Physical Bayesian modelling of the non-linear matter distribution: New insights into the nearby universe

Jasche, Jens; Lavaux, Guilhem

doi:10.1051/0004-6361/201833710

Cited by 121 publications

(93 citation statements)

References 159 publications

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“…II A we laid out the screening proxies that we consider for segregating Cepheids into screened and unscreened subpopulations. Proxies (i)-(iii) are determined using the screening maps of [99], which synthesises galaxy survey data, halo catalogues from N-body simulations and analytic and numerical structure formation models (based partly on the BORG algorithm [100,101]) to reconstruct the gravitational field out to a distance ∼250 Mpc. Full details can be found in the original paper.…”

Section: A Calculating Fifth Force Strength: the Screening Modelsmentioning

confidence: 99%

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

2019

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The discrepancy between the values of the Hubble constant H 0 derived from the local distance ladder and the Cosmic Microwave Background provides a tantalising hint of new physics. We explore a potential resolution involving screened fifth forces in the local Universe, which alter the Cepheid calibration of supernova distances. In particular, if the Cepheids with direct distance measurements from parallax or water masers are screened but a significant fraction of those in other galaxies are not, neglecting the difference between their underlying period-luminosity relations biases the local H 0 measurement high. This difference derives from a reduction in the Cepheid pulsation period and possible increase in luminosity under a fifth force. We quantify the internal and environmental gravitational properties of the Riess et al. distance ladder galaxies to assess their degrees of screening under a range of phenomenological models, and propagate this information into the H 0 posterior as a function of fifth force strength. We consider well-studied screening models in scalar-tensor gravity theories such as chameleon, K-mouflage and Vainshtein, along with a recently-proposed mechanism based on baryon-dark matter interactions in which screening is governed by the local dark matter density. We find that a fifth force strength ∼ 5 − 30% that of gravity can alleviate the H 0 tension in many scenarios, around the sensitivity level at which tests based on other distance ladder data can constrain this strength. Our most successful models achieve consistency with Planck at the ∼1.5σ level. Although our analysis is exploratory and based on screening models that are not necessarily realised in full theories, our results demonstrate that new physics-based local resolutions of the H 0 tension are possible, supplementing those already known in the pre-recombination era. * harry.desmond@physics.ox.ac.uk

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Section: A Calculating Fifth Force Strength: the Screening Modelsmentioning

confidence: 99%

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

2019

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“…We note that Jasche & Lavaux (2019) failed to detect a Local Hole underdensity in 2M++ data. Nevertheless their Figs.…”

Section: Discussionmentioning

confidence: 66%

Local Hole revisited: evidence for bulk motions and self-consistent outflow

Shanks

Hogarth

Metcalfe

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We revisit our mapping of the 'Local Hole', a large underdensity in the local galaxy redshift distribution that extends out to redshift, z ≈ 0.05 and a potential source of outflows that may perturb the global expansion rate and thus help mitigate the present 'H 0 tension'. First, we compare local peculiar velocities measured via the galaxy average redshift-magnitude Hubble diagram, z(m), with a simple dynamical outflow model based on the average underdensity in the Local Hole. We find that this outflow model is in good agreement with our peculiar velocity measurements from z(m) and not significantly inconsistent with SNIa peculiar velocity measurements from at least the largest previous survey. This outflow could cause an ≈ 2 − 3% increase in the local value of Hubble's constant. Second, considering anisotropic motions, we find that the addition of the outflow model may improve the z(m) fit of a bulk flow where galaxies are otherwise at rest in the Local Group frame. We conclude that the Local Hole plus neighbouring overdensities such as the Shapley Supercluster may cause outflow and bulk motions out to ≈ 150h −1 Mpc that are cosmologically significant and that need to be taken into account in estimating Hubble's constant.

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“…In this Appendix we present an alternative measurement of the local density field δ 0 (R) using the Bayesian Origin Reconstruction from Galaxies (BORG) method of Ref. [21] for reconstructing the dark matter density field. This technique provides samples from the full posterior of the dark matter density field given the 2M++ galaxy catalogue.…”

Section: Acknowledgementsmentioning

confidence: 99%

Impact of our local environment on cosmological statistics

Hall

2020

Phys. Rev. D

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We conduct a thorough investigation into the possibility that residing in an overdense region of the Universe may induce bias in measurements of the large-scale structure. We compute the conditional correlation function and angular power spectrum of density and lensing fluctuations while holding the local spherically-averaged density fixed and show that for Gaussian fields this has no effect on the angular power at l > 0. We identify a range of scales where a perturbative approach allows analytic progress to be made, and we compute leading-order conditional power spectra using an Edgeworth expansion and second-order perturbation theory. We find no evidence for any significant bias to cosmological power spectra from our local density contrast. We show that when smoothed over a large region around the observer, conditioning on the local density typically affects density power spectra by less than a percent at cosmological distances, below cosmic variance. We find that while typical corrections to the lensing angular power spectrum can be at the 10% level on the largest angular scales and for source redshifts zs 0.1, for the typical redshifts targeted by upcoming wide imaging surveys the corrections are sub-percent and negligible, in contrast to previous claims in the literature. Using an estimate of the local spherically-averaged density from a composite galaxy redshift catalogue we find that the corrections from conditioning on our own local density are below cosmic variance and subdominant to other non-linear effects. We discuss the potential implications of our results for cosmology and point out that a measurement of the local density contrast may be used as a consistency test of cosmological models. * Electronic address: ahall@roe.ac.uk 1 https://sci.esa.int/web/euclid 2 https://www.lsst.org/ 3 https://www.desi.lbl.gov/

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Physical Bayesian modelling of the non-linear matter distribution: New insights into the nearby universe

Cited by 121 publications

References 159 publications

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

Local Hole revisited: evidence for bulk motions and self-consistent outflow

Impact of our local environment on cosmological statistics

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