COSMOLOGICAL CONSTRAINTS FROM THE SLOAN DIGITAL SKY SURVEY MaxBCG CLUSTER CATALOG

Rozo, Eduardo; Wechsler, Risa H.; Rykoff, E. S.; Annis, J.; Becker, M. R.; Evrard, A. E.; Frieman, Joshua A.; Hansen, S. M.; Hao, Jiangang; Johnston, David; Koester, Benjamin P.; McKay, Timothy A.; Sheldon, E.; Weinberg, David H.

doi:10.1088/0004-637x/708/1/645

Cited by 465 publications

(549 citation statements)

References 59 publications

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“…consistent with recent measurements based on WMAP fiveyear data release (Komatsu et al 2009) and abundance of the Sloan Digital Sky Survey clusters (Rozo et al 2010). The simulation box has a side length equal to 250h −1 Mpc and contains 2048 3 particles, each with mass of 1.35×10 8 h −1 M⊙.…”

Section: Simulationssupporting

confidence: 83%

Orbital anisotropy in cosmological haloes revisited

Wojtak

Gottlöber

Klypin

2013

Monthly Notices of the Royal Astronomical Society

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The velocity anisotropy of particles inside dark matter (DM) haloes is an important physical quantity, which is required for the accurate modelling of mass profiles of galaxies and clusters of galaxies. It is typically measured using the ratio of the radialto-tangential velocity dispersions at a given distance from the halo centre. However, this measure is insufficient to describe the dynamics of realistic haloes, which are not spherical and are typically quite elongated. Studying the velocity distribution in massive DM haloes in cosmological simulations, we find that in the inner parts of the haloes the local velocity ellipsoids are strongly aligned with the major axis of the halo, the alignment being stronger for more relaxed haloes. In the outer regions of the haloes, the alignment becomes gradually weaker and the orientation is more random. These two distinct regions of different degree of the alignment coincide with two characteristic regimes of the DM density profile: a shallow inner cusp and a steep outer profile that are separated by a characteristic radius at which the density declines as ρ ∝ r −2 . This alignment of the local velocity ellipsoids requires reinterpretation of features found in measurements based on the spherically averaged ratio of the radial-to-tangential velocity dispersions. In particular, we show that the velocity distribution in the central halo regions is highly anisotropic. For cluster-size haloes with mass 10 14 − 10 15 h −1 M ⊙ , the velocity anisotropy along the major axis is nearly independent of radius and is equal to β = 1 − σ 2 perp /σ 2 radial ≈ 0.4, which is significantly larger than the previously estimated spherically averaged velocity anisotropy. The alignment of density and velocity anisotropies, and the radial trends may also have some implications for the mass modelling based on kinematical data of such objects as galaxy clusters or dwarf spheroidals, where the orbital anisotropy is a key element in an unbiased mass inference.

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Section: Simulationssupporting

confidence: 83%

Orbital anisotropy in cosmological haloes revisited

Wojtak

Gottlöber

Klypin

2013

Monthly Notices of the Royal Astronomical Society

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“…Prominent examples include the supernova and weak lensing programs of the CFHT Legacy Survey (CFHTLS; Conley et al 2011;Semboloni et al 2006a;Heymans et al 2012b), the ESSENCE supernova survey (Wood-Vasey et al, 2007), BAO measurements from the Sloan Digital Sky Survey (SDSS; Eisenstein et al 2005;Percival et al 2010;Padmanabhan et al 2012), and the SDSS-II supernova survey . These have been complemented by extensive multi-wavelength studies of local and high-redshift supernovae such as the Carnegie Supernova Project (Hamuy et al, 2006;Freedman et al, 2009), by systematic searches for z > 1 supernovae with Hubble Space Telescope Suzuki et al, 2012), by dark energy constraints from the evolution of X-ray or optically selected clusters (Henry et al, 2009;Vikhlinin et al, 2009;Rozo et al, 2010), by improved measurements of the Hubble constant (Riess et al, , 2011Freedman et al, 2012), and by CMB data from the WMAP satellite (Bennett et al, 2003;Larson et al, 2011) and from ground-based experiments that probe smaller angular scales. 4 Most data remain consistent with a spatially flat universe and a cosmological constant with Ω Λ = 1 − Ω m ≈ 0.75, with an uncertainty in the equation-of-state parameter w that is roughly ±0.1 at the 1 − 2σ level.…”

Section: Looking Forwardmentioning

confidence: 99%

“…Because the current X-ray and optical mass calibrations are fundamentally different (hydrostatic vs. weak lensing), the excellent agreement illustrated in Figure 22 provides a strong test of systematic uncertainties. However, the results from the Planck Collaboration et al (2011b) have sounded a cautionary note, as the optical mass estimates used to derive cosmological parameters in Rozo et al (2010) appear to be inconsistent with SZ data (see also Draper et al, 2012). Biesiadzinski et al (2012) have attributed this inconsistency to miscentering, while Angulo et al (2012) point out the importance of systematics covariance.…”

Section: The Current State Of Playmentioning

confidence: 99%

“…Tinker et al (2012) use a halo occupation model (see §2.3) fit to SDSS galaxy clustering, which yields a prediction for the massto-number ratio of clusters 66 as a function of σ 8 and Ω m . While this analysis uses the same weak lensing mass calibration as Rozo et al (2010), the method is less sensitive to the mass scale and is entirely independent of abundance uncertainties, making it a largely independent measurement and a powerful systematics cross-check. The same approach can be adapted to future, deeper photometric surveys.…”

Section: The Current State Of Playmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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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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“…Observations testing the predicted mass function and cluster baryon ⋆ E-mail: amantz@slac.stanford.edu fraction have largely validated CDM (e.g. White et al 1993;Bahcall & Fan 1998;Reiprich & Böhringer 2002;Ettori et al 2003Ettori et al , 2009Allen et al 2004Allen et al , 2008Allen et al , 2011Vikhlinin et al 2009;Mantz et al 2010Mantz et al , 2015bRozo et al 2010;Sehgal et al 2011;Benson et al 2013;Hasselfield et al 2013;Planck Collaboration 2014, 2015.…”

Section: Introductionmentioning

confidence: 99%

Cosmology and astrophysics from relaxed galaxy clusters – V. Consistency with cold dark matter structure formation

Mantz

Allen

Morris

2016

Mon. Not. R. Astron. Soc.

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This is the fifth in a series of papers studying the astrophysics and cosmology of massive, dynamically relaxed galaxy clusters. Our sample comprises 40 clusters identified as being dynamically relaxed and hot in Papers I and II of this series. Here we use constraints on cluster mass profiles from X-ray data to test some of the basic predictions of cosmological structure formation in the Cold Dark Matter (CDM) paradigm. We present constraints on the concentration-mass relation for massive clusters, finding a power-law mass dependence with a slope of κ m = −0.16 ± 0.07, in agreement with CDM predictions. For this relaxed sample, the relation is consistent with a constant as a function of redshift (power-law slope with 1 + z of κ ζ = −0.17 ± 0.26), with an intrinsic scatter of σ ln c = 0.16 ± 0.03. We investigate the shape of cluster mass profiles over the radial range probed by the data (typically ∼ 50 kpc-1 Mpc), and test for departures from the simple Navarro, Frenk & White (NFW) form, for which the logarithmic slope of the density profile tends to −1 at small radii. Specifically, we consider as alternatives the generalized NFW (GNFW) and Einasto parametrizations. For the GNFW model, we find an average value of (minus) the logarithmic inner slope of β = 1.02 ± 0.08, with an intrinsic scatter of σ β = 0.22 ± 0.07, while in the Einasto case we constrain the average shape parameter to be α = 0.29 ± 0.04 with an intrinsic scatter of σ α = 0.12 ± 0.04. Our results are thus consistent with the simple NFW model on average, but we clearly detect the presence of intrinsic, cluster-to-cluster scatter about the average.

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COSMOLOGICAL CONSTRAINTS FROM THE SLOAN DIGITAL SKY SURVEY MaxBCG CLUSTER CATALOG

Cited by 465 publications

References 59 publications

Orbital anisotropy in cosmological haloes revisited

Orbital anisotropy in cosmological haloes revisited

Observational probes of cosmic acceleration

Cosmology and astrophysics from relaxed galaxy clusters – V. Consistency with cold dark matter structure formation

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