A Bayesian method for point source polarisation estimation

The estimation of the polarisation P of extragalactic compact sources in cosmic microwave background (CMB) images is a very important task in order to clean these images for cosmological purposes ?for example, to constrain the tensor-to-scalar ratio of primordial fluctuations during inflation? and a...

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Autores: Herranz Muñoz, Diego|||0000-0003-4540-1417, Argüeso, F., To olatti, L., Manjón García, Alberto|||0000-0002-7413-8825, López Caniego, M.
Tipo de recurso: artículo
Fecha de publicación:2021
País:España
Institución:Universidad de Cantabria (UC)
Repositorio:UCrea Repositorio Abierto de la Universidad de Cantabria
Idioma:inglés
OAI Identifier:oai:repositorio.unican.es:10902/25002
Acceso en línea:http://hdl.handle.net/10902/25002
Access Level:acceso abierto
Palabra clave:Methods: data analysis
Techniques: image processing
Polarization
Cosmic background radiation
Radio continuum: galaxies
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spelling A Bayesian method for point source polarisation estimationHerranz Muñoz, Diego|||0000-0003-4540-1417Argüeso, F.To olatti, L.Manjón García, Alberto|||0000-0002-7413-8825López Caniego, M.Methods: data analysisTechniques: image processingPolarizationCosmic background radiationRadio continuum: galaxiesThe estimation of the polarisation P of extragalactic compact sources in cosmic microwave background (CMB) images is a very important task in order to clean these images for cosmological purposes ?for example, to constrain the tensor-to-scalar ratio of primordial fluctuations during inflation? and also to obtain relevant astrophysical information about the compact sources themselves in a frequency range, ????10?200 GHz, where observations have only very recently started to become available. In this paper, we propose a Bayesian maximum a posteriori approach estimation scheme which incorporates prior information about the distribution of the polarisation fraction of extragalactic compact sources between 1 and 100 GHz. We apply this Bayesian scheme to white noise simulations and to more realistic simulations that include CMB intensity, Galactic foregrounds, and instrumental noise with the characteristics of the QUIJOTE (Q U I JOint TEnerife) experiment wide survey at 11 GHz. Using these simulations, we also compare our Bayesian method with the frequentist filtered fusion method that has been already used in the Wilkinson Microwave Anisotropy Probe data and in the Planck mission. We find that the Bayesian method allows us to decrease the threshold for a feasible estimation of P to levels below ?100 mJy (as compared to ?500 mJy which was the equivalent threshold for the frequentist filtered fusion). We compare the bias introduced by the Bayesian method and find it to be small in absolute terms. Finally, we test the robustness of the Bayesian estimator against uncertainties in the prior and in the flux density of the sources. We find that the Bayesian estimator is robust against moderate changes in the parameters of the prior and almost insensitive to realistic errors in the estimated photometry of the sources.We thank the Spanish MINECO and the Spanish Ministerio de Ciencia, Innovación y Universidades for partial financial support under projects AYA2015-64508-P and PGC2018-101814-B-I00, respectively. D. H. also acknowledges funding from the European Union’s Horizon 2020 research and innovation programme (COMPET-05-2015) under grant agreement number 687312 (RADIOFOREGROUNDS). Some of the results in this paper have been derived using the HEALPix (Górski et al. 2005) and healpy (Zonca et al. 2019) packages. This research made use of astropy, (http://www.astropy.org) a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), matplotlib, a Python library for publication quality graphics (Hunter 2007), and SciPy, a Python-based ecosystem of open-source software for mathematics, science, and engineering (Virtanen et al. 2020). We acknowledge Santander Supercomputacion support group at the University of Cantabria (UC) who provided access to the supercomputer Altamira Supercomputer at the Institute of Physics of Cantabria (IFCA-UC-CSIC), member of the Spanish Supercomputing Network (https://www.res.es/en/about), for performing simulations/analyses.EDP SciencesUniversidad de Cantabria20212021-01-01journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articlehttp://hdl.handle.net/10902/25002Astronomy & Astrophysics. Vol 651, Jul 2021. A24reponame:UCrea Repositorio Abierto de la Universidad de Cantabriainstname:Universidad de Cantabria (UC)InglésengEuropean Commission http://dx.doi.org/10.13039/501100000780 Horizon 2020 Framework Programme 687312open accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:repositorio.unican.es:10902/250022026-06-02T12:39:31Z
dc.title.none.fl_str_mv A Bayesian method for point source polarisation estimation
title A Bayesian method for point source polarisation estimation
spellingShingle A Bayesian method for point source polarisation estimation
Herranz Muñoz, Diego|||0000-0003-4540-1417
Methods: data analysis
Techniques: image processing
Polarization
Cosmic background radiation
Radio continuum: galaxies
title_short A Bayesian method for point source polarisation estimation
title_full A Bayesian method for point source polarisation estimation
title_fullStr A Bayesian method for point source polarisation estimation
title_full_unstemmed A Bayesian method for point source polarisation estimation
title_sort A Bayesian method for point source polarisation estimation
dc.creator.none.fl_str_mv Herranz Muñoz, Diego|||0000-0003-4540-1417
Argüeso, F.
To olatti, L.
Manjón García, Alberto|||0000-0002-7413-8825
López Caniego, M.
author Herranz Muñoz, Diego|||0000-0003-4540-1417
author_facet Herranz Muñoz, Diego|||0000-0003-4540-1417
Argüeso, F.
To olatti, L.
Manjón García, Alberto|||0000-0002-7413-8825
López Caniego, M.
author_role author
author2 Argüeso, F.
To olatti, L.
Manjón García, Alberto|||0000-0002-7413-8825
López Caniego, M.
author2_role author
author
author
author
dc.contributor.none.fl_str_mv Universidad de Cantabria
dc.subject.none.fl_str_mv Methods: data analysis
Techniques: image processing
Polarization
Cosmic background radiation
Radio continuum: galaxies
topic Methods: data analysis
Techniques: image processing
Polarization
Cosmic background radiation
Radio continuum: galaxies
description The estimation of the polarisation P of extragalactic compact sources in cosmic microwave background (CMB) images is a very important task in order to clean these images for cosmological purposes ?for example, to constrain the tensor-to-scalar ratio of primordial fluctuations during inflation? and also to obtain relevant astrophysical information about the compact sources themselves in a frequency range, ????10?200 GHz, where observations have only very recently started to become available. In this paper, we propose a Bayesian maximum a posteriori approach estimation scheme which incorporates prior information about the distribution of the polarisation fraction of extragalactic compact sources between 1 and 100 GHz. We apply this Bayesian scheme to white noise simulations and to more realistic simulations that include CMB intensity, Galactic foregrounds, and instrumental noise with the characteristics of the QUIJOTE (Q U I JOint TEnerife) experiment wide survey at 11 GHz. Using these simulations, we also compare our Bayesian method with the frequentist filtered fusion method that has been already used in the Wilkinson Microwave Anisotropy Probe data and in the Planck mission. We find that the Bayesian method allows us to decrease the threshold for a feasible estimation of P to levels below ?100 mJy (as compared to ?500 mJy which was the equivalent threshold for the frequentist filtered fusion). We compare the bias introduced by the Bayesian method and find it to be small in absolute terms. Finally, we test the robustness of the Bayesian estimator against uncertainties in the prior and in the flux density of the sources. We find that the Bayesian estimator is robust against moderate changes in the parameters of the prior and almost insensitive to realistic errors in the estimated photometry of the sources.
publishDate 2021
dc.date.none.fl_str_mv 2021
2021-01-01
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 http://hdl.handle.net/10902/25002
url http://hdl.handle.net/10902/25002
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.relation.none.fl_str_mv European Commission http://dx.doi.org/10.13039/501100000780 Horizon 2020 Framework Programme 687312
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
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
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv Astronomy & Astrophysics. Vol 651, Jul 2021. A24
reponame:UCrea Repositorio Abierto de la Universidad de Cantabria
instname:Universidad de Cantabria (UC)
instname_str Universidad de Cantabria (UC)
reponame_str UCrea Repositorio Abierto de la Universidad de Cantabria
collection UCrea Repositorio Abierto de la Universidad de Cantabria
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,300724

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