlation structure of dark matter halo properties

Jeeson-Daniel, Akila; Vecchia, Claudio Dalla; Haas, M.; Schaye, Joop

doi:10.1111/j.1745-3933.2011.01081.x

Cited by 52 publications

(73 citation statements)

References 29 publications

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“…Our results for the concentration parameter are in contrast with those of Jeeson-Daniel et al (2011), who found from a Principal Component Analysis (PCA) of N -body haloes that the DM concentration can be even more fundamental than the halo mass. The lack of correlation between the infall subhalo abundance and the concentration indicates that the concentration might not be as fundamental as Jeeson-Daniel et al (2011) concluded, and reflects the lack of a physical connection between the concentration and infall abundance, with the concentration becoming relevant only after infall. Yet, a correlation at infall might be detected because of some degree of correlation between pairs of host halo properties themselves, as has been observed between halo formation time and concentration and between halo formation time and halo shape 4 .…”

Section: Origin Of the Halo-to-halo Variationcontrasting

confidence: 56%

“…On the other hand, at fixed host mass, Gao et al (2011) have found in MS-II that DM haloes with higher concentrations and earlier formation times contain fewer subhaloes. The mass fraction in substructure, related to the subhalo abundance, has also been found to depend on the halo shape and spin (Wang et al 2011); the impact of environment has been much more controversial, with some studies finding environmental dependence of the subhalo abundance (Fakhouri & Ma 2010;Croft et al 2012;Wang et al 2011), and with others finding no such evidence Jeeson-Daniel et al 2011).…”

Section: Physical Origin Of Baryonic Effects and Scattermentioning

confidence: 99%

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Subhalo demographics in the Illustris simulation: effects of baryons and halo-to-halo variation

Chua

Pillepich

Rodríguez-Gómez

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We study the abundance of subhaloes in the hydrodynamical cosmological simulation Illustris, which includes both baryons and dark matter in a ΛCDM volume 106.5 Mpc a side. We compare Illustris to its dark matter-only (DMO) analog, Illustris-Dark, and quantify the effects of baryonic processes on the demographics of subhaloes in the host mass range 10 11 to 3 × 10 14 M . We focus on both the evolved (z = 0) subhalo cumulative mass functions (SHMF) and the statistics of subhaloes ever accreted, i.e. infall subhalo mass function. We quantify the variance in subhalo abundance at fixed host mass and investigate the physical reasons responsible for such scatter. We find that in Illustris, baryonic physics impacts both the infall and z = 0 subhalo abundance by tilting the DMO function and suppressing the abundance of low-mass subhaloes. The breaking of self-similarity in the subhalo abundance at z = 0 is enhanced by the inclusion of baryonic physics. The non-monotonic alteration of the evolved subhalo abundances can be explained by the modification of the concentration-mass relation of Illustris hosts compared to Illustris-Dark. Interestingly, the baryonic implementation in Illustris does not lead to an increase in the halo-to-halo variation compared to Illustris-Dark. In both cases, the fractional intrinsic scatter today is larger for Milky Way-like haloes than for cluster-sized objects. For Milky Way-like haloes, it increases from about eight per cent at infall to about 25 per cent at the current epoch. In both runs, haloes of fixed mass formed later host more subhaloes than early formers.

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Section: Origin Of the Halo-to-halo Variationcontrasting

confidence: 56%

Section: Physical Origin Of Baryonic Effects and Scattermentioning

confidence: 99%

Subhalo demographics in the Illustris simulation: effects of baryons and halo-to-halo variation

Chua

Pillepich

Rodríguez-Gómez

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…However, five principal components are needed to explain more than 90% of the variance of the parametres, thus clusters with their environment are complicated objects whose properties cannot be explained with a small number of parametres as found also for the dark matter haloes by Jeeson-Daniel et al (2011). The locations of clusters in the PC1-PC2 plane shows that unimodal clusters in superclusters are located at upper lefthand part of the plot and have larger PC2 and smaller (larger negative) PC1 values (for example, clusters 608, 13408, 25078, and 28508).…”

Section: The Large-scale Environment Of Clustersmentioning

confidence: 99%

Multimodality of Rich Clusters From the SDSS Dr8 Within the Supercluster-Void Network

Einasto

2015

The Thirteenth Marcel Grossmann Meeting

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Context. The study of the properties of galaxy clusters and their environment gives us information about the formation and evolution of galaxies, groups and clusters, and larger structures -superclusters of galaxies and the whole cosmic web. Aims. We study the relations between the multimodality of galaxy clusters drawn from the SDSS DR8 and the environment where they reside. As cluster environment we consider the global luminosity density field, supercluster membership, and supercluster morphology. Methods. We use 3D normal mixture modelling, the Dressler-Shectman test, and the peculiar velocity of cluster main galaxies as signatures of multimodality of clusters. We calculate the luminosity density field to study the environmental densities around clusters, and to find superclusters where clusters reside. We determine the morphology of superclusters with the Minkowski functionals and compare the properties of clusters in superclusters of different morphology. We apply principal component analysis to study the relations between the multimodality parametres of clusters and their environment simultaneously. Results. Multimodal clusters reside in higher density environment than unimodal clusters. Clusters in superclusters have higher probability to have substructure than isolated clusters. The superclusters can be divided into two main morphological types, spiders and filaments. Clusters in superclusters of spider morphology have higher probabilities to have substructure and larger peculiar velocities of their main galaxies than clusters in superclusters of filament morphology. The most luminous clusters are located in the high-density cores of rich superclusters. Five of seven most luminous clusters, and five of seven most multimodal clusters reside in spider-type superclusters; four of seven most unimodal clusters reside in filament-type superclusters. Conclusions. Our study shows the importance of the role of superclusters as high density environment which affects the properties of galaxy systems in them.

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“…They found that halos in higher tidal field environments and in higher density environments have higher spins, with the trends stronger for higher mass halos. Skibba & Macciò (2011) and Jeeson-Daniel et al (2011) used principal component analyses to study the correlations of many halo properties including environment. Skibba & Macciò (2011) used the overdensity in spheres of 2, 4 and 8h −1 Mpc to measure the environmental density, and found that at fixed halo mass the environmental density does not significantly determine any of a halo's properties.…”

Section: Introductionmentioning

confidence: 99%

Properties of dark matter haloes as a function of local environment density

Lee

Primack

Behroozi

et al. 2016

Mon. Not. R. Astron. Soc.

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We study how properties of discrete dark matter halos depend on halo environment, characterized by the mass density around the halos on scales from 0.5 to 16 h −1 Mpc. We find that low mass halos (those less massive than the characteristic mass M C of halos collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations, and rounder shapes than halos in median density environments. Halos in median and low-density environments have similar accretion rates and concentrations, but halos in low density environments have lower spins and are more elongated. Halos of a given mass in high-density regions accrete material earlier than halos of the same mass in lower-density regions. All but the most massive halos in high-density regions are losing mass (i.e., being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low mass halos in high density regions at low redshifts z < 1, by preferentially removing higher angular momentum material from halos. Halos in low-density regions have lower than average spins because they lack nearby halos whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an Extreme Value Distribution, and that the density distribution becomes broader with cosmic time.

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The correlation structure of dark matter halo properties

Cited by 52 publications

References 29 publications

Subhalo demographics in the Illustris simulation: effects of baryons and halo-to-halo variation

Subhalo demographics in the Illustris simulation: effects of baryons and halo-to-halo variation

Multimodality of Rich Clusters From the SDSS Dr8 Within the Supercluster-Void Network

Properties of dark matter haloes as a function of local environment density

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