Toward a Halo Mass Function for Precision Cosmology: The Limits of Universality

Tinker, Jeremy L.; Kravtsov, Andrey V.; Klypin, Anatoly; Abazajian, Kevork N.; Warren, Michael S.; Yepes, Gustavo; Gottlöber, Stefan; Holz, D. E.

doi:10.1086/591439

Cited by 1,853 publications

(2,661 citation statements)

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“…(A3) provides a good approximation. Fitting the approximation to the mass function proposed by Tinker et al (2008), we found that at z 0.3 (1.0), β1 6.8 (11.3) around a pivot mass of M200 = 5 × 10 14 M /h for the standard ΛCDM cosmology.…”

Section: Appendix A: the Mass Functionmentioning

confidence: 80%

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Sereno¹,

Ettori²

2015

Monthly Notices of the Royal Astronomical Society

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The scaling of observable properties of galaxy clusters with mass evolves with time. Assessing the role of the evolution is crucial to study the formation and evolution of massive halos and to avoid biases in the calibration. We present a general method to infer the mass and the redshift dependence, and the time-evolving intrinsic scatter of the mass-observable relations. The procedure self-calibrates the redshift dependent completeness function of the sample. The intrinsic scatter in the mass estimates used to calibrate the relation is considered too. We apply the method to the scaling of mass M ∆ versus line of sight galaxy velocity dispersion σ v , optical richness, X-ray luminosity, L X , and Sunyaev-Zel'dovich signal. Masses were calibrated with weak lensing measurements. The measured relations are in good agreement with time and mass dependencies predicted in the self-similar scenario of structure formation. The lone exception is the L X -M ∆ relation whose time evolution is negative in agreement with formation scenarios with additional radiative cooling and uniform preheating at high redshift. The intrinsic scatter in the σ v -M ∆ relation is notably small, of order of 14 per cent. Robust predictions on the observed properties of the galaxy clusters in the CLASH sample are provided as cases of study. Catalogs and scripts are publicly available at

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Section: Appendix A: the Mass Functionmentioning

confidence: 80%

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Sereno¹,

Ettori²

2015

Monthly Notices of the Royal Astronomical Society

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“…Here δ c is the linear theory overdensity at which a spherically symmetric perturbation would collapse. 16 In detail, Tinker et al (2008) find that f (σ) depends on redshift at the 10-20% level, probably because of the dependence of halo mass profiles on Ω m (z). At overdensities of ∼ 200, the baryon fraction in group and cluster mass halos (M > 10 13 M ⊙ ) is expected to be close to the cosmic mean ratio Ω b /Ω m , but gas pressure, dissipation, and feedback from star formation and AGN can alter this fraction and change baryon density profiles relative to dark matter profiles.…”

Section: Cmb Anisotropies and Large Scale Structurementioning

confidence: 97%

“…To a first approximation, the function f (σ) is universal, and the effects of power spectrum shape, redshift (and thus power spectrum amplitude), and background cosmological model (e.g., Ω m and Ω Λ ) enter only through determining |d ln σ/dM | andρ m . The state-of-the-art numerical investigation is that of Tinker et al (2008), who fit a large number of N-body simulation results with the functional form…”

Section: Cmb Anisotropies and Large Scale Structurementioning

confidence: 99%

“…Within a reasonable range, such variation is acceptable, provided each study is self-consistent and the halocluster relation is accurately characterized. In recent years, numerical studies have mostly shifted from the friends-of-friends algorithm used in earlier work (e.g., Efstathiou et al 1988) to spherical overdensity definitions (e.g., Tinker et al 2008), thus avoiding the tendency of the friends-of-friends method to occasionally link distinct mass concentrations via narrow bridges (see More et al, 2011, and references therein for a more detailed discussion). Halo boundaries are typically drawn at overdensities ∆ ≈ 100 − 500, where clusters are in approximate dynamical equilibrium and where mass predictions are fairly robust to baryonic physics.…”

Section: General Principlesmentioning

confidence: 99%

“…We plot the ratio α/α σ -computed using the Tinker et al (2008) mass function rather than the Press-Schechter mass function -in Figure 25. (141), these figures allow one to quickly estimate how well σ 11,abs (z) can be constrained at each redshift by a galaxy cluster sample with N clusters.…”

Section: Expected Numbers and Cosmological Sensitivitymentioning

confidence: 99%

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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The current standard model for the evolution of cosmic structure is reviewed, tracing its development over the last forty years and focussing specifically on the role played by numerical simulations and on aspects related to the nature of dark matter. PreambleThe development of a standard model of cosmological structure formation over the last forty years must count as one of the great success stories in Physics. The model describes the geometry and material content of the Universe, explaining how structure -galaxies of various sizes and types, groups and clusters of galaxies, the entire cosmic web of filaments and voids -emerged from a hot and near-uniform Big Bang. This astonishing richness appears to have grown from quantum zero-point fluctuations produced during a period of cosmic inflation occurring very soon after the beginning of our Universe. Over the subsequent 13.7 billion years, these small density perturbations were amplified by the relentless action of gravitational forces due predominantly to dark matter, but illuminated by complex astrophysical phenomena involving ordinary matter. In the standard model, the dark matter, which makes up five sixths of all matter, is hypothesised to be a weakly interacting non-baryonic elementary particle, created in the early stages of cosmic evolution.In this article we will review the standard model of cosmic structure formation, focusing on the nonlinear processes that transformed the near-uniform universe that emerged from the Big Bang into the highly structured world we observe today. We will highlight the critical role that computer simulations have played in understanding this transformation, emphasizing gravitational phenomena associated with the dark matter, and only rather briefly discussing the crucially important, but more complex, processes that shape the directly observable baryonic components. Rather than presenting a complete and thorough review of the literature, our intention is to provide an account of the main ideas and advances that have shaped the subject. We begin by presenting in Table 1 a chronological listing of the landmark developments that have driven this remarkable story.

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Toward a Halo Mass Function for Precision Cosmology: The Limits of Universality

Cited by 1,853 publications

References 65 publications

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Observational probes of cosmic acceleration

Dark matter and cosmic structure

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