Large-scale non-Gaussian mass function and halo bias: tests on<i>N</i>-body simulations

Grossi, M.; Verde, Licia; Carbone, C.; Dolag, K.; Branchini, E.; Iannuzzi, Francesca; Matarrese, S.; Moscardini, L.

doi:10.1111/j.1365-2966.2009.15150.x

Cited by 163 publications

(321 citation statements)

References 59 publications

(188 reference statements)

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“…A final caveat related to the halo mass function is that primordial non-Gaussianity could alter its form (e.g., Weinberg and Cole, 1992;Dalal et al, 2008;Grossi et al, 2009;LoVerde and Smith, 2011;D'Amico et al, 2011) and thereby change the cluster abundances predicted for a given dark energy model (e.g., Pillepich et al, 2012). Of course, evidence for non-Gaussian initial conditions would be exciting in its own right, with important implications for early-universe physics.…”

Section: Theoretical Systematicsmentioning

confidence: 99%

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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Section: Theoretical Systematicsmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…2 our results for the halo mass function with numerical simulations from Grossi et al (2009). They use the LSS convention for f NL , so that in terms of the CMB convention used in this article this corresponds to f NL ±151.…”

Section: Mass Functionmentioning

confidence: 99%

“…we can have the hierarchy Γ (0) Γ (1) 1 Γ (2) ). Since the low-mass tail (49) does not match numerical simulations, it is sometimes proposed to keep the ratio (58) given by the Press-Schechter mass function, and to multiply the fit from simulations of the Gaussian mass function by this factor (Grossi et al 2007(Grossi et al , 2009Lo Verde et al 2008). However, this procedure clearly violates the normalization condition (54).…”

Section: Mass Functionmentioning

confidence: 99%

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Mass function and bias of dark matter halos for non-Gaussian initial conditions

Valageas

2010

A&A

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Aims. We revisit the derivation of the mass function and the bias of dark matter halos for non-Gaussian initial conditions. Methods. We use a steepest-descent approach to point out that exact results can be obtained for the high-mass tail of the halo mass function and the two-point correlation of massive halos. Focusing on primordial non-Gaussianity of the local type, we check that these results agree with numerical simulations. Results. The high-mass cutoff of the halo mass function takes the same form as the one obtained from the Press-Schechter formalism, but with a linear threshold δ L that depends on the definition of the halo (i.e. δ L 1.59 for a nonlinear density contrast of 200). We show that a simple formula, which obeys this high-mass asymptotic and uses the fit obtained for Gaussian initial conditions, matches numerical simulations while keeping the mass function normalized to unity. Next, by deriving the real-space halo two-point correlation in the spirit of Kaiser (1984, ApJ, 284, L9) and taking a Fourier transform, we obtain good agreement with simulations for the correction to the halo bias, Δb M (k, f NL ), due to primordial non-Gaussianity. Therefore, neither the halo mass function nor the bias require an ad-hoc parameter q (such as δ c → δ c √ q), provided one uses the correct linear threshold δ L and pays attention to halo displacements. The nonlinear real-space expression can be useful for checking that the "linearized" bias is a valid approximation. Moreover, it clearly shows how the baryon acoustic oscillation at ∼100 h −1 Mpc is amplified by the bias of massive halos and modified by primordial non-Gaussianity. On smaller scales, 30 < x < 90 h −1 Mpc, the correction to the real-space bias roughly scales asThe low-k behavior of the halo bias does not imply a divergent real-space correlation, so that one does not need to introduce counterterms that depend on the survey size.

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“…2014) and numerical N-body (dark matter only) simulation (see e.g. Kang et al 2007;Grossi et al 2007Grossi et al , 2009Desjacques, Seljak & Iliev 2009;Pillepich et al 2010;Wagner et al 2010;Smith, Desjacques & Marian 2011;Wagner & Verde 2012) methods.…”

Section: Introductionmentioning

confidence: 99%

Effect of primordial non-Gaussianities on galaxy clusters scaling relations

Trindade¹,

Silva²

2017

Monthly Notices of the Royal Astronomical Society

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Galaxy clusters are a valuable source of cosmological information. Their formation and evolution depends on the underlying cosmology and on the statistical nature of the primordial density fluctuations. In this work we investigate the impact of primordial non-gaussianities (PNG) on the scaling properties of galaxy clusters. We performed a series of cosmological hydrodynamic N-body simulations featuring adiabatic gas physics and different levels of nonGaussian initial conditions within the ΛCDM framework. We focus on the T −M, S −M, Y −M and Y X − M scalings relating the total cluster mass with temperature, entropy and SZ cluster integrated pressure that reflect the thermodynamical state of the intra-cluster medium. Our results show that PNG have an impact on cluster scalings laws. The mass power-law indexes of the scalings are almost unaffected by the existence of PNG but the amplitude and redshift evolution of their normalizations are clearly affected. The effect is stronger for the evolution of the Y − M and Y X − M normalizations, which change by as much as 22% and 16% when f NL varies from −500 to 500, respectively. These results are consistent with the view that positive/negative f NL affect cluster profiles due to an increase/decrease of cluster concentrations. At low values of f NL , as suggested by present Planck constraints on a scale invariant f NL , the impact on the scalings normalizations is only a few percent, which is small when compared with the effect of additional gas physics and other cosmological effects such as dark energy. However if f NL is in fact a scale dependent parameter, PNG may have larger positive/negative amplitudes at clusters scales and therefore our results suggest that PNG should be taken into account when galaxy cluster data is used to infer cosmological parameters or to asses the constraining power of future cluster surveys.

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Large-scale non-Gaussian mass function and halo bias: tests onN-body simulations

Cited by 163 publications

References 59 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Mass function and bias of dark matter halos for non-Gaussian initial conditions

Effect of primordial non-Gaussianities on galaxy clusters scaling relations

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