{"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/polarization-fraction-of-planck-galactic-cold","title":"Polarization fraction of Planck Galactic cold clumps and forecasts for the Simons Observatory","arxiv_id":"2303.02788","date":"2023-03-05","proceeding":null,"authors":["J. Clancy","G. Puglisi","S. E. Clark","G. Coppi","G. Fabbian","C. Hervias-Caimapo","J. C. Hill","F. Nati","C. L. Reichardt"],"abstract":"We measure the polarization fraction of a sample of $6282$ Galactic cold clumps at $353 \\, \\mathrm{GHz} $, consisting of $Planck$ Galactic cold clump (PGCC) catalogue category 1 objects (flux densities measured with signal-to-noise ratio $(\\mathrm{S/N}) > 4$). We find the mean-squared polarization fraction at $353 \\, \\mathrm{GHz} $ to be $ \\langle \\Pi ^ 2 \\rangle = [ 4.79 \\pm 0.44 ] \\times 10 ^ {-4} $ equating to an $ 11 \\, \\sigma $ detection of polarization. We test if the polarization fraction depends on the clumps' physical properties, including flux density, luminosity, Galactic latitude and physical distance. We see a trend towards increasing polarization fraction with increasing Galactic latitude, but find no evidence that polarization depends on the other tested properties. The Simons Observatory, with an angular resolution of order $1 \\, \\mathrm{arcmin } $ and noise levels between $22$ and $54$ $ \\mu \\mathrm{ K-arcmin } $ at high frequencies, will substantially enhance our ability to determine the magnetic field structure in Galactic cold clumps. At $\\ge5\\,\\sigma$ significance, we predict the Simons Observatory will detect at least $\\sim12,000$ cold clumps in intensity and $\\sim430$ cold clumps in polarization. This number of polarization detections would represent a two orders of magnitude increase over the current $Planck$ results. We also release software that can be used to mask these Galactic cold clumps in other analyses.","url_abs":"https://arxiv.org/abs/2303.02788v3","url_pdf":"https://arxiv.org/pdf/2303.02788v3.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":"polarization-fraction-of-planck-galactic-cold","repo_url":"https://github.com/justinc97/pgcc_mask_generation","is_official":1,"mentioned_in_paper":1,"mentioned_in_github":0,"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}