The structure of voids

By Stefan Gottloeber, E. Lokas, Anatoly Klypin, Yehuda Hoffman Aip, C. Center, Nmsu, R. I. O. Physics. 2003

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Using high resolution N-body simulations we address the problem of emptiness of giant � 20h −1 Mpc–diameter voids found in the distribution of bright galaxies. Are the voids filled by dwarf galaxies? Do cosmological models predict too many small dark matter haloes inside the voids? Can the problems of cosmological models on small scales be addressed by studying the abundance of dwarf galaxies inside voids? We find that voids in the distribution of 10 12 h −1 M⊙ haloes (expected galactic magnitudes � M∗) are almost the same as the voids in 10 11 h −1 M⊙ haloes. Yet, much smaller haloes with masses 10 9 h −1 M⊙ and circular velocities vcirc � 20 km/s readily fill the voids: there should be almost 1000 of these haloes in a 20h −1 Mpc–diameter void. A typical void of diameter 20h −1 Mpc contains about 50 haloes with vcirc > 50 km/s. The haloes are arranged in a pattern, which looks like a miniature Universe: it has the same structural elements as the large-scale structure of the galactic distribution of the Universe. There are filaments and voids; larger haloes are at the intersections of filaments. The only difference is that all masses are four orders of magnitude smaller. There is severe (anti)bias in the distribution of haloes, which depends on halo mass and on the distance from the centre of the void. Large haloes are more antibiased and have a tendency to form close to void boundaries. The mass function of haloes in voids is different from the “normal” mass function. It is much steeper for high masses resulting in very few M33-type galaxies (vcirc � 100 km/s). We present an analytical approximation for the mass function of haloes in voids.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9a162a4e2e6ff89fe5df6cfadd41a0af89372868

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Citations in the corpus

A cosmic watershed: the WVF void detection technique (2007, background): “…activity in this direction (Benson et al. 1996; Szomoru et al. 1998; Grogin & Geller 1999; Friedmann & Piran 2001; Hoyle & Vogeley 2002; Mathis & White 2002; Gottl¨ober et al. 2003; Rojas et al. 2005; Ceccarelli et al. 2006; Furlanetto & Piran 2006; Patiri et al. 2006b; Hoeft et al. 2007).”
A marked correlation function analysis of halo formation times in the Millennium Simulation (2005, background): “…easy to interpret usingzf as the mark, since it is well established that the halo mass functiodepends on local density: in high-density regions, it becomessk wed towards more massive haloes (Frenk et al. 1988; Cole & Kaiser 1989; Lemson & Kauffmann 1999; Gottlöber et al. 2003; Mo et al. 2004).”
Cosmic Voids in Sloan Digital Sky Survey Data Release 7 (2011, methodology): “Simulations of the Cold Dark Matter model for structure formation indicate that the interiors of voids should include dark matter filaments and many low mass halos (Mathis & White 2002; Benson et al. 2003; Gottlöber et al. 2003).”
Unusually Large Fluctuations in the Statistics of Galaxy Formation at High Redshift (2003, methodology): “On the other hand, simulations show that voids actually place a larger fraction of their dark matter content in dwarf halos of mass below 1010M⊙ (Gottlöber et al. 2003).”
Dwarf galaxies in voids: suppressing star formation with photoheating (2005, methodology): “More than one thousand galaxies passed their selection criterion (which differs slightly from the criterion used in the numerical simulations of Gottlöber et al. (2003) and in this paper).”
A hierarchy of voids: much ado about nothing (2003, background): “For similar reasons, the clouds associated with the more massive halos should be more massive on average (this is also discussed more fully by Mo & White 1996; Sheth & Tormen 2002 and Gottlöber et al. 2003).”
Multiscale phenomenology of the cosmic web (2010, background): “Ultrahigh resolution N-body simulations show that even in the most underdense regions one can find systems of tenuous filaments extending along the whole physical extent of the voids (van de Weygaert & van Kampen 1993; Gottlöber et al. 2003; Platen et al. 2007).”
Evolution of the cosmic web (2014, background): “…void size, shape and inner structure (Martel & Wasserman 1990; van de Weygaert 1991a; van de Weygaert & van Kampen 1993; Mathis & White 2002; Gottlöber et al. 2003; Colberg et al. 2005b; Platen, van de Weygaert & Jones 2008; van de Weygaert & Platen 2011; Aragon-Calvo & Szalay 2013;…”
A Dynamical Classification of the Cosmic Web (2008, unknown): “41 35 v1 [ as tr oph ] 2 4 Se 2005; Gottlöber et al. 2003; Arbabi-Bidgoli & Müller 2002; Neyrinck 2008; Platen et al. 2007; Plionis & Basilakos 2002; Shandarin et al. 2006).”
Linking halo mass to galaxy luminosity (2004, methodology): “In order to do this, we follow the method outlined in Gottlöber et al. (2003).”
The Aspen-Amsterdam void finder comparison project (2008, background): “…et al. 1993 or Van de Weygaert & Van Kampen 1993, and the more recent Arbabi-Bidgoli & Müller 2002, Mathis & White 2002, Benson et al. 2003, Gottlöber et al. 2003, Goldberg & Vogeley 2004, Sheth & Van de Weygaert 2004, Bolejko et al. 2005, Colberg et al. 2005, Padilla et al. 2005,…”