The evolution of dark matter halo properties in clusters, filaments, sheets and voids

By Oliver Hahn, C. Carollo, C. Porciani, A. Z. E. Zurich, HU Jerusalem. 2007

252 citations recorded by the source corpus.

We use a series of high-resolution N-body simulations of the concordance cosmology to investigate the redshift evolution since z = 1 of the properties and alignment with the large-scale structure (LSS) of haloes in clusters, filaments, sheets and voids. We find that (i) once a rescal-ing of the halo mass with M * (z), the typical mass scale collapsing at redshift z, is performed, there is no further significant redshift dependence in the halo properties; (ii) the environment influences the halo shape and formation time at all investigated redshifts for haloes with masses M ≤ M * and (iii) there is a significant alignment of both spin and shape of haloes with filaments and sheets. In detail, at all redshifts up to z = 1: (a) haloes with masses below ∼ M * tend to be more oblate when located in clusters than in the other environments; this trend is reversed at higher masses: above about M * , haloes in clusters are typically more prolate than similar massive haloes in sheets, filaments and voids. (b) The haloes with M ≥ M * in filaments spin more rapidly than similar mass haloes in clusters; haloes in voids have the lowest median spin parameters. (c) Haloes with M ≤ M * tend to be younger in voids and older in clusters. (d) In sheets, halo spin vectors tend to lie preferentially within the sheet plane independent of halo mass; in filaments, instead, haloes with M ≤ M * tend to spin parallel to the filament and higher mass haloes perpendicular to it. For halo masses M ≥ M * , the major axis of haloes in filaments and sheets is strongly aligned with the host filament or the sheet plane, respectively. Such halo-LSS alignments may be of importance in weak lensing analyses of cosmic shear. A question that is opened by our study is why, in the 0 < z < 1 redshift regime that we have investigated, the mass scale for gravitational collapse, M * , sets roughly the threshold below which the LSS environment either begins to affect, or reverses, fundamental properties of dark matter haloes.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ef7672cedb65fe0dfc253022478f5640147231dc

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Tracing the cosmic web (2017, methodology): “…large class of approaches exploits the morphological and (local) geometric information included in the Hessian of the density, tidal or velocity shear fields (e.g. Aragón-Calvo et al. 2007a; Hahn et al. 2007a; Forero-Romero et al. 2009; Bond et al. 2010a; Libeskind et al. 2012; Cautun et al. 2013).”
Dancing in the dark: galactic properties trace spin swings along the cosmic web (2014, methodology): “More recently, a consensus emerged when several works (Aubert, Pichon & Colombi 2004; Bailin & Steinmetz 2005; Aragón-Calvo et al. 2007; Hahn et al. 2007b; Paz, Stasyszyn & Padilla 2008; Sousbie et al. 2008; Libeskind et al. 2012; Trowland, Lewis & Bland-Hawthorn 2013) reported that large-scale…”
The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, background): “…that galaxy spin alignment can be strongly influenced by large-scale filaments and sheets (e.g., Aubert et al. (2004); Bailin and Steinmetz (2005); Hahn et al. (2007); Aragón-Calvo et al. (2007); Paz et al. (2008); Sousbie et al. (2008)), which was predicted by Lee and Pen (2000); Sugerman et…”
Galaxy Alignments: Observations and Impact on Cosmology (2015, methodology): “Voids correspond to the emptiest parts of the sky (in terms of galaxy density): underdense regions with scales of & 10 Mpc; while knots correspond to massive galaxy groups and clusters (e.g., Hahn et al. 2007). Alignment measurements that take into account the different environments started in the l”
Connecting the cosmic web to the spin of dark haloes: implications for galaxy formation (2012, methodology): “For instance, using N-body simulations Hahn et al. (2007b), Sousbie et al. (2009) and Zhang et al. (2009) found that halo spins are preferentially oriented perpendicularly to the filaments whatever their mass, with Faltenbacher et al. (2002) measuring a random distribution of the spin in the plane…”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, background): “…neighbor and the filament connecting the halos (e.g., Splinter et al. 1997; Onuora & Thomas 2000; Faltenbacher et al. 2002; Hopkins et al. 2005; Bailin & Steinmetz 2005; Kasun & Evrard 2005; Basilakos et al. 2006; Aragón-Calvo et al. 2007; Lee & Evrard 2007; Hahn et al. 2007; Zhang et al. 2009).”
The shape of dark matter haloes in the Aquarius simulations: evolution and memory (2011, background): “…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), albeit with…”
THE SPIN AND ORIENTATION OF DARK MATTER HALOS WITHIN COSMIC FILAMENTS (2009, methodology): “These trends agree well with results obtained by Hahn et al. (2007b) and Aragón-Calvo et al. (2007b).”
Galaxy Alignments: An Overview (2015, background): “Other statistical measures with desirable properties can be derived from the shear correlation functions, for instance the aperture mass dispersion (Schneider et al. 1998), which to a good approximation separates the field of gravitational shears into a curl-free and a divergence-free part, called E”
Evolution of the cosmic web (2014, methodology): “They characterize the cosmic web based on the density field Hessian, the tidal and the velocity shear fields (AragónCalvo et al. 2007a,b; Hahn et al. 2007a,b; Forero-Romero et al. 2009; Wu, Batuski & Khalil 2009; Bond, Strauss & Cen 2010a; Bond et al. 2010b; Hoffman et al. 2012; Cautun et al.…”
NEXUS: Tracing the cosmic web connection (2012, methodology): “Hahn et al. (2007a) (referred to as HPCD) proposed the use of the tidal field eigenvalues for environment classifica- tion7.”
Multiscale phenomenology of the cosmic web (2010, background): “In the case of the alignment of halos with their embedding filaments, Aragón-Calvo et al. (2007a) and Hahn et al. (2007) found evidence for a mass and redshift dependence, which has been confirmed by the studies of Paz et al. (2008) and Zhang et al. (2009).”