The halo mass function from the dark ages through the present day

By Darren S. Reed, Richard G. Bower, Carlos S. Frenk, Adrian Jenkins, Tom Theuns. 2006

318 citations recorded by the source corpus.

We use an array of high-resolution N-body simulations to determine the mass function of dark matter haloes at redshifts 10-30. We develop a new method for compensating for the effects of finite simulation volume that allows us to find an approximation to the true 'global' mass function. By simulating a wide range of volumes at different mass resolution, we calculate the abundance of haloes of mass 10 5-12 h -1 M ⊙ . This enables us to predict accurately the abundance of the haloes that host the sources that reionize the Universe. In particular, we focus on the small mass haloes (≥10 5.5-6 h -1 M ⊙ ) likely to harbour Population III stars where gas cools by molecular hydrogen emission, early galaxies in which baryons cool by atomic hydrogen emission at a virial temperature of ∼10 4 K (∼10 7.5-8 h -1 M ⊙ ), and massive galaxies that may be observable at redshift ∼10. When we combine our data with simulations that include high-mass haloes at low redshift, we find that the best fit to the halo mass function depends not only on the linear overdensity, as is commonly assumed in analytic models, but also on the slope of the linear power spectrum at the scale of the halo mass. The Press-Schechter model gives a poor fit to the halo mass function in the simulations at all epochs; the Sheth-Tormen model gives a better match, but still overpredicts the abundance of rare objects at all times by up to 50 per cent. Finally, we consider the consequences of the recently released WMAP 3-yr cosmological parameters. These lead to much less structure at high redshift, reducing the number of z = 10 'mini-haloes' by more than a factor of two and the number of z=30 galaxy hosts by nearly four orders of magnitude. Code to generate our best-fitting halo mass function may be downloaded from http://icc.dur.ac.uk/Research/PublicDownloads/genmf.readme.html.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0b773aa43561a24e5aab4dc28e255bb6b0578711

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Citations in the corpus

MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, background): “Different calculations now yield results for e.g. the dark matter halo mass function that agree at the∼ 5−10% level (see e.g. Reed et al. 2007, and references therein).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, background): “There is little ambiguity in this calculation at all redshifts andmasses of interest (zP 6; see, e.g., Reed et al. 2007), and we do not consider it a significant source of uncertainty.”
Galaxies–intergalactic medium interaction calculation – I. Galaxy formation as a function of large-scale environment (2009, background): “The GIMIC mass functions are also compared with the global mass function fit of Reed et al. (2007), which extends to both higher and lower mass scales since it was derived from an ensemble of dark matter simulations covering a wide dynamic range in mass (including the Millennium Simulation; see…”
Building merger trees from cosmological N-body simulations. Towards improving galaxy formation model (2009, background): “Monte-Carlo merging trees not only do not contain position information but they also fail to describe environment effects on low mass halo assembly (Sheth & Tormen 2004; Wechsler et al. 2006; Reed et al. 2007; Zhu et al. 2006).”
The Halo Mass Function: High-Redshift Evolution and Universality (2007, methodology): “Agreement with the Reed et al. (2003, 2007) fits is also good, within the 10% level.”
Large-scale bias and efficient generation of initial conditions for nonlocal primordial non-Gaussianity (2011, background): “While deviations from the former have not yet been established in a precise quantitative way, there is a significant body of work showing that universality of the mass function does not hold at the 5-10% level [40, 52, 53, 71–73] for FOF halos, with more significant deviations for spherical overdens”
Galaxy formation theory (2010, methodology): “The mass function of dark matter halos rises steeply (approximately asM−1.9; Reed et al. 2007) at low masses.”
The galaxy luminosity function at z ≃ 6 and evidence for rapid evolution in the bright end from z ≃ 7 to 5 (2014, methodology): “Evolving the HMF according to the Reed et al. (2007) model, and using the same scaling as at z ' 7, we find the curve shown in Fig.”
An accurate halo model for fitting non-linear cosmological power spectra and baryonic feedback models (2015, background): “Universality in the halo mass function is an approximation and theSheth & Tormen(1999) mass function is only accurate at the≃ 20 per cent level (e.g.,Warren et al. 2006; Reed et al. 2007; Lukić et al. 2007; Tinker et al. 2008; Courtin et al. 2011).”
THE ARECIBO LEGACY FAST ALFA SURVEY. X. THE H i MASS FUNCTION AND FROM THE 40% ALFALFA SURVEY (2010, methodology): “The publicly available GENMF code6 produces halo mass function fits to the Reed et al. (2007) N-body simulations at high resolution, from 105 to 1012 h−1 M⊙.”
Radiative Transfer Simulations of Cosmic Reionization. I. Methodology and Initial Results (2006, background): “Our results are consistent with recent work on the mass function of high-redshift dark matter halos (Reed et al. 2007; Lukic et al. 2007; Cohn & White 2007), and are further confirmation that standard PS underpredicts the abundance of high-redshift halos, particularly at the high-mass end.”
COLOSSUS: A Python Toolkit for Cosmology, Large-scale Structure, and Dark Matter Halos (2017, methodology): “…to Sheth & Tormen 1999 model (FOF, uses δc(z)) warren06 Warren et al. 2006 A calibration based on numerical results (FOF, no z-dependence) reed07 Reed et al. 2007 A model that takes the varying slope of the power spectrum into account (FOF, z-dependent) tinker08 Tinker et al. 2008…”
Simulating cosmic reionization: how large a volume is large enough? (2013, result): “The results confirmed the trend observed previously by us and others (Iliev et al. 2006; Reed et al. 2007; Lukić et al. 2007; Iliev et al. 2012), namely that at the high redshifts of interest here the halo mass functions differ significantly from both the Press-Schechter (Press & Schechter1974)…”
Formation of Galaxy Clusters (2012, background): “…of halos canbe parameterized via a universal function of peak heightν (Bhattacharya et al. 2011, Courtin et al. 2011, Crocce et al. 2010, Evrard et al. 2002, Jenkins et al. 2001, Lukić et al. 2007, Reed et al. 2007, Sheth & Tormen 1999, Tinker et al. 2008, Warren et al. 2006, White 2002).”