The void size function in dynamical dark energy cosmologies

Verza, Giovanni; Pisani, Alice; Carbone, C.; Hamaus, Nico; Guzzo, L.

doi:10.1088/1475-7516/2019/12/040

Cited by 69 publications

(87 citation statements)

References 142 publications

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“…Understanding the tracer bias around voids is crucial for many other cosmological tests involving voids, for example when modeling their abundance (Jennings et al 2013;Chan et al 2014;Pisani et al 2015;Achitouv et al 2015;Ronconi & Marulli 2017;Ronconi et al 2019;Contarini et al 2019;Verza et al 2019), or RSDs (Hamaus et al 2015(Hamaus et al , 2016(Hamaus et al , 2017Cai et al 2016;Chuang et al 2017;Achitouv et al 2017;Hawken et al 2017;Achitouv 2019;Correa et al 2019). Thanks to the state-of-the-art DES Year 1 (Y1) shear catalogue (Zuntz et al 2018), we have access to the lensing signal by both 2D and 3D voids with unprecedented accuracy.…”

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confidence: 99%

Dark Energy Survey year 1 results: the relationship between mass and light around cosmic voids

Fang

Hamaus

Jain

et al. 2019

Monthly Notices of the Royal Astronomical Society

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What are the mass and galaxy profiles of cosmic voids? In this paper, we use two methods to extract voids in the Dark Energy Survey (DES) Year 1 redMaGiC galaxy sample to address this question. We use either 2D slices in projection, or the 3D distribution of galaxies based on photometric redshifts to identify voids. For the mass profile, we measure the tangential shear profiles of background galaxies to infer the excess surface mass density. The signal-to-noise ratio for our lensing measurement ranges between 10.7 and 14.0 for the two void samples. We infer their 3D density profiles by fitting models based on N-body simulations and find good agreement for void radii in the range 15–85 Mpc. Comparison with their galaxy profiles then allows us to test the relation between mass and light at the 10 per cent level, the most stringent test to date. We find very similar shapes for the two profiles, consistent with a linear relationship between mass and light both within and outside the void radius. We validate our analysis with the help of simulated mock catalogues and estimate the impact of photometric redshift uncertainties on the measurement. Our methodology can be used for cosmological applications, including tests of gravity with voids. This is especially promising when the lensing profiles are combined with spectroscopic measurements of void dynamics via redshift-space distortions.

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Section: Take Down Policymentioning

confidence: 99%

Dark Energy Survey year 1 results: the relationship between mass and light around cosmic voids

Fang

Hamaus

Jain

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Two of the most important cosmological statistics in void studies are the void size function, that describes the abundance of voids (Sheth & van de Weygaert 2004;Furlanetto & Piran 2006;Jennings et al 2013;Achitouv et al 2015;Pisani et al 2015;Ronconi & Marulli 2017;Contarini et al 2019;Ronconi et al 2019;Verza et al 2019), and the void-galaxy cross-correlation function, that characterises the density and peculiar velocity fields around them (Paz et al 2013;Hamaus et al 2015;Cai et al 2016;Hamaus et al 2016;Achitouv 2017;Achitouv et al 2017;Chuang et al 2017;Hamaus et al 2017;Hawken et al 2017;Achitouv 2019;Nadathur & Percival 2019;Nadathur et al 2019a,b;Hawken et al 2020;Hamaus et al 2020;Nadathur et al 2020;Paillas et al 2021). Both statistics are affected by distortions in the observed spatial distribution of the galaxies, which translate into anisotropic patterns.…”

Section: Introductionmentioning

confidence: 99%

Redshift-space effects in voids and their impact on cosmological tests. Part I: the void size function

Correa

Paz

Sánchez

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Voids are promising cosmological probes. Nevertheless, every cosmological test based on voids must necessarily employ methods to identify them in redshift space. Therefore, redshift-space distortions (RSD) and the Alcock-Paczyński effect (AP) have an impact on the void identification process itself generating distortion patterns in observations. Using a spherical void finder, we developed a statistical and theoretical framework to describe physically the connection between the identification in real and redshift space. We found that redshift-space voids above the shot noise level have a unique real-space counterpart spanning the same region of space, they are systematically bigger and their centres are preferentially shifted along the line of sight. The expansion effect is a by-product of RSD induced by tracer dynamics at scales around the void radius, whereas the off-centring effect constitutes a different class of RSD induced at larger scales by the global dynamics of the whole region containing the void. The volume of voids is also altered by the fiducial cosmology assumed to measure distances, this is the AP change of volume. These three systematics have an impact on cosmological statistics. In this work, we focus on the void size function. We developed a theoretical framework to model these effects and tested it with a numerical simulation, recovering the statistical properties of the abundance of voids in real space. This description depends strongly on cosmology. Hence, we lay the foundations for improvements in current models of the abundance of voids in order to obtain unbiased cosmological constraints from redshift surveys.

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“…Park et al 2012;Hwang et al 2016). In particular, the void statistics including abundance, shape, and density profile have been utilized to constrain dark energy (Lee & Park 2009;Lavaux & Wandelt 2010;Bos et al 2012;Pisani et al 2015;Verza et al 2019), the interaction between dark sectors (Li 2011;Sutter et al 2015), gravity theories (Peebles 2001;Nusser et al 2005;Li et al 2012;Cai et al 2015), and initial conditions (Blumenthal et al 1992;van de Weygaert & van Kampen 1993;Colberg et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Identification of Cosmic Voids as Massive Cluster Counterparts

Shim,

Park,

Kim

et al. 2020

Preprint

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We develop a method to identify cosmic voids from the matter density field by adopting a physicallymotivated concept that voids are the counterpart of massive clusters. To prove the concept we use a pair of ΛCDM simulations, a reference and its initial density-inverted mirror simulation, and study the relation between the effective size of voids and the mass of corresponding clusters. Galaxy cluster-scale dark matter halos are identified in the Mirror simulation at z = 0 by linking dark matter particles. The void corresponding to each cluster is defined in the Reference simulation as the region occupied by the member particles of the cluster. We study the voids corresponding to the halos more massive than 10 13 h −1 M . We find a power-law scaling relation between the void size and the corresponding cluster mass. Voids with corresponding cluster mass above 10 15 h −1 M occupy ∼ 1% of the total simulated volume, whereas this fraction increases to ∼ 54% for voids with corresponding cluster mass above 10 13 h −1 M . It is also found that the density profile of the identified voids follows a universal functional form. Based on these findings, we propose a method to identify cluster-counterpart voids directly from the matter density field without their mirror information by utilizing three parameters such as the smoothing scale, density threshold, and minimum core fraction. We recover voids corresponding to clusters more massive than 3×10 14 h −1 M at 70-74 % level of completeness and reliability. Our results suggest that we are able to identify voids in a way to associate them with clusters of a particular massscale.

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The void size function in dynamical dark energy cosmologies

Cited by 69 publications

References 142 publications

Dark Energy Survey year 1 results: the relationship between mass and light around cosmic voids

Dark Energy Survey year 1 results: the relationship between mass and light around cosmic voids

Redshift-space effects in voids and their impact on cosmological tests. Part I: the void size function

Identification of Cosmic Voids as Massive Cluster Counterparts

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