Properties of dark matter haloes in clusters, filaments, sheets and voids

By Oliver Hahn, C. Porciani, M. Carollo, A. Dekel. 2006

401 citations recorded by the source corpus.

Using a series of high-resolution N-body simulations of the concordance cosmology we investigate how the formation histories, shapes and angular momenta of dark-matter haloes depend on environment. We first present a classification scheme that allows to distinguish between haloes in clusters, filaments, sheets and voids in the large-scale distribution of matter. This method (which goes beyond a simple measure of the local density) is based on a local-stability criterion for the orbits of test particles and closely relates to the Zel’dovich approximation. Applying this scheme to our simulations we then find that: i) Mass assembly histories and formation redshifts strongly depend on environment for haloes of mass M < M� (haloes of a given mass tend to be older in ′

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Detecting filamentary pattern in the cosmic web: a catalogue of filaments for the SDSS (2013, methodology): “Among them are the algorithms based on the gravitational tidal tensor – the Hessian of the gravitational potential (Hahn et al. 2007; Lee & Lee 2008; Forero-Romero et al. 2009; Bond, Strauss & Cen 2010a,b; Wang et al. 2012), on the velocity field (Shandarin 2011; Hoffman et al. 2012; Wang et al.…”
The persistent cosmic web and its filamentary structure II: Illustrations (2010, background): “Quite a few such options have been presented recently (Stoica et al. 2005; Novikov, Colombi & Doré 2006; Hahn et al. 2007; Platen, van de Weygaert & Jones 2007; Stoica, Martı́nez & Saar 2007, 2010; Neyrinck 2008; Sousbie et al. 2008a,b; Forero-Romero et al. 2009; Sousbie, Colombi & Pichon 2009;…”
The Initial Conditions of the Universe from Constrained Simulations (2012, background): “The reconstructed density field is especially valueable as it permitsone to study the cosmic web and perform environmental studies (seee.g. Hahn et al. 2007; Forero-Romero et al. 2009; Jasche et al. 2010; Muñoz-Cuartas et al. 2011; Wang et al. 2012; Platen et al. 2011).”
Spin alignments within the cosmic web: a theory of constrained tidal torques near filaments (2015, background): “Both numerical (e.g. Aragón-Calvo et al. 2007; Hahn et al. 2007; Sousbie et al. 2008; Paz et al. 2008; Zhang et al. 2009; Codis et al. 2012; Libeskind et al. 2013; Aragón-Calvo 2013; Dubois et al. 2014), and observational evidence (e.g. Tempel et al. 2013) have recently supported this scenario.”
zobov: a parameter-free void-finding algorithm (2007, background): “Some other void finders (e.g. El-Ad & Piran 1997; Aikio & Mähönen 1998; Plionis & Basilakos 2002; Shandarin et al. 2006; Hahn et al. 2007; Aragón-Calvoet al. 2007; Platen, van de Weygaert & Jones 2007) also define voids with no, or only weak, rules about their shapes.”
Multi-scale initial conditions for cosmological simulations (2011, methodology): “…at which the circular velocity profile is maximal, the dimensionless spin parameter λ (Bullock et al. 2001), the three-dimensional velocity dispersion σ v as well as the minor-to-major axial ratio c/a, determined using the eigenvalues of the moment of inertia tensor (see e.g. Hahn et al. 2007).”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “…exhibit systematic differences between low and high density environments at fixed halo mass (Sheth & Tormen 2004; Gao et al. 2005; Wechsler et al. 2006; Harker et al. 2006; Zhu et al. 2006; Hahn et al. 2007; Jing et al. 2007; Li et al. 2008; Faltenbacher & White 2010; Croft et al. 2012).”
A kinematic classification of the cosmic web (2012, methodology): “Hence, the web classification of Hahn et al. (2007) and FR09 can be reformulated in terms of the (velocity) shear tensor.”
A Dynamical Classification of the Cosmic Web (2008, methodology): “The algorithm presented here is an extension and improvement of the one suggested by Hahn et al. (2007).”
Assembly bias in the clustering of dark matter haloes (2006, background): “(See also Hahn et al. (2007) for a slightly different approach to studying environmental effects on halo spin.)”
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 Multiscale Morphology Filter: Identifying and Extracting Spatial Patterns in the Galaxy Distribution (2007, neutral): “(Hahn et al. 2007) reach similar conclusions.”
A cosmic watershed: the WVF void detection technique (2007, background): “…of void identiﬁcation procedures (Kauffmann & Fairall 1991; El-Ad & Piran 1997; Aikio & M¨ah¨onen 1998; Arbabi-Bidgoli & M¨uller 2002; Hoyle & Vogeley 2002; Plionis & Basilakos 2002; Colberg et al. 2005; Patiri et al. 2006a; Shandarin et al. 2006; Hahn et al. 2007; Neyrinck, in preparation).”
Tracing the dark matter sheet in phase space (2011, result): “This is compatible with previous results on mass and volume fractions in the various parts of the cosmic web e.g. by Hahn et al. (2007) using a fixed scale, or by Aragón-Calvo et al. (2010) using adaptive filtering.”
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 persistent cosmic web and its filamentary structure I: Theory and implementation (2010, background): “…identification of all types of astrophysically significant features of the large-scale galaxy distribution in the universe (see e.g. Novikov, Colombi & Doré 2006; Hahn et al. 2007; Sousbie et al. 2008a,b; Forero-Romero et al. 2009; Sousbie, Colombi & Pichon 2009; Aragón-Calvo et al. 2010b).”
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…”
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).”
The evolution of dark matter halo properties in clusters, filaments, sheets and voids (2007, background): “At the same time it has become clear that also other halo properties as concentration and spin correlate with local environment (Avila-Reese et al. 2005; Wechsler et al. 2006; Bett et al. 2007; Macciò et al. 2006; Wetzel et al. 2007; Hahn et al. 2007).”