Precision Determination of the Mass Function of Dark Matter Halos

By Michael S. Warren, K. Abazajian, D. Holz, L. Teodoro. 2005

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The predicted mass function of dark matter halos is essential in connecting observed galaxy-cluster counts and models of galaxy clustering to the properties of the primordial density field. We determine the mass function in the concordance ΛCDM cosmology, as well as its uncertainty, using sixteen 10243 particle nested-volume dark matter simulations spanning a mass range of over 5 orders of magnitude. Using the nested volumes and single-halo tests, we find and correct for a systematic error in the friends-of-friends halo-finding algorithm. We find a fitting form and full error covariance for the mass function that successfully describes the simulations' mass function and is well behaved outside the simulations' resolutions. Estimated forecasts of uncertainty in cosmological parameters from future cluster-count surveys receive a negligible contribution from remaining statistical uncertainties in the central cosmology multiplicity function. There exists a potentially nonnegligible cosmological dependence (nonuniversality) of the halo multiplicity function.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/01e5596bec821fbf012c4e8468416530fbf870d9

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Citations in the corpus

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).”
Effects of scale-dependent non-Gaussianity on cosmological structures (2007, methodology): “Expressions for the halo mass function in the presence of non-Gaussian initial conditions have been derived as extensions of the Press–Schechter formula [72, 36, 73, 40, 74, 75].”
Toward a Halo Mass Function for Precision Cosmology: The Limits of Universality (2008, methodology): “Warren et al. (2006) have further improved the calibration to ≈ 5% accuracy for a fixed cosmology atz = 0.”
The halo mass function through the cosmic ages (2012, methodology): “Warren et al. (2006) proposed the following correction to particle counts in haloes: Ncorrected = N (1 − N−0.6).”
The MassiveBlack-II simulation: The evolution of haloes and galaxies to z ~ 0 (2014, methodology): “…(orange) lines are for the MFs from Press & Schechter (1974), Sheth & Tormen (2002) and Watson et al. (2013) The solid (black) line in the bottom panels (FOF MFs) denote the best-fitting MF to the MB and MBII data based on the Tinker et al. (2008) parametrization of the Warren et al. (2006) MF.”
The X-Ray Luminosity-Mass Relation for Local Clusters of Galaxies (2006, methodology): “However, Warren et al. (2005) also find that one out of four non-concordance simulations shows a larger discrepancy with the model expectations, roughly 20% in number.”
A COMPREHENSIVE ANALYSIS OF UNCERTAINTIES AFFECTING THE STELLAR MASS–HALO MASS RELATION FOR 0 < z < 4 (2010, background): “…Mass Function Dark matter halo properties over the mass range 1010−1015 M⊙ have been extensively analyzed in simulations (e.g., Jenkins et al. 2001; Warren et al. 2006; Tinker et al. 2008), and the overall cosmology has been constrained by probes such as WMAP (Spergel et al. 2003; Komatsu et al.…”
THE HALO MASS FUNCTION FROM EXCURSION SET THEORY. I. GAUSSIAN FLUCTUATIONS WITH NON-MARKOVIAN DEPENDENCE ON THE SMOOTHING SCALE (2009, background): “(2), the ﬁt to the N - body simulation of Warren et al. (2006), and our result (120).”
The GALEX Arecibo SDSS Survey - VIII. Final data release. The effect of group environment on the gas content of massive galaxies (2013, methodology): “Once the group catalog was finalized, Yang et al. (2007) assigned halo masses via abundance matching, assuming the halo mass function of Warren et al. (2006).”
The MICE Grand Challenge lightcone simulation – II. Halo and galaxy catalogues (2013, methodology): “The exact value depends on whether halo masses are corrected for discreteness following Warren et al. (2006) or not (for poorly resolved haloes the applicability of this correction is unclear and makes the effect worse).”
Constraining primordial non-Gaussianity with future galaxy surveys (2011, methodology): “Fitting formulae that improve agreement with Nbody simulations have also been presented (Sheth & Tormen 1999, 2002; Jenkins et al. 2001; Warren et al. 2006; Tinker et al. 2008; Pillepich et al. 2010).”
Numerical simulations of the dark universe: State of the art and the next decade (2012, methodology): “This prediction is usually parametrized in terms of the linearly extrapolated variance of the underlying DM field [20–22, 216].”
The warm dark matter halo mass function below the cut-off scale (2013, methodology): “In a CDM calculation, essentially all dense structures are always part of haloes, and even the simplest approaches, such as the FoF algorithm, succeed in selecting appropriate objects above a certain mass limit (e.g. Warren et al. 2006; More et al. 2011).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “Above 1015 h−1 M⊙, their fit lies up to 30% above prior calibrations (Jenkins et al. 2001; Warren et al. 2006).”
Structure finding in cosmological simulations: the state of affairs (2013, methodology): “…lines in the upper-left mass function panel represent two analytical mass functions based upon fits to the numerical mass functions found in cosmological simulations: Warren et al. (2006), who use an FOF-based finder for their best-fitting model, and Tinker et al. (2008), who applied an SO finder.”
Lensing and x-ray mass estimates of clusters (simulations) (2012, background): “Second, their mass function is highly sensitive to cosmology, since its evolution traces the growth of the linear density perturbations with exponential magnification (Press & Schechter 1974; Sheth & Tormen 2002; Jenkins et al. 2001; Warren et al. 2006).”
Weighing simulated galaxy clusters using lensing and X-ray (2009, background): “…linear density Chandra Fellow, Fellow of Michigan Society of Fellows, Department of Physics, University of Michigan, 450 Church St., Ann Arbor, MI 48109-1120, USA. perturbations with exponential magnification (Press & Schechter 1974; Sheth & Tormen 2002; Jenkins et al. 2001; Warren et al. 2006).”