Convergence and scatter of cluster density profiles

By J. Diemand, B. Moore, Joachim Stadel. 2004

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We present new results from a series of ACDM simulations of cluster mass haloes resolved with high force and mass resolution. These results are compared with recently published simulations from groups using various codes including PKDGRAV, ART, TPM, GRAPE and GADGET. Careful resolution tests show that with 25 million particles within the high-resolution region we can resolve to about 0.3 per cent of the virial radius and that convergence in radius is proportional to the mean interparticle separation. The density profiles of 26 high-resolution clusters obtained with the different codes and from different initial conditions agree very well. The average logarithmic slope at one per cent of the virial radius is y = 1.26 with a scatter of ±0.17. Over the entire resolved regions the density profiles are well fitted by a smooth function that asymptotes to a central cusp p oc r -γ , where we find y = 1.16 ± 0.14 from the mean of the fits to our six highest-resolution clusters.

Subfields: Atmospheric Science, Nuclear and High Energy Physics, Physical and Theoretical Chemistry

View Paper: https://www.semanticscholar.org/paper/2d60d77484b2afc9eec51705b8790fa4032e90be

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Citations in the corpus

Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology (2007, methodology): “Diemand et al. (2004a) pointed out that subhalo populations in clusters are very close to stationary solutions of the Jeans equation.”
Quantifying the heart of darkness with GHALO – a multibillion particle simulation of a galactic halo (2008, methodology): “The first CDM halo simulated with enough resolution to resolve substructure used 106 particles (Moore et al. 1998), resolving the density profile to about one percent of the virial radius (Ghigna et al. 1998; Moore et al. 1999; Power et al. 2003; Navarro et al. 2004; Diemand et al. 2004).”
On the efficiency and reliability of cluster mass estimates based on member galaxies (2006, background): “As far as the velocity distribution ofsubhaloesis concerned, most studies have found it to be wider than that of DM particles (Colı́n et al. 2000; Diemand et al. 2004), at leastnear the cluster centre (Ghigna et al. 2000; Reed et al. 2005).”
Dark Matter Substructure and Gamma-Ray Annihilation in the Milky Way Halo (2006, background): “…decreases and approaches the other two estimates, presumably because it too starts to be affected by the finite resolution: with this low number of particles, halo density profiles are artificially flattened by numerical effects out to a radius of about N 1/3 rt ¼ 0:07rt (Diemand et al. 2004a).”
The dark matter haloes of massive, relaxed galaxy clusters observed with Chandra (2006, methodology): “Finally, we reiterate that the simulations used to predict the mass-concentration relation and central dark matter slopes (e.g., Navarro et al. 1995, 1997; Diemand et al. 2004; Shaw et al. 2006) are CDM only.”
The impact of dark matter cusps and cores on the satellite galaxy population around spiral galaxies (2010, result): “For example, Diemand et al. (2004, 2005) claims a central slope of γ = 1.2, whereas other authors argued in favour of steeper, γ = 1.5, cusps (Moore et al. 1999b; Gighna et al. 2000).”
The structural and scaling properties of nearby galaxy clusters. I. The universal mass profile (2005, background): “…still a matter of debate, recent high resolution simulations predict that dark matter profiles are cusped (Navarro et al. 1997; Moore et al. 1999; Diemand et al. 2004; Navarro et al. 2004) and that the concentration of the Dark Matter varies only slightly with system mass (e.g. Dolag et al.…”
Modified Newtonian dynamics in the Milky Way (2005, background): “The halo introduced by BEG is not cuspy like the haloes predicted by CDM cosmology (Diemand et al. 2004, and references therein).”
Dynamical insight into dark matter haloes (2005, background): “…1057–1068 Downloaded from https://academic.oup.com/mnras/article-abstract/363/4/1057/1043779 by guest on 29 July 2018 the resolved radial range, as the latter has been shown to provide a very accurate description of many simulated dark matter haloes (e.g. Diemand et al. 2004b; Navarro et al. 2004).”
The Phoenix Project: the dark side of rich galaxy clusters (2012, background): “…the highest-resolution galaxy cluster simulations published to date have at most of order af w million particles within the virial radius (e.g. Jing & Suto2000; Springel et al. 2001a; Diemand et al. 2004a; Reed et al. 2005), roughly one thousand times fewer than the best resolved Aquar- ius halo.”
The redshift dependence of the structure of massive Λ cold dark matter haloes (2007, background): “…rather limited, derived largely from small numbers of individual realizations or from extrapolation of models calibrated on different mass scales (NFW; Moore et al. 1998; Ghigna et al. 2000; Klypin et al. 2001; Navarro et al. 2004; Tasitsiomi et al. 2004; Diemand et al. 2004; Reed et al. 2005).”
The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST (2008, background): “Central Flux Corrections The host halo center is another area where our simulation must be corrected to account for the artificially low density caused by the finite numerical resolution (Diemand et al. 2004b).”
Small scale problems of the $\Lambda$CDM model: a short review (2016, background): “Already then, convergence tests performed by [229] showed that N-body simulations correctly determine the CDM density profiles.”
The diversity and similarity of simulated cold dark matter haloes (2008, background): “• These results convincingly rule out recent claims that typical ΛCDM halos may have asymptotic central cusps as steep as r−1.2 (Diemand et al., 2004, 2005, 2008).”
Non-linear evolution of cosmological structures in warm dark matter models (2011, background): “Over the years, extensive numerical work has shown that, for the case of the CDM model, the density profiles of dark matter haloes are reasonably well characterized by the NFW profile (Navarro et al. 1997; Moore et al. 1999; Diemand et al. 2004; Springel et al. 2008; Stadel et al. 2009).”