The abundance and clustering of dark haloes in the standard ΛCDM cosmogony

By H. Mo, Simon D. M. White. 2002

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Much evidence suggests that we live in a flat cold dark matter universe with a cosmological constant. Accurate analytic formulae are now available for many properties of the dark halo population in such a Universe. Assuming current ‘concordance’ values for the cosmological parameters, we plot halo abundance against redshift as a function of halo mass, halo temperature, the fraction of cosmic matter in haloes, halo clustering strength, and the clustering strength of the z= 0 descendants of high-redshift haloes. These plots are useful for understanding how nonlinear structure grows in the model. They demonstrate a number of properties that may seem surprising, for example: 109 M⊙ haloes are as abundant at z= 20 as L* galaxies are today; 106 K haloes are equally abundant at z= 8 and at z= 0; 10 per cent of all matter is currently in haloes hotter than 1 keV, while more than half is in haloes too cool to trap photo-ionized gas; 1 per cent of all matter at z= 15 is in haloes hot enough to ionize hydrogen; haloes of given mass or temperature are more clustered at higher redshift; haloes with the abundance of present-day L* galaxies are equally clustered at all z 10 are more clustered at z= 0 than are L* galaxies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0cec0d0d4b63de7f03af434d258c1952a732c865

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Citations in the corpus

The luminosity function, halo masses and stellar masses of luminous Lyman-break galaxies at redshifts 5 < z < 6 (2008, background): “Based on the predictions of dark matter halo models (Sheth et al. 2001; Mo & White 2002), and assuming a one-to-one correspondance between galaxies and halos, we infer that our5.”
Two populations of metal-free stars in the early Universe (2006, methodology): “…effect of biasing, we use the well-known linear correlation function ξhh(M, R, z) between two haloes of mass M at a comoving distance R: ξhh(M, R, z) = b 2(M, z)ξmm(R) , (10) where b(M, z) is the linear bias of a halo of mass M , and ξmm(R) is the mass correlation function (e.g. Mo & White 2002).”
Constraining galaxy formation and cosmology with the conditional luminosity function of galaxies (2002, background): “…the brightest sample, and smaller for fainter samples), one can show that these two bias factors are related by beff(z) = 1 + [D(0)/D(z)](b− 1) , (35) (Mo & White 1996, 2002; Fry 1996) where D(z) is the linear growth rate at redshift z, related to the linear growth factor g(z) by D(z) =…”
Bimodal gas accretion in the Horizon–MareNostrum galaxy formation simulation (2008, methodology): “…critical mass for shock stability, Mshock, as log(Mstream) = 2 log(Mshock) − log(M∗) − log(3) , (13) where M∗ is the typical dark matter halo mass at a given redshift as computed using the formalisms of Lahav et al. (1991); Carroll et al. (1992); Mo & White (2002) and following Appendix 3 of DB06.”
Gravitational quenching in massive galaxies and clusters by clumpy accretion (2007, background): “This may be the case before the universe becomes reionized at z ∼ 9, by which most ∼ 107M⊙ haloes are already in place (Mo & White 2002, based on the PressSchechter formalism).”
Integral field spectroscopy with SINFONI of VVDS galaxies I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6 (2009, methodology): “We have estimated the total halo mass (Mhalo) using a spherical virialized collapse model (Peebles 1980; White & Frenk 1991; Mo & White 2002).”
Toy models for galaxy formation versus simulations (2013, background): “This is largely basic material, based for example on Lahav, Rees, Lilje, & Primack (1991); Carroll, Press, & Turner (1992) and Mo & White (2002); Birnboim & Dekel (2003); Dekel & Birnboim (2006), with the addition of accretion rates from Neistein, van den Bosch & Dekel (2006); Neistein & Dekel…”
The birth of a galaxy – III. Propelling reionization with the faintest galaxies (2014, background): “The comoving density of these haloes only varies by a factor of a few during the redshift range 7–15 (Mo & White 2002).”
Ongoing assembly of massive galaxies by major merging in large groups and clusters from the SDSS (2007, background): “Yet, a simple calculation shows that there is only a 10% chance for a line-of-sight projection of a distinct group with Mhalo ≥ 10 13M⊙ within 1 Mpc radius and±400 km s−1 depth (following the group-centric properties of the SAT-SAT mergers in Fig.”
Chemical Evolution in Hierarchical Models of Cosmic Structure. I. Constraints on the Early Stellar Initial Mass Function (2005, methodology): “The numerical results calculated from the EPS formalism also agree well with the halo number-density and mass distributions presented by Mo & White (2002) when their fiducial cosmological parameters are adopted.”
Bursting and quenching in massive galaxies without major mergers or AGNs (2007, unknown): “Following Mo & White (2002), in a flat universe D(z) = g(z) g(0) 1 (1 + z) , (A24) g(z) 5 2 ( −3/7m (z) + 3 2 )−1 , (A25) with a negligible error on the order of λ/70 in g(z).”
The history of star formation in a lcdm universe (2002, methodology): “Following Mo & White (2002), we assign a physical radius to a halo of mass M according to r200 = [ GM 100Ωm(z)H2(z) ]1/3 = 1 1 + z [ GM 100Ω0H20 ]1/3 , (1) and a corresponding circular velocity Vc = (GM/r200) 1/2.”
METALLICITY-DEPENDENT QUENCHING OF STAR FORMATION AT HIGH REDSHIFT IN SMALL GALAXIES (2011, methodology): “(9) Here M∗,PS(z) is the Press-Schechter mass at a given redshift, which we compute from the Sheth & Tormen (1999) ellipsoidal collapse model following the procedure outlined in Mo & White (2002).”
The Herschel Multi-tiered Extragalactic Survey: HerMES (2012, background): “Examination of each of those requirements requires survey comoving volumes of 106–107 Mpc3 or larger.”
A Population of Faint Extended Line Emitters and the Host Galaxies of Optically Thick QSO Absorption Systems (2007, background): “The space density inferred by our sample of objects corresponds to the cumulative space density of dark matter halos with total mass >3 ; 1010 M and circular velocities vc > 50 km s 1 (e.g., Mo & White 2002; Wang et al. 2007).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data Release (2015, methodology): “We have modelled threshold bias (Kaiser 1984; Bardeen et al. 1986; Cole & Kaiser 1989; Sheth, Mo & Tormen 2001; Mo & White 2002) as a combination of a step function θ (ρM − ρ th) (Kitaura et al. 2014) and an exponential cut-off exp [ − ( ρM ρ ) ] (Neyrinck et al. 2014).”