The halo bias inside cosmic voids

Verza, Giovanni; Carbone, C.; Renzi, A.

doi:10.48550/arxiv.2207.04039

Cited by 3 publications

(5 citation statements)

References 87 publications

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“…Mass-weighted profiles are amplified with respect to number density profiles, featuring higher compensation walls and deeper cores, most notably for small voids. This implies that the least massive halos tend to reside closer to the void centers, whereas more massive halos are rather located in the more clustered regions at the void boundary, as expected from previous studies [e.g., 48,103]. For larger voids, however, this effect diminishes.…”

Section: Mass Weightingsupporting

confidence: 69%

“…However, this only applies when the threshold is defined in the full matter density field and when spherical symmetry is assumed. For voids defined in the number density field of tracers one additionally has to account for the tracer bias [27,[101][102][103]. Moreover, the sparsity of tracer particles effectively smooths the density field on scales below their typical separation, which can affect density ridges between voids [104].…”

Section: Vide Void Findingmentioning

confidence: 99%

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Why Cosmic Voids Matter: Nonlinear Structure & Linear Dynamics

Schuster¹,

Hamaus²,

Dolag³

et al. 2022

Preprint

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We use the Magneticum suite of state-of-the-art hydrodynamical simulations to identify cosmic voids based on the watershed technique and investigate their most fundamental properties across different resolutions in mass and scale. This encompasses the distributions of void sizes, shapes, and content, as well as their radial density and velocity profiles traced by the distribution of cold dark matter particles and halos. We also study the impact of various tracer properties, such as their sparsity and mass, and the influence of void merging on these summary statistics. Our results reveal that all of the analyzed void properties are physically related to each other and describe universal characteristics that are largely independent of tracer type and resolution. Most notably, we find that the motion of tracers around void centers is perfectly consistent with linear dynamics, both for individual, as well as stacked voids. Despite the large range of scales accessible in our simulations, we are unable to identify the occurrence of nonlinear dynamics even inside voids of only a few Mpc in size. This suggests voids to be among the most pristine probes of cosmology down to scales that are commonly referred to as highly nonlinear in the field of large-scale structure.

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Section: Mass Weightingsupporting

confidence: 69%

Section: Vide Void Findingmentioning

confidence: 99%

Why Cosmic Voids Matter: Nonlinear Structure & Linear Dynamics

Schuster¹,

Hamaus²,

Dolag³

et al. 2022

Preprint

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“…The DEMNUni simulations have been produced with the aim of investigating the clustering of large scale structures in the presence of massive neutrinos and DDE and they were conceived for the nonlinear analysis and modelling of different probes, including dark matter halo-and galaxy-clustering [67,[69][70][71][72][73][74], CMB lensing, SZ and ISW effects [68,75,76], cosmic void statistics [77][78][79][80], and cross-correlations among these probes [81,82].…”

Section: The Demnuni Simulationsmentioning

confidence: 99%

DEMNUni: comparing nonlinear power spectra prescriptions in the presence of massive neutrinos and dynamical dark energy

Parimbelli

Carbone

Bel

et al. 2022

J. Cosmol. Astropart. Phys.

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We provide an accurate comparison, against large cosmological N-body simulations, of different prescriptions for modelling nonlinear matter power spectra in the presence of massive neutrinos and dynamical dark energy. We test the current most widely used approaches: fitting functions (HALOFIT and HMcode), the halo-model reaction (ReACT) and emulators (baccoemu and EuclidEmulator2). Focussing on redshifts z ≤ 2 and scales k ≲ 1 h/Mpc (where the simulation mass resolution provides ∼ 1% accuracy), we find that HMcode and ReACT considerably improve over the HALOFIT prescriptions of Smith and Takahashi (both combined with the Bird correction), with an overall agreement of 2% for all the cosmological scenarios considered. Concerning emulators, we find that, especially at low redshifts, EuclidEmulator2 remarkably agrees with the simulated spectra at ≲ 1% level in scenarios with dynamical dark energy and massless neutrinos, reaching a maximum difference of ∼ 2% at z = 2. baccoemu has a similar behaviour as EuclidEmulator2, except for a couple of dark energy models. In cosmologies with massive neutrinos, at z = 0 all the nonlinear prescriptions improve their agreement with respect to the massless neutrino case, except for the Bird and TakaBird models which, however, are not tailored to w 0–wa models. At z > 0 we do not find a similar improvement when including massive neutrinos, probably due to the lower impact of neutrino free-streaming at higher redshifts; rather at z = 2 EuclidEmulator2 exceeds 2% agreement for some dark energy equation of state. When considering ratios between the matter power spectrum computed in a given cosmological model and its ΛCDM counterpart, all the tested prescriptions agree with simulated data, at sub-percent or percent level, depending on z. Finally, we also test how nonlinear prescriptions compare against simulations when computing cosmic shear and angular galaxy clustering spectra. For the former, we find a 2–3% agreement for HMcode, baccoemu, EuclidEmulator2 and ReACT; for the latter, due to the minimum stellar mass of the simulated galaxies, shot noise highly affects the signal and makes the discrepancies as high as 5%.

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“…The Main Galaxy Sample (MGS; Strauss et al 2002 ) is a selection of galaxies from the SDSS-I and SDSS-II surv e ys' (York et al 2000 ) Data Release 7 (DR7; Abazajian et al 2009 ), at redshifts z < 0.2, with spectra taken using spectrographs mounted on the 2.5-m telescope at Apache Point Observatory in New Mexico (Gunn et al 2006 ). A subsample of this catalogue, created for large-scale structure analyses, is described by Ross et al ( 2015 ) and Howlett et al ( 2015b ), which used additional colour, magnitude, and redshift cuts to obtain a high-bias ( b ∼ 1.5) sample of galaxies occupying dark matter haloes with M halo > 10 12 M , and with a high galaxy density.…”

Section: Mgsmentioning

confidence: 99%

“…In this paper, we build on previous work developed for the cosmological analysis of voids to analyse galaxy samples within the Sloan Digital Sky Survey (SDSS-II; York et al 2000 ). We analyse the Main Galaxy Sample (MGS; Howlett et al 2015b ;Ross et al 2015 ), the Baryon Oscillation Spectroscopic Surv e y (BOSS; Da wson et al 2013 ) of SDSS-III (Eisenstein et al 2011 ), and the extended BOSS (eBOSS; Dawson et al 2016 ) of SDSS-IV (Blanton et al 2017 ), co v ering a wide range in redshift using a single analysis method for the first time.…”

Section: Introductionmentioning

confidence: 99%

Measurements of cosmic expansion and growth rate of structure from voids in the Sloan Digital Sky Survey between redshift 0.07 and 1.0

Woodfinden

Nadathur

Percival

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present measurements of the anisotropic cross-correlation of galaxies and cosmic voids in data from the Sloan Digital Sky Survey Main Galaxy Sample (MGS), Baryon Oscillation Spectroscopic Survey (BOSS) and extended BOSS (eBOSS) luminous red galaxy catalogues from SDSS Data Releases 7, 12 and 16, covering the redshift range 0.07 < z < 1.0. As in our previous work analysing voids in subsets of these data, we use a reconstruction method applied to the galaxy data before void-finding in order to remove selection biases when constructing the void samples. We report results of a joint fit to the multipole moments of the measured cross-correlation for the growth rate of structure, fσ8(z), and the ratio DM(z)/DH(z) of the comoving angular diameter distance to the Hubble distance, in six redshift bins. For DM/DH, we are able to achieve a significantly higher precision than that obtained from analyses of the baryon acoustic oscillations (BAO) and galaxy clustering in the same datasets. Our growth rate measurements are of lower precision but still comparable with galaxy clustering results. For both quantities, the results agree well with the expectations for a ΛCDM model. Assuming a flat Universe, our results correspond to a measurement of the matter density parameter $\Omega _\mathrm{m}=0.337^{+0.026}_{-0.029}$. For more general models the degeneracy directions obtained are consistent with and complementary to those from other cosmological probes. These results consolidate void-galaxy cross-correlation measurements as a pillar of modern observational cosmology.

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The halo bias inside cosmic voids

Cited by 3 publications

References 87 publications

Why Cosmic Voids Matter: Nonlinear Structure & Linear Dynamics

Why Cosmic Voids Matter: Nonlinear Structure & Linear Dynamics

DEMNUni: comparing nonlinear power spectra prescriptions in the presence of massive neutrinos and dynamical dark energy

Measurements of cosmic expansion and growth rate of structure from voids in the Sloan Digital Sky Survey between redshift 0.07 and 1.0

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