{"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/modeling-parity-violating-spectra-in-galactic","title":"Modeling parity-violating spectra in Galactic dust polarization with filaments and its applications to cosmic birefringence searches","arxiv_id":"2408.06214","date":"2024-08-12","proceeding":null,"authors":["Carlos Hervías-Caimapo","Ari J. Cukierman","Patricia Diego-Palazuelos","Kevin M. Huffenberger","Susan E. Clark"],"abstract":"We extend the dust-filament-based model presented in Herv\\'ias-Caimapo & Huffenberger 2022 to produce parity-violating foreground spectra by manipulating the filament orientations relative to the magnetic field. We calibrate our model to observations of the misalignment angle using cross-correlations of Planck and HI 21-cm line data, producing a fiducial model that predicts a $\\mathcal{D}_{\\ell}^{EB}\\sim$few $\\mu$K$^2$ dust signal at 353 GHz and where $\\sim 56$\\% of filaments have a positive misalignment angle. The main purpose of this model is to be used as dust with non-zero parity-violating emission in forecasting a measurement of cosmic birefringence by upcoming experiments. Here, we also use our fiducial model to assess the impact of dust in measurements of the isotropic cosmic birefringence angle $\\beta$ with Planck data by measuring the misalignment angle as a function of scale, as well as directly using our model's $\\mathcal{D}_{\\ell}^{EB}$ prediction as a template. In both cases, we measure $\\beta$ to be consistent within $0.83\\sigma$ of the analyses that use the 353 GHz channel of Planck to constrain the filamentary misalignment or that use the commander sky model as a template for the dust $\\mathcal{D}_{\\ell}^{EB}$ spectrum. We attribute this consistency to the extra degrees of freedom introduced by the ad-hoc amplitude parameters for the dust parity-violating spectrum, which are capable of absorbing most of the differences between the model and data as long as a reasonable dust model is provided.","url_abs":"https://arxiv.org/abs/2408.06214v3","url_pdf":"https://arxiv.org/pdf/2408.06214v3.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":"modeling-parity-violating-spectra-in-galactic","repo_url":"https://github.com/chervias/DustFilaments","is_official":1,"mentioned_in_paper":0,"mentioned_in_github":0,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"syntology_url":null,"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}