QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI
We derive linearly polarized astrophysical component maps in the Northern Sky from the QUIJOTE-MFI data at 11 and 13?GHz in combination with the Wilkinson Microwave Anisotropy Probe K and Ka bands (23 and 33?GHz) and all Planck polarized channels (30-353-GHz), using the parametric component separati...
| Autores: | , , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2023 |
| País: | España |
| Institución: | Universidad de Cantabria (UC) |
| Repositorio: | UCrea Repositorio Abierto de la Universidad de Cantabria |
| Idioma: | inglés |
| OAI Identifier: | oai:repositorio.unican.es:10902/27713 |
| Acceso en línea: | https://hdl.handle.net/10902/27713 |
| Access Level: | acceso abierto |
| Palabra clave: | Cosmology: Observations Methods: Data Analysis Polarization Cosmic Microwave Background |
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| dc.title.none.fl_str_mv |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI |
| title |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI |
| spellingShingle |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI Hoz López-Collado, Elena de la Cosmology: Observations Methods: Data Analysis Polarization Cosmic Microwave Background |
| title_short |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI |
| title_full |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI |
| title_fullStr |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI |
| title_full_unstemmed |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI |
| title_sort |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI |
| dc.creator.none.fl_str_mv |
Hoz López-Collado, Elena de la Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Vielva Martínez, Patricio|||0000-0003-0051-272X Martínez González, Enrique Rubiño-Martín, J.A. Casaponsa Galí, Biuse Guidi, Federica Ashdown, Mark Génova Santos, Ricardo Tanausú Artal, E. Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Fernández Cobos, Raúl|||0000-0001-6185-7903 Fernández-Torreiro, M. Herranz Muñoz, Diego|||0000-0003-4540-1417 Watson, R.A. |
| author |
Hoz López-Collado, Elena de la |
| author_facet |
Hoz López-Collado, Elena de la Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Vielva Martínez, Patricio|||0000-0003-0051-272X Martínez González, Enrique Rubiño-Martín, J.A. Casaponsa Galí, Biuse Guidi, Federica Ashdown, Mark Génova Santos, Ricardo Tanausú Artal, E. Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Fernández Cobos, Raúl|||0000-0001-6185-7903 Fernández-Torreiro, M. Herranz Muñoz, Diego|||0000-0003-4540-1417 Watson, R.A. |
| author_role |
author |
| author2 |
Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Vielva Martínez, Patricio|||0000-0003-0051-272X Martínez González, Enrique Rubiño-Martín, J.A. Casaponsa Galí, Biuse Guidi, Federica Ashdown, Mark Génova Santos, Ricardo Tanausú Artal, E. Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Fernández Cobos, Raúl|||0000-0001-6185-7903 Fernández-Torreiro, M. Herranz Muñoz, Diego|||0000-0003-4540-1417 Watson, R.A. |
| author2_role |
author author author author author author author author author author author author author author |
| dc.contributor.none.fl_str_mv |
Universidad de Cantabria |
| dc.subject.none.fl_str_mv |
Cosmology: Observations Methods: Data Analysis Polarization Cosmic Microwave Background |
| topic |
Cosmology: Observations Methods: Data Analysis Polarization Cosmic Microwave Background |
| description |
We derive linearly polarized astrophysical component maps in the Northern Sky from the QUIJOTE-MFI data at 11 and 13?GHz in combination with the Wilkinson Microwave Anisotropy Probe K and Ka bands (23 and 33?GHz) and all Planck polarized channels (30-353-GHz), using the parametric component separation method B-SeCRET. The addition of QUIJOTE-MFI data significantly improves the parameter estimation of the low-frequency foregrounds, especially the estimation of the synchrotron spectral index, [beta]s. We present the first detailed ?s map of the Northern Celestial Hemisphere at a smoothing scale of 2°. We find statistically significant spatial variability across the sky. We obtain an average value of ?3.08 and a dispersion of 0.13, considering only pixels with reliable goodness of fit. The power-law model of the synchrotron emission provides a good fit to the data outside the Galactic plane but fails to track the complexity within this region. Moreover, when we assume a synchrotron model with uniform curvature, cs, we find a value of cs = ?0.0797 ± 0.0012. However, there is insufficient statistical significance to determine which model is favoured, either the power law or the power law with uniform curvature. Furthermore, we estimate the thermal dust spectral parameters in polarization. Our cosmic microwave background, synchrotron, and thermal dust maps are highly correlated with the corresponding products of the PR4 Planck release, although some large-scale differences are observed in the synchrotron emission. Finally, we find that the ?s estimation in the high signal-to-noise synchrotron emission areas is prior-independent, while, outside these regions, the prior governs the [beta]s estimation. |
| publishDate |
2023 |
| dc.date.none.fl_str_mv |
2023 2023-01-01 |
| dc.type.none.fl_str_mv |
journal article http://purl.org/coar/resource_type/c_6501 NA http://purl.org/coar/version/c_be7fb7dd8ff6fe43 |
| dc.type.openaire.fl_str_mv |
info:eu-repo/semantics/article |
| format |
article |
| dc.identifier.none.fl_str_mv |
https://hdl.handle.net/10902/27713 |
| url |
https://hdl.handle.net/10902/27713 |
| dc.language.none.fl_str_mv |
Inglés eng |
| language_invalid_str_mv |
Inglés |
| language |
eng |
| dc.rights.none.fl_str_mv |
open access http://purl.org/coar/access_right/c_abf2 Attribution 4.0 International http://creativecommons.org/licenses/by/4.0/ |
| dc.rights.openaire.fl_str_mv |
info:eu-repo/semantics/openAccess |
| rights_invalid_str_mv |
open access http://purl.org/coar/access_right/c_abf2 Attribution 4.0 International http://creativecommons.org/licenses/by/4.0/ |
| eu_rights_str_mv |
openAccess |
| dc.publisher.none.fl_str_mv |
Oxford University Press |
| publisher.none.fl_str_mv |
Oxford University Press |
| dc.source.none.fl_str_mv |
Monthly notices of the Royal Astronomical Society, 2023, (519)3, 3504-3525 reponame:UCrea Repositorio Abierto de la Universidad de Cantabria instname:Universidad de Cantabria (UC) |
| instname_str |
Universidad de Cantabria (UC) |
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UCrea Repositorio Abierto de la Universidad de Cantabria |
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UCrea Repositorio Abierto de la Universidad de Cantabria |
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|
| _version_ |
1869415855777906688 |
| spelling |
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFIHoz López-Collado, Elena de laBarreiro Vilas, Rita Belén|||0000-0002-6139-4272Vielva Martínez, Patricio|||0000-0003-0051-272XMartínez González, EnriqueRubiño-Martín, J.A.Casaponsa Galí, BiuseGuidi, FedericaAshdown, MarkGénova Santos, Ricardo TanausúArtal, E.Casas Reinares, Francisco Javier|||0000-0002-2217-5843Fernández Cobos, Raúl|||0000-0001-6185-7903Fernández-Torreiro, M.Herranz Muñoz, Diego|||0000-0003-4540-1417Watson, R.A.Cosmology: ObservationsMethods: Data AnalysisPolarizationCosmic Microwave BackgroundWe derive linearly polarized astrophysical component maps in the Northern Sky from the QUIJOTE-MFI data at 11 and 13?GHz in combination with the Wilkinson Microwave Anisotropy Probe K and Ka bands (23 and 33?GHz) and all Planck polarized channels (30-353-GHz), using the parametric component separation method B-SeCRET. The addition of QUIJOTE-MFI data significantly improves the parameter estimation of the low-frequency foregrounds, especially the estimation of the synchrotron spectral index, [beta]s. We present the first detailed ?s map of the Northern Celestial Hemisphere at a smoothing scale of 2°. We find statistically significant spatial variability across the sky. We obtain an average value of ?3.08 and a dispersion of 0.13, considering only pixels with reliable goodness of fit. The power-law model of the synchrotron emission provides a good fit to the data outside the Galactic plane but fails to track the complexity within this region. Moreover, when we assume a synchrotron model with uniform curvature, cs, we find a value of cs = ?0.0797 ± 0.0012. However, there is insufficient statistical significance to determine which model is favoured, either the power law or the power law with uniform curvature. Furthermore, we estimate the thermal dust spectral parameters in polarization. Our cosmic microwave background, synchrotron, and thermal dust maps are highly correlated with the corresponding products of the PR4 Planck release, although some large-scale differences are observed in the synchrotron emission. Finally, we find that the ?s estimation in the high signal-to-noise synchrotron emission areas is prior-independent, while, outside these regions, the prior governs the [beta]s estimation.We thank the staff of the Teide Observatory for invaluable assistance in the commissioning and operation of QUIJOTE. The QUIJOTE experiment is being developed by the Instituto de Astrofisica de Canarias (IAC), the Instituto de Fisica de Cantabria (IFCA), and the Universities of Cantabria, Manchester, and Cambridge. Partial financial support was provided by the Spanish Ministry of Science and Innovation under the projects AYA2007-68058-C03-01, AYA2007- 68058-C03-02, AYA2010-21766-C03-01, AYA2010-21766-C03-02, AYA2014-60438-P, ESP2015-70646-C2-1-R, AYA2017-84185-P, ESP2017-83921-C2-1-R, AYA2017-90675-REDC (co-funded with EU FEDER funds), PGC2018-101814-B-I00, PID2019-110610RBC21, PID2020-120514GB-I00, IACA13-3E-2336, IACA15-BE3707, EQC2018-004918-P, the Severo Ochoa Programs SEV-2015- 0548 and CEX2019-000920-S, the Maria de Maeztu Program MDM2017-0765, and by the Consolider-Ingenio project CSD2010-00064 (EPI: Exploring the Physics of Inflation). We acknowledge support from the ACIISI, Consejeria de Economia, Conocimiento y Empleo del Gobierno de Canarias, and the European Regional Development Fund (ERDF) under grant with reference ProID2020010108. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement number 687312 (RADIOFOREGROUNDS). EdlH acknowledges financial support from the Concepcion´ Arenal Programme of the Universidad de Cantabria. DT acknowledges the support from the Chinese Academy of Sciences (CAS) President’s International Fellowship Initiative (PIFI) with grant no. 2020PM0042. FP acknowledges support from the Spanish State Research Agency (AEI) under grant number PID2019-105552RB-C43. The authors acknowledge the computer resources, technical expertise, and assistance provided by the Spanish Supercomputing Network (RES) node at Universidad de Cantabria. Some of the presented results are based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA) and the Planck Legacy Archive (PLA). Support for LAMBDA is provided by the NASA Office of Space Science. Some of the results in this paper have been derived using the HEALPIX package (Gorski ´ et al. 2005), and the HEALPY (Zonca et al. 2019), NUMPY (Harris et al. 2020), EMCEE (ForemanMackey et al. 2013), and MATPLOTLIB (Hunter 2007) PYTHON packages.Oxford University PressUniversidad de Cantabria20232023-01-01journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articlehttps://hdl.handle.net/10902/27713Monthly notices of the Royal Astronomical Society, 2023, (519)3, 3504-3525reponame:UCrea Repositorio Abierto de la Universidad de Cantabriainstname:Universidad de Cantabria (UC)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Attribution 4.0 Internationalhttp://creativecommons.org/licenses/by/4.0/info:eu-repo/semantics/openAccessoai:repositorio.unican.es:10902/277132026-06-02T12:39:31Z |
| score |
15,298079 |