Imprint of primordial non-Gaussianity on dark matter halo profiles

Dizgah, Azadeh Moradinezhad; Dodelson, Scott; Riotto, Antonio

doi:10.1103/physrevd.88.063513

Cited by 9 publications

(9 citation statements)

References 35 publications

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“…These results are in line with the predictions that f NL changes the internal structure of cluster profiles, as a result of an increase/decrease of cluster concentrations for positive/negative f NL (Smith, Desjacques & Marian 2011;Moradinezhad Dizgah, Dodelson & Riotto 2013). The impact on cluster scaling relations is mostly due to changes in the evolution of their normalizations.…”

Section: Discussionsupporting

confidence: 90%

“…More sophisticated approaches rely on galaxy cluster scaling relations derived from hydrodynamic or N-body simulations, calibrated by observations, that do not include primordial non-gaussianities (see eg Mak & Pierpaoli 2012;Roncarelli et al 2010). This procedure is clearly not ideal given that non-gaussianities are known to influence the internal structure of clusters (Smith, Desjacques & Marian 2011;Moradinezhad Dizgah, Dodelson & Riotto 2013) and therefore they may cause significant changes in the slope and normalization of galaxy cluster scalings. The study of the impact of PNG on cluster scaling relations is also essential for an accurate characterization of the physical state of the ICM gass and to assess the relative strength of cosmological effects shaping the evolution of galaxy clusters.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Discussionsupporting

confidence: 90%

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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“…In all those studies it has been found that the presence of pNG modifies the abundances of halos and voids increasingly with the rarity of the object. While in principle the presence of pNG might also alter the density profiles of rare objects, the impact on halo profiles has been observed to be small (Moradinezhad Dizgah et al 2013) and a similar study for voids that is underway shows no perceptible differences on void profiles. 1 Furthermore, following an observation from Dalal et al (2008); Desjacques et al (2009), pNG leads to strongly scaledependent bias that impacts the large-scale clustering of rare objects (peaks of the density distribution such as halos) which hence can be used to constrain pNG from large scale structure (Slosar et al 2008).…”

Section: Abundance and Large Scale Clustering Of Rare Objectsmentioning

confidence: 90%

Hunting high and low: disentangling primordial and late-time non-Gaussianity with cosmic densities in spheres

Uhlemann

Pajer

Pichon

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Non-Gaussianities of dynamical origin are disentangled from primordial ones using the formalism of large deviation statistics with spherical collapse dynamics. This is achieved by relying on accurate analytical predictions for the one-point probability distribution function (PDF) and the two-point clustering of spherically-averaged cosmic densities (sphere bias). Sphere bias extends the idea of halo bias to intermediate density environments and voids as underdense regions. In the presence of primordial non-Gaussianity, sphere bias displays a strong scale dependence relevant for both high and low density regions, which is predicted analytically. The statistics of densities in spheres are built to model primordial non-Gaussianity via an initial skewness with a scale-dependence that depends on the bispectrum of the underlying model. The analytical formulas with the measured nonlinear dark matter variance as input are successfully tested against numerical simulations. For local non-Gaussianity with a range from f NL = −100 to +100 they are found to agree within 2% or better for densities ρ ∈ [0.5, 3] in spheres of radius 15 Mpc/h down to z = 0.35. The validity of the large deviation statistics formalism is thereby established for all observationally relevant local-type departures from perfectly Gaussian initial conditions. The corresponding estimators for the amplitude of the nonlinear variance σ 8 and primordial skewness f NL are validated using a fiducial joint maximum likelihood experiment. The influence of observational effects and the prospects for a future detection of primordial non-Gaussianity from joint one-and two-point densities-in-spheres statistics are discussed.

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“…The primordial non-Gaussianity can be imprinted even in the profiles of the galactic halos (Moradinezhad Dizgah, Dodelson & Riotto 2013), thus linking the latter to the inflationary phase of the Universe . Halo properties can thus be probes for the nature of perturbations; for example, even though we presently possess no observable evidence of non-adiabatic (iso-curvature) perturbations, we have strong constraints on their possible resistance and it was shown that during re-ionization the iso-curvature modes are transferred to adiabatic ones (Weinberg 2004).…”

Section: Introductionmentioning

confidence: 99%

Rotating baryonic dark halos

Paolis

Gurzadyan

Nucita

et al. 2019

A&A

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Galactic halos are of great importance for our understanding of both the dark matter nature and primordial non-Gaussianity in the perturbation spectrum, a powerful discriminant of the physical mechanisms that generated the cosmological fluctuations observed today. In this paper we analyze Planck data towards the galaxy M104 (Sombrero) and find an asymmetry in the microwave temperature which extends up to about 1 0 from the galactic center. This frequency-independent asymmetry is consistent with that induced by the Doppler effect due to the galactic rotation and we find a probability of less than about 0.2% that it is due to a random fluctuation of the microwave background. In addition, Planck data indicate the relatively complex dynamics of the M104 galactic halo, and this appears to be in agreement with previous studies. In view of our previous analysis of the dark halos of nearby galaxies, this finding confirms the efficiency of the method used in revealing and mapping the dark halos around relatively nearby edge-on galaxies.

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Imprint of primordial non-Gaussianity on dark matter halo profiles

Cited by 9 publications

References 35 publications

Effect of primordial non-Gaussianities on galaxy clusters scaling relations

Effect of primordial non-Gaussianities on galaxy clusters scaling relations

Hunting high and low: disentangling primordial and late-time non-Gaussianity with cosmic densities in spheres

Rotating baryonic dark halos

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