Determining the Hubble constant without the sound horizon: Measurements from galaxy surveys

Philcox, Oliver H. E.; Sherwin, Blake D.; Farren, Gerrit S.; Baxter, Eric J.

doi:10.1103/physrevd.103.023538

Cited by 72 publications

(85 citation statements)

References 43 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In addition, the same analysis is performed with a Ω m prior from uncalibrated BAO (6dFGS, MGS, and eBOSS DR14 Lyman-α measurements) giving H 0 = 65.6 +3. 4 −5.5 km s −1 Mpc −1 at 68% CL [49]. Finally, considering the combination of P (k) with the Planck 2018 CMB-marginalized lensing likelihood [50], and a prior on A s twice tighter than before, reference [49] obtains H 0 = 70.6 +3.…”

Section: Earlymentioning

confidence: 95%

“…4 −5.5 km s −1 Mpc −1 at 68% CL [49]. Finally, considering the combination of P (k) with the Planck 2018 CMB-marginalized lensing likelihood [50], and a prior on A s twice tighter than before, reference [49] obtains H 0 = 70.6 +3. 7 −5.0 km s −1 Mpc −1 at 68% CL.…”

Section: Earlymentioning

confidence: 95%

“…By combining the unreconstructed BOSS DR12 Galaxy power spectra P (k), modeled using the EFTofLSS, assuming a weak Gaussian prior on the amplitude of the scalar PPS A s centered on the Planck best-fit, and a Ω m prior from Pantheon, reference [49] finds H 0 = 65.1 +3.0 −5.4 km s −1 Mpc −1 at 68% CL. In addition, the same analysis is performed with a Ω m prior from uncalibrated BAO (6dFGS, MGS, and eBOSS DR14 Lyman-α measurements) giving H 0 = 65.6 +3.…”

Section: Earlymentioning

confidence: 99%

See 2 more Smart Citations

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,155

760

View full text Add to dashboard Cite

The simplest ΛCDM model provides a good fit to a large span of cosmological data but harbors large areas of phenomenology and ignorance. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant, H 0, made by the early time probes in concert with the ‘vanilla’ ΛCDM cosmological model, and a number of late time, model-independent determinations of H 0 from local measurements of distances and redshifts. The high precision and consistency of the data at both ends present strong challenges to the possible solution space and demands a hypothesis with enough rigor to explain multiple observations—whether these invoke new physics, unexpected large-scale structures or multiple, unrelated errors. A thorough review of the problem including a discussion of recent Hubble constant estimates and a summary of the proposed theoretical solutions is presented here. We include more than 1000 references, indicating that the interest in this area has grown considerably just during the last few years. We classify the many proposals to resolve the tension in these categories: early dark energy, late dark energy, dark energy models with 6 degrees of freedom and their extensions, models with extra relativistic degrees of freedom, models with extra interactions, unified cosmologies, modified gravity, inflationary models, modified recombination history, physics of the critical phenomena, and alternative proposals. Some are formally successful, improving the fit to the data in light of their additional degrees of freedom, restoring agreement within 1–2σ between Planck 2018, using the cosmic microwave background power spectra data, baryon acoustic oscillations, Pantheon SN data, and R20, the latest SH0ES Team Riess, et al (2021 Astrophys. J. 908 L6) measurement of the Hubble constant (H 0 = 73.2 ± 1.3 km s−1 Mpc−1 at 68% confidence level). However, there are many more unsuccessful models which leave the discrepancy well above the 3σ disagreement level. In many cases, reduced tension comes not simply from a change in the value of H 0 but also due to an increase in its uncertainty due to degeneracy with additional physics, complicating the picture and pointing to the need for additional probes. While no specific proposal makes a strong case for being highly likely or far better than all others, solutions involving early or dynamical dark energy, neutrino interactions, interacting cosmologies, primordial magnetic fields, and modified gravity provide the best options until a better alternative comes along.

show abstract

Section: Earlymentioning

confidence: 95%

Section: Earlymentioning

confidence: 95%

Section: Earlymentioning

confidence: 99%

See 1 more Smart Citation

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,155

760

View full text Add to dashboard Cite

show abstract

“…Recent measurements of the Hubble constant H 0 span a range of ∼10% (e.g., Abbott et al 2017Abbott et al , 2018Freedman et al 2019Freedman et al , 2020Riess et al 2019;Wong et al 2020;Choi et al 2020;Khetan et al 2020;Philcox et al 2020;Planck Collaboration et al 2020), and significant tension remains between predictions for H 0 based on early-universe observables and direct late-universe measurements (e.g., Verde et al 2019). Multiply lensed supernovae (SNe) are ideal for measuring time delays and H 0 because of their well-characterized light curves, and in the case of Type Ia, with the added benefit of standardizable luminosity (Refsdal 1964;Oguri & Marshall 2010;Treu 2010).…”

Section: Introductionmentioning

confidence: 99%

Discovering New Strong Gravitational Lenses in the DESI Legacy Imaging Surveys

Huang

Storfer

et al. 2021

ApJ

View full text Add to dashboard Cite

We have conducted a search for new strong gravitational lensing systems in the Dark Energy Spectroscopic Instrument Legacy Imaging Surveys' Data Release 8. We use deep residual neural networks, building on previous work presented by Huang et al. These surveys together cover approximately one-third of the sky visible from the Northern Hemisphere, reaching a z-band AB magnitude of ∼22.5. We compile a training sample that consists of known lensing systems as well as non-lenses in the Legacy Surveys and the Dark Energy Survey. After applying our trained neural networks to the survey data, we visually inspect and rank images with probabilities above a threshold. Here we present 1210 new strong lens candidates.Unified Astronomy Thesaurus concepts: Strong gravitational lensing (1643); High-redshift galaxies (734); AGN host galaxies (2017); Galaxies (573); Galaxy clusters (584); Galaxy groups (597); Quasars (1319)

show abstract

“…Much previous work has investigated how exploiting information contained in the turnover and the full-shape power spectrum on larger scales can break certain degeneracies (Ivanov et al 2020a;Philcox et al 2020;Philcox et al 2021;D'Amico et al 2021), reveal information about curvature (Vagnozzi et al 2021) and also sharpen constraints on beyond ΛCDM models (Chudaykin et al 2021). We refer the reader to these investigations for a more comprehensive analysis of this topic in general.…”

Section: Cosmology From Turnover Scalesmentioning

confidence: 99%

Detecting the power spectrum turnover with HI intensity mapping

Cunnington

2022

Preprint

View full text Add to dashboard Cite

A goal for pathfinder intensity mapping (IM) surveys will be detecting features in the neutral hydrogen (H ) power spectrum, which serve as conclusive evidence of cosmological signals. Observing such features at the expected scales in H IM auto-correlations, where contribution from systematics is uncertain, will provide a more convincing cosmological detection. We demonstrate how the turnover, i.e. the peak of the power spectrum at ultra-large scales, can be detected with H IM. We find that a MeerKAT 4,000 deg 2 survey using the UHF-band is capable of a 3.1𝜎 detection of the turnover, relative to a null model power spectrum with no turnover. This should exceed that capable from current galaxy surveys in optical and near-infrared. The detection significance falls to ∼1𝜎 in MeerKAT's L-band but can reach ∼13𝜎 with the SKAO, which should easily surpass the constraint capable from future Stage-IV-like spectroscopic galaxy surveys. We also propose a new model-independent methodology for constraining the precise turnover scale (𝑘 0 ) and our tests on UHF-band simulated data achieved a precision of 10%. This improved to 2.4% when using the full SKAO. We demonstrate how the results are robust to foreground contamination by using transfer functions, even when an incorrect cosmology has been assumed in their construction. Given that the turnover is related to the horizon scale at matter-radiation equality, a sufficiently precise constraint of 𝑘 0 presents the possibility for a novel probe of cosmology. We therefore present a potential methodology for constructing a standard-ruler-based distance measurement, independent of the sound horizon, using the turnover location in the H power spectrum.

show abstract

Determining the Hubble constant without the sound horizon: Measurements from galaxy surveys

Cited by 72 publications

References 43 publications

In the realm of the Hubble tension—a review of solutions ^*

In the realm of the Hubble tension—a review of solutions ^*

Discovering New Strong Gravitational Lenses in the DESI Legacy Imaging Surveys

Detecting the power spectrum turnover with HI intensity mapping

Contact Info

Product

Resources

About

Determining the Hubble constant without the sound horizon: Measurements from galaxy surveys

Cited by 72 publications

References 43 publications

In the realm of the Hubble tension—a review of solutions *

In the realm of the Hubble tension—a review of solutions *

Discovering New Strong Gravitational Lenses in the DESI Legacy Imaging Surveys

Detecting the power spectrum turnover with HI intensity mapping

Contact Info

Product

Resources

About

In the realm of the Hubble tension—a review of solutions ^*

In the realm of the Hubble tension—a review of solutions ^*