Concentration, spin and shape of dark matter haloes: Scatter and the dependence on mass and environment

By A. Macciò, A. Dutton, F. V. D. Bosch, B. Moore, Doug PotterJoachim Stadel. 2006

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We use a series of cosmological N-body simulations for a flat A cold dark matter (ACDM) cosmology to investigate the structural properties of dark matter haloes, at redshift zero, in the mass range 3 x 10 9 h -1 ≤ M vir ≤ 3 x 10 13 h -1 M ⊙ . These properties include the concentration parameter, c, the spin parameter, λ, and the mean axis ratio, q. For the concentration-mass relation we find c oc M -0.11 vir agreement with the model proposed by Bullock et al., but inconsistent with the alternative model of Eke et al. The normalization of the concentration-mass relation, however, is 15 per cent lower than suggested by Bullock et al. The results for X and q are in good agreement with previous studies, when extrapolated to the lower halo masses probed here, while c and λ are anticorrelated, in that high-spin haloes have, on average, lower concentrations. In an attempt to remove unrelaxed haloes from the sample, we compute for each halo the offset parameter, x off , defined as the distance between the most bound particle and the centre of mass, in units of the virial radius. Removing haloes with large x off increases the mean concentration by ∼ 10 per cent, lowers the mean spin parameter by ∼ 15 per cent, and removes the most prolate haloes. In addition, it largely removes the anticorrelation between c and λ, though not entirely. We also investigate the relation between halo properties and their large-scale environment density. For low-mass haloes we find that more concentrated haloes live in denser environments than their less concentrated counterparts of the same mass, consistent with recent correlation function analyses. Note, however, that the trend is weak compared to the scatter. For the halo spin parameters we find no environment dependence, while there is a weak indication that the most spherical haloes reside in slightly denser environments. Finally, using a simple model for disc galaxy formation we show that haloes that host low surface brightness galaxies are expected to be hosted by a biased subset of haloes. Not only do these haloes have spin parameters that are larger than average, they also have concentration parameters that are ∼15 per cent lower than the average at a given halo mass. We discuss the implications of all these findings for the claimed disagreement between halo concentrations inferred from low surface brightness rotation curves, and those expected for a ACDM cosmology.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/459bfcfd62dc54426a9afa7499f3a680d49c5b24

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Citations in the corpus

CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847 (2013, background): “Our result lies at the high concentration end of the allowed theoretical range, a region occupied by more dynamically relaxed halos in numerical simulations (e.g. Macciò et al. 2007; De Boni et al. 2013; Bhattacharya et al. 2013).”
Quantifying the heart of darkness with GHALO – a multibillion particle simulation of a galactic halo (2008, background): “A larger sample of haloes, such as Bullock et al. (2001) and Macciò et al. (2007), would be required to determine if this functional form provides a universal fit.”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, background): “We note that this is not what is usually done (e.g., Macciò et al. 2007; Gao et al. 2008; Dutton & Macciò 2014).”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, background): “…parameters for dark matter halos as a function of their mass has been studied by several authors (Barnes & Efstathiou 1987; Warren et al. 1992; Cole & Lacey 1996; Lemson & Kauffmann 1999; Bullock et al. 2001a; Bailin & Steinmetz 2005; Macciò et al. 2007; Bett et al. 2007; Macciò et al. 2008).”
Cores in warm dark matter haloes: a Catch 22 problem (2012, background): “Secondly, the central densities of CDM haloes in simulations show a cuspy behavior (Moore 1994; Flores & Primack 1994; Diemand et al. 2005; Macciò et al. 2007; Springel et al. 2008), whereas the density profiles inferred from galaxy rotation curves point to a core like structure (e.g. de Blok et…”
Are Brightest Halo Galaxies Central Galaxies (2010, methodology): “We model the halo concentrations using the c(M) relation of Macciò et al. (2007).”
GHASP: an Hα kinematic survey of spiral and irregular galaxies – V. Dark matter distribution in 36 nearby spiral galaxies (2007, background): “The problem is that internal dynamics and interaction between the dark halo and the luminous disk (e.g. adiabatic contraction: Dutton et al. 2005) and interaction with the environment (Maccio et al. 2007) may have altered the shape of the halo density profile.”
Radial migration in disc galaxies — I. Transient spiral structure and dynamics (2011, methodology): “The gas is also given a spin consistent with values obtained from collisionless co mological simulations (Bullock et al. 2001; Macciò et al. 2007), i.e. λ = (J/G) √ |E|/M5 = 0.039, whereJ is the total angular momentum,E is the total energy of the system andM is the mass.”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, background): “…(e.g., Warren et al. 1992; Jing & Suto 2002; Bailin & Steinmetz 2005; Kasun & Evrard 2005; Allgood et al. 2006; Shaw et al. 2006; Bett et al. 2007; Macciò et al. 2007, 2008) can bias a spherically-symmetric model fit of the reduced tangential shear profile and lead to errors of≈±30− 50% in the…”
Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations (2016, result): “…we analyze all dark matter halos and subhalos found by Rockstar, and do not just focus on those that satisfy some criteria for being “relaxed” or otherwise “good,” in contrast to some earlier studies of dark matter halo properties (e.g., Bett et al. 2007; Macciò et al. 2007; Ludlow et al. 2014).”
Cuspy No More: How Outflows Affect the Central Dark Matter and Baryon Distribution in Lambda CDM Galaxies (2012, methodology): “As most halos were re–run including only the DM component we also verified that the central DM profiles in the absence of baryons were as cuspy as those in the literature (Reed et al. 2005; Macciò et al. 2007, e.g.).”
Galaxy Groups in the SDSS DR4. I. The Catalog and Basic Properties (2007, methodology): “(6) The latter is a fitting function that accurately captures the halo mass dependence of the one-dimensional velocity dispersion as given by equation (14) in van den Bosch et al. (2004), using the halo concentrations of Maccio et al. (2007).”
The shape of dark matter haloes in the Aquarius simulations: evolution and memory (2011, background): “…have been found so far in simulations (e.g. Avila-Reese et al. 2005; Faltenbacher et al. 2005; Patiri et al. 2006; Basilakos et al. 2006; Macciò et al. 2007; Hahn et al. 2007) and observations (e.g. Pimbblet 2005; God lowski & Flin 2010; Niederste-Ostholt et al. 2010; Paz et al. 2011),…”
Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, background): “…in ΛCDM cosmology, an intrinsic, irreducible scatter is expected on the concentration of DM halos of the same mass (Jing 2000; Bullock et al. 2001; Macciò et al. 2007; Neto et al. 2007; Macciò et al. 2008; Dutton & Macciò 2014), which mainly reflects their slightly different formation epochs…”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, background): “The concentration is correlated with the formation c© 2011 RAS, MNRAS 000, 1–27 history of the halo (Wechsler et al. 2002), with earlier forming haloes having higher concentrations.”
Galaxy clustering and galaxy-galaxy lensing: a promising union to constrain cosmological parameters (2008, methodology): “9 shows (R) obtained for three of these models: the solid lines (labelled MAC) corresponds to our fiducial model for which we have used the cdm(M) relation of Macciò et al. (2007).”
Ultradiffuse galaxies: the high-spin tail of the abundant dwarf galaxy population (2016, background): “Under the assumption that the spin distribution is not strongly dependent on environment (e.g., Macciò et al. 2007; Kim et al. 2015) and that these extended disks are capable of forming stars in a similar way when in isolation, our model suggests that an abundant tail of extended galaxies should…”