{"about":{"site":"https://codewithpapers.app","non_affiliation":"Code with Papers and Syntology are not affiliated with, endorsed by, or sponsored by Papers with Code, Meta, or the pwc-archive mirror.","licence":"CC BY-SA 4.0","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","attribution":"https://codewithpapers.app/attribution","modified":"archive material modified by Syntology; see the attribution page"},"url":"/paper/dark-energy-from-the-thermal-sunyaev","title":"Dark Energy from the Thermal Sunyaev Zeldovich Power Spectrum","arxiv_id":"1712.00788","date":"2017-12-03","proceeding":null,"authors":["Boris Bolliet","Barbara Comis","Eiichiro Komatsu","Juan Francisco Macías-Pérez"],"abstract":"We constrain the dark energy equation of state parameter, $w$, using the power spectrum of the thermal Sunyaev-Zeldovich (tSZ) effect. We improve upon previous analyses by taking into account the trispectrum in the covariance matrix and marginalising over the foreground parameters, the correlated noise, the mass bias $B$ in the Planck universal pressure profile, and all the relevant cosmological parameters (i.e., not just $\\Omega_{\\mathrm{m}}$ and $\\sigma_8$). We find that the amplitude of the tSZ power spectrum at $\\ell\\lesssim 10^3$ depends primarily on $F\\equiv \\sigma_{8}(\\Omega_{{\\mathrm{m}}}/B)^{0.40}h^{-0.21}$, where $B$ is related to more commonly used variable $b$ by $B=(1-b)^{-1}$. We measure this parameter with 2.6\\% precision, $F=0.460\\pm 0.012$ (68% CL). By fixing the bias to $B=1.25$ and adding the local determination of the Hubble constant $H_0$ and the amplitude of the primordial power spectrum constrained by the Planck Cosmic Microwave Background (CMB) data, we find $w=-1.10\\pm0.12$, $\\sigma_{\\mathrm{8}}=0.802\\pm0.037$, and $\\Omega_{{\\mathrm{m}}}=0.265\\pm0.022$ (68% CL). Our limit on $w$ is consistent with and is as tight as that from the distance-alone constraint from the CMB and $H_0$. Finally, by combining the tSZ power spectrum and the CMB data we find, in the $\\Lambda$ Cold Dark Matter (CDM) model, the mass bias of $B=1.71\\pm 0.17$, i.e., $1-b=0.58\\pm 0.06$ (68% CL).","url_abs":"https://arxiv.org/abs/1712.00788v2","url_pdf":"https://arxiv.org/pdf/1712.00788v2.pdf","source":{"archive":"pwc-archive (Hugging Face), CC BY-SA 4.0","snapshot":"2025-07-28","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","row_kind":"links_only","authors_date_abstract":"arXiv metadata, CC0 1.0 (https://info.arxiv.org/help/license), from the Kaggle arXiv metadata snapshot of 2026-09-12"},"code_links":[{"paper_slug":"dark-energy-from-the-thermal-sunyaev","repo_url":"https://github.com/borisbolliet/class_sz","is_official":1,"mentioned_in_paper":0,"mentioned_in_github":1,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}