QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument
We present QUIJOTE intensity and polarization maps in four frequency bands centred around 11, 13, 17, and 19-GHz, and covering approximately 29?000?deg2, including most of the northern sky region. These maps result from 9000?h of observations taken between May 2013 and June 2018 with the first QUIJO...
| 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:10902/27714 |
| Acceso en línea: | https://hdl.handle.net/10902/27714 |
| Access Level: | acceso abierto |
| Palabra clave: | Cosmology: Observations Cosmic Background Radiation Instrumentation: Polarimeters Methods: Data Analysis |
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oai:repositorio.unican.es:10902/27714 |
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España |
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| dc.title.none.fl_str_mv |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument |
| title |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument |
| spellingShingle |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument Herranz Muñoz, Diego|||0000-0003-4540-1417 Cosmology: Observations Cosmic Background Radiation Instrumentation: Polarimeters Methods: Data Analysis |
| title_short |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument |
| title_full |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument |
| title_fullStr |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument |
| title_full_unstemmed |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument |
| title_sort |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrument |
| dc.creator.none.fl_str_mv |
Herranz Muñoz, Diego|||0000-0003-4540-1417 Vielva Martínez, Patricio|||0000-0003-0051-272X Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Bilbao Ahedo, Juan Daniel Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Casaponsa Galí, Biuse Hoz López-Collado, Elena de la Fernández Cobos, Raúl|||0000-0001-6185-7903 Martínez González, Enrique |
| author |
Herranz Muñoz, Diego|||0000-0003-4540-1417 |
| author_facet |
Herranz Muñoz, Diego|||0000-0003-4540-1417 Vielva Martínez, Patricio|||0000-0003-0051-272X Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Bilbao Ahedo, Juan Daniel Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Casaponsa Galí, Biuse Hoz López-Collado, Elena de la Fernández Cobos, Raúl|||0000-0001-6185-7903 Martínez González, Enrique |
| author_role |
author |
| author2 |
Vielva Martínez, Patricio|||0000-0003-0051-272X Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Bilbao Ahedo, Juan Daniel Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Casaponsa Galí, Biuse Hoz López-Collado, Elena de la Fernández Cobos, Raúl|||0000-0001-6185-7903 Martínez González, Enrique |
| author2_role |
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 Cosmic Background Radiation Instrumentation: Polarimeters Methods: Data Analysis |
| topic |
Cosmology: Observations Cosmic Background Radiation Instrumentation: Polarimeters Methods: Data Analysis |
| description |
We present QUIJOTE intensity and polarization maps in four frequency bands centred around 11, 13, 17, and 19-GHz, and covering approximately 29?000?deg2, including most of the northern sky region. These maps result from 9000?h of observations taken between May 2013 and June 2018 with the first QUIJOTE multifrequency instrument (MFI), and have angular resolutions of around 1°, and sensitivities in polarization within the range 35?40?µK per 1° beam, being a factor ?2?4 worse in intensity. We discuss the data processing pipeline employed, and the basic characteristics of the maps in terms of real space statistics and angular power spectra. A number of validation tests have been applied to characterize the accuracy of the calibration and the residual level of systematic effects, finding a conservative overall calibration uncertainty of 5 per?cent. We also discuss flux densities for four bright celestial sources (Tau A, Cas A, Cyg A, and 3C274), which are often used as calibrators at microwave frequencies. The polarization signal in our maps is dominated by synchrotron emission. The distribution of spectral index values between the 11?GHz and WMAP 23?GHz map peaks at [Beta] = -3.09 with a standard deviation of 0.14. The measured BB/EE ratio at scales of [L lower case+ = 80 is 0.26 ± 0.07 for a Galactic cut |b| > 10°. We find a positive TE correlation for 11?GHz at large angular scales ([L lower case+ [less than or equivalent to] 50), while the EB and TB signals are consistent with zero in the multipole range 30 [less than or equivalent to] [L lower case+ [less than or equivalent to] 150. The maps discussed in this paper are publicly available. |
| 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/10902/27714 |
| url |
https://hdl.handle.net/10902/27714 |
| 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 |
| 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 |
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), 3383-3431 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 |
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|
| repository.mail.fl_str_mv |
|
| _version_ |
1869408998121275392 |
| spelling |
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20-GHz with the multifrequency instrumentHerranz Muñoz, Diego|||0000-0003-4540-1417Vielva Martínez, Patricio|||0000-0003-0051-272XBarreiro Vilas, Rita Belén|||0000-0002-6139-4272Bilbao Ahedo, Juan DanielCasas Reinares, Francisco Javier|||0000-0002-2217-5843Casaponsa Galí, BiuseHoz López-Collado, Elena de laFernández Cobos, Raúl|||0000-0001-6185-7903Martínez González, EnriqueCosmology: ObservationsCosmic Background RadiationInstrumentation: PolarimetersMethods: Data AnalysisWe present QUIJOTE intensity and polarization maps in four frequency bands centred around 11, 13, 17, and 19-GHz, and covering approximately 29?000?deg2, including most of the northern sky region. These maps result from 9000?h of observations taken between May 2013 and June 2018 with the first QUIJOTE multifrequency instrument (MFI), and have angular resolutions of around 1°, and sensitivities in polarization within the range 35?40?µK per 1° beam, being a factor ?2?4 worse in intensity. We discuss the data processing pipeline employed, and the basic characteristics of the maps in terms of real space statistics and angular power spectra. A number of validation tests have been applied to characterize the accuracy of the calibration and the residual level of systematic effects, finding a conservative overall calibration uncertainty of 5 per?cent. We also discuss flux densities for four bright celestial sources (Tau A, Cas A, Cyg A, and 3C274), which are often used as calibrators at microwave frequencies. The polarization signal in our maps is dominated by synchrotron emission. The distribution of spectral index values between the 11?GHz and WMAP 23?GHz map peaks at [Beta] = -3.09 with a standard deviation of 0.14. The measured BB/EE ratio at scales of [L lower case+ = 80 is 0.26 ± 0.07 for a Galactic cut |b| > 10°. We find a positive TE correlation for 11?GHz at large angular scales ([L lower case+ [less than or equivalent to] 50), while the EB and TB signals are consistent with zero in the multipole range 30 [less than or equivalent to] [L lower case+ [less than or equivalent to] 150. The maps discussed in this paper are publicly available.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 finan- cial 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, PID2019-110610RB- C21, PID2020-120514GB-I00, IACA13-3E-2336, IACA15-BE- 3707, EQC2018-004918-P, the Severo Ochoa Programs SEV-2015- 0548 and CEX2019-000920-S, the Maria de Maeztu Program MDM- 2017-0765, 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 Framework Programme under grant agreement number 687312 (RADIOFOREGROUNDS). This research made use of computing time available on the high-performance computing systems at the IAC. We thankfully acknowledge the technical expertise and assistance provided by the Spanish Supercomputing Network (Red Espa ˜ nola de Supercom- putaci ´on), as well as the computer resources used: the Deimos/Di v a Supercomputer, located at the IAC. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The PWV data used in the tests presented in Section 4 comes from the Iza ˜ na Atmospheric Observatory (IZO), and have been made available to us by the Iza ˜ na Atmospheric Research Center (AEMET). SEH and CD acknowledge support from the STFC Consolidated Grant (ST/P000649/1). FP acknowledges support from the Spanish State Research Agency (AEI) under grant number PID2019-105552RB- C43. DT acknowledges the support from the Chinese Academy of Sciences (CAS) President’s International Fellowship Initiative (PIFI) with Grant N. 2020PM0042. 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 acknowl- edge the use of the Le gac y Archiv e for Microwav e Background Data Analysis (LAMBDA). 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 (G ´orski et al. 2005 ) and HEALPY (Zonca et al. 2019 ) packages. We also use Numpy (Harris et al. 2020 ), Matplotlib (Hunter 2007 ), and the SKLEARN module (Pedregosa et al. 2011 ).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/10902/27714Monthly Notices of the Royal Astronomical Society, 2023, 519(3), 3383-3431reponame:UCrea Repositorio Abierto de la Universidad de Cantabriainstname:Universidad de Cantabria (UC)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:repositorio.unican.es:10902/277142026-06-02T12:39:31Z |
| score |
15,298079 |