Hubble constant difference between CMB lensing and BAO measurements
We apply a tension metric $Q_\textrm{UDM}$, the update difference in mean parameters, to understand the source of the difference in the measured Hubble constant $H_0$ inferred with cosmic microwave background lensing measurements from the Planck satellite ($H_0=67.9^{+1.1}_{-1.3}\, \mathrm{km/s/Mpc}...
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ftdatacite:10.48550/arxiv.2004.10207 2023-05-15T18:22:44+02:00 Hubble constant difference between CMB lensing and BAO measurements Wu, W. L. Kimmy Motloch, Pavel Hu, Wayne Raveri, Marco 2020 https://dx.doi.org/10.48550/arxiv.2004.10207 https://arxiv.org/abs/2004.10207 unknown arXiv https://dx.doi.org/10.1103/physrevd.102.023510 Creative Commons Attribution Non Commercial Share Alike 4.0 International https://creativecommons.org/licenses/by-nc-sa/4.0/legalcode cc-by-nc-sa-4.0 CC-BY-NC-SA Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences article-journal Article ScholarlyArticle Text 2020 ftdatacite https://doi.org/10.48550/arxiv.2004.10207 https://doi.org/10.1103/physrevd.102.023510 2022-03-10T16:21:59Z We apply a tension metric $Q_\textrm{UDM}$, the update difference in mean parameters, to understand the source of the difference in the measured Hubble constant $H_0$ inferred with cosmic microwave background lensing measurements from the Planck satellite ($H_0=67.9^{+1.1}_{-1.3}\, \mathrm{km/s/Mpc}$) and from the South Pole Telescope ($H_0=72.0^{+2.1}_{-2.5}\, \mathrm{km/s/Mpc}$) when both are combined with baryon acoustic oscillation (BAO) measurements with priors on the baryon density (BBN). $Q_\textrm{UDM}$ isolates the relevant parameter directions for tension or concordance where the two data sets are both informative, and aids in the identification of subsets of data that source the observed tension. With $Q_\textrm{UDM}$, we uncover that the difference in $H_0$ is driven by the tension between Planck lensing and BAO+BBN, at probability-to-exceed of 6.6%. Most of this mild tension comes from the galaxy BAO measurements parallel to the line of sight. The redshift dependence of the parallel BAOs pulls both the matter density $Ω_m$ and $H_0$ high in $Λ$CDM, but these parameter anomalies are usually hidden when the BAO measurements are combined with other cosmological data sets with much stronger $Ω_m$ constraints. : 9 pages, 9 figures. Match published version Article in Journal/Newspaper South pole DataCite Metadata Store (German National Library of Science and Technology) Hubble ENVELOPE(158.317,158.317,-80.867,-80.867) South Pole |
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DataCite Metadata Store (German National Library of Science and Technology) |
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ftdatacite |
language |
unknown |
topic |
Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences |
spellingShingle |
Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences Wu, W. L. Kimmy Motloch, Pavel Hu, Wayne Raveri, Marco Hubble constant difference between CMB lensing and BAO measurements |
topic_facet |
Cosmology and Nongalactic Astrophysics astro-ph.CO FOS Physical sciences |
description |
We apply a tension metric $Q_\textrm{UDM}$, the update difference in mean parameters, to understand the source of the difference in the measured Hubble constant $H_0$ inferred with cosmic microwave background lensing measurements from the Planck satellite ($H_0=67.9^{+1.1}_{-1.3}\, \mathrm{km/s/Mpc}$) and from the South Pole Telescope ($H_0=72.0^{+2.1}_{-2.5}\, \mathrm{km/s/Mpc}$) when both are combined with baryon acoustic oscillation (BAO) measurements with priors on the baryon density (BBN). $Q_\textrm{UDM}$ isolates the relevant parameter directions for tension or concordance where the two data sets are both informative, and aids in the identification of subsets of data that source the observed tension. With $Q_\textrm{UDM}$, we uncover that the difference in $H_0$ is driven by the tension between Planck lensing and BAO+BBN, at probability-to-exceed of 6.6%. Most of this mild tension comes from the galaxy BAO measurements parallel to the line of sight. The redshift dependence of the parallel BAOs pulls both the matter density $Ω_m$ and $H_0$ high in $Λ$CDM, but these parameter anomalies are usually hidden when the BAO measurements are combined with other cosmological data sets with much stronger $Ω_m$ constraints. : 9 pages, 9 figures. Match published version |
format |
Article in Journal/Newspaper |
author |
Wu, W. L. Kimmy Motloch, Pavel Hu, Wayne Raveri, Marco |
author_facet |
Wu, W. L. Kimmy Motloch, Pavel Hu, Wayne Raveri, Marco |
author_sort |
Wu, W. L. Kimmy |
title |
Hubble constant difference between CMB lensing and BAO measurements |
title_short |
Hubble constant difference between CMB lensing and BAO measurements |
title_full |
Hubble constant difference between CMB lensing and BAO measurements |
title_fullStr |
Hubble constant difference between CMB lensing and BAO measurements |
title_full_unstemmed |
Hubble constant difference between CMB lensing and BAO measurements |
title_sort |
hubble constant difference between cmb lensing and bao measurements |
publisher |
arXiv |
publishDate |
2020 |
url |
https://dx.doi.org/10.48550/arxiv.2004.10207 https://arxiv.org/abs/2004.10207 |
long_lat |
ENVELOPE(158.317,158.317,-80.867,-80.867) |
geographic |
Hubble South Pole |
geographic_facet |
Hubble South Pole |
genre |
South pole |
genre_facet |
South pole |
op_relation |
https://dx.doi.org/10.1103/physrevd.102.023510 |
op_rights |
Creative Commons Attribution Non Commercial Share Alike 4.0 International https://creativecommons.org/licenses/by-nc-sa/4.0/legalcode cc-by-nc-sa-4.0 |
op_rightsnorm |
CC-BY-NC-SA |
op_doi |
https://doi.org/10.48550/arxiv.2004.10207 https://doi.org/10.1103/physrevd.102.023510 |
_version_ |
1766202150792200192 |