Substructures in cold dark matter haloes

By G. Lucia, G. Kauffmann, Volker Springel, Simon D. M. White, B. Lanzoni, Felix Stoehr, G. Tormen, N. Y. Mpa, Garching, Heidelberg · Germany and 4 more. 2003

247 citations recorded by the source corpus.

We analyse the properties of substructures within dark matter haloes (subhaloes) using a set of high-resolution numerical simulations of the formation of structure in a ACDM universe. Our simulation set includes 11 high-resolution simulations of massive clusters as well as a region of mean density, allowing us to study the spatial and mass distribution of substructures down to a mass resolution limit of 10 9 h -1 M ○. . We also investigate how the properties of substructures vary as a function of the mass of the 'parent' halo in which they are located. We find that the substructure mass function depends at most weakly on the mass of the parent halo and is well described by a power law. The radial number density profiles of substructures are steeper in low mass haloes than in high-mass haloes. More massive substructures tend to avoid the centres of haloes and are preferentially located in the external regions of their parent haloes. We also study the mass accretion and merging histories of substructures, which we find to be largely independent of environment. We find that a significant fraction of the substructures residing in clusters at the present day were accreted at redshifts z < 1. This implies that a significant fraction of present-day 'passive' cluster galaxies were still outside the cluster progenitor and were more active at z ∼ 1.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/1b1019201e71acf7c3c1c848199070fe45076b61

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Citations in the corpus

Gravitational Lens Time Delays: A Statistical Assessment of Lens Model Dependences and Implications for the Global Hubble Constant (2006, methodology): “We distribute subhalos randomlywith an uniform spatial density in the projected two-dimensional plane in order to take account of the suggested antibias of the subhalo spatial distribution (De Lucia et al. 2004; Mao et al. 2004; Oguri & Lee 2004).”
Structure finding in cosmological simulations: the state of affairs (2013, background): “…Moore et al. 1999), concentration–mass relation (Bullock et al. 2001a; Wechsler et al. 2002), mass accretion histories (Wechsler et al. 2002; De Lucia et al. 2004; De Lucia & Blaizot 2007; Diemand et al. 2007; Behroozi, Wechsler & Conroy 2013c), shape distributions (Dubinski & Carlberg 1991;…”
The many manifestations of downsizing: hierarchical galaxy formation models confront observations (2009, methodology): “A possibly related trend is the increase with time of faint red-sequence galaxies in galaxy clusters (see e.g. De Lucia et al. 2004b, 2007; Gilbank et al. 2008), which may be due to a differential decline of the SSFR. DS in stellar mass: the high-mass end of the stellar mass function (MF) evolves…”
Statistics of Physical Properties of Dark Matter Clusters (2005, methodology): “…parallel algorithms, has enabled us to achieve the numerical resolution required to overcome the numerical problems (Ghigna et al. 1998a, 2000; Klypin et al. 1999; Moore et al. 1999; Okamoto & Habe 1999; Springel et al. 2001, 2005; Bode et al. 2001; Kravtsov et al. 2004a; De Lucia et al. 2004).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, background): “…al. 2005, normalized to match cosmological simulations as in Shaw et al. 2006), which brackets the range of a number of different estimates (e.g., Springel et al. 2001; Tormen et al. 2004; De Lucia et al. 2004; Gao et al. 2004; Nurmi et al. 2008), and demonstrate the uncertainty due to this choice.”
K-Band Properties of Galaxy Clusters and Groups: Luminosity Function, Radial Distribution, and Halo Occupation Number (2004, methodology): “More recently, a study of subhalo properties within a large cluster ensemble shows that the subhalos are less concentrated than the mass (De Lucia et al. 2004).”
Ahf: AMIGA'S HALO FINDER (2009, background): “It has been found before (e.g. Ghigna et al. 2000; Helmi et al. 2002; De Lucia et al. 2004; Gao et al. 2004; van den Bosch et al. 2005; Diemand et al. 2007; Giocoli et al. 2008; Springel et al. 2008) that the subhalo mass function can be described with a functional form Nsub(> M) ∝ M −α, with α =…”
MERGERS AND BULGE FORMATION IN ΛCDM: WHICH MERGERS MATTER? (2009, background): “Alternative subhalo mass functions from e.g. De Lucia et al. (2004); Gao et al. (2004); Nurmi et al. (2006) are consistent.”
The mass function and average mass-loss rate of dark matter subhaloes (2004, methodology): “These findings are in good agreement with those of Gao et al. (2004), based on numerical simulations that span three orders of magnitude in parent halo mass, and strongly argue against earlier claims for a universal subhalo mass function (e.g. Moore et al. 1998; De Lucia et al. 2004).”
Velocity and spatial biases in cold dark matter subhalo distributions (2004, background): “De Lucia et al. (2004) confirmed this recently for several CDM haloes, but at a resolution of less than 1 × 106 particles inside the virial radius.”
Subhaloes going Notts: the subhalo‐finder comparison project (2012, background): “…between5 per cent and 10 per cent of the material within simulated galactic sized haloes exists within bound substructures (e.g. Gao et l. 2004; De Lucia et al. 2004; Contini et al. 2011) and a substantial part of the host halo has formed from disrupted subhalo material (e.g. Gill et al. 2004;…”
Linking halo mass to galaxy luminosity (2004, background): “Its results are similar to those obtained by the simulations of De Lucia et al. (2004), who find a power-law fit to the subhalo mass function with a slope close to −2 (that is, in terms of equation (1), α = 2).”
DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, background): “…and it makes no difference whether we adopt the fits from different authors (we have alsocompared the subhalo mass functions in Springel et al. 2001; Tormen et al. 2004; De Lucia et al. 2004; Gao et al. 2004; Zentner et al. 2005; Nurmi et al. 2006, and reach similar conclusions).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, background): “…al. 2005, normalized to match cosmological simulations as in Shaw et al. 2006), which bracket the range of a number of different estimates (e.g., Springel et al. 2001; Tormen et al. 2004; De Lucia et al. 2004; Gao et al. 2004; Nurmi et al. 2006) and demonstrate the uncertainty owing to this choice.”
The alignment between the distribution of satellites and the orientation of their central galaxy (2006, background): “…centrally concentrated than the dark matter, with a pronounced deficit of subhaloes near the center (Ghigna et al. 1998, 2000; Coĺin et al. 1999; Springel et al. 2001; De Lucia et al. 2004; Gao et al. 2004; Diemand, Moore & Stadel 2004; Mao et al. 2004; Nagai & Kravtsov 2005; Kang et al. 2005).”
The Sloan Lens ACS Survey. IV. The Mass Density Profile of Early-Type Galaxies out to 100 Effective Radii (2007, background): “…MA 02138, USA 6 Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Ave., Cambridge, MA 02139, USA abundant substructure (e.g. Moore et al. 1999; De Lucia et al. 2004; Gao et al. 2004; Taylor & Babul 2004).”