Planck intermediate results: LVII. Joint Planck LFI and HFI data processing
We present the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LFI) and High Frequency Instrument (HFI) using high-performance computers. NPIPE represents a natural evolution of previous Planck an...
| Autores: | , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2020 |
| País: | España |
| Institución: | Universidad de Cantabria (UC) |
| Repositorio: | UCrea Repositorio Abierto de la Universidad de Cantabria |
| Idioma: | inglés |
| OAI Identifier: | oai:repositorio.unican.es:10902/24980 |
| Acceso en línea: | http://hdl.handle.net/10902/24980 |
| Access Level: | acceso abierto |
| Palabra clave: | Cosmic background radiation Cosmology: observations Cosmological parameters Galaxy: general Methods: data analysis |
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oai:repositorio.unican.es:10902/24980 |
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España |
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| dc.title.none.fl_str_mv |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processing |
| title |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processing |
| spellingShingle |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processing Akrami, Y. Cosmic background radiation Cosmology: observations Cosmological parameters Galaxy: general Methods: data analysis |
| title_short |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processing |
| title_full |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processing |
| title_fullStr |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processing |
| title_full_unstemmed |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processing |
| title_sort |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processing |
| dc.creator.none.fl_str_mv |
Akrami, Y. Casaponsa Galí, Biuse Diego Rodríguez, José María|||0000-0001-9065-3926 Fernández Cobos, Raúl|||0000-0001-6185-7903 Herranz Muñoz, Diego|||0000-0003-4540-1417 Marcos Caballero, Airam Eduardo Martínez González, Enrique Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author |
Akrami, Y. |
| author_facet |
Akrami, Y. Casaponsa Galí, Biuse Diego Rodríguez, José María|||0000-0001-9065-3926 Fernández Cobos, Raúl|||0000-0001-6185-7903 Herranz Muñoz, Diego|||0000-0003-4540-1417 Marcos Caballero, Airam Eduardo Martínez González, Enrique Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author_role |
author |
| author2 |
Casaponsa Galí, Biuse Diego Rodríguez, José María|||0000-0001-9065-3926 Fernández Cobos, Raúl|||0000-0001-6185-7903 Herranz Muñoz, Diego|||0000-0003-4540-1417 Marcos Caballero, Airam Eduardo Martínez González, Enrique Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author2_role |
author author author author author author author |
| dc.contributor.none.fl_str_mv |
Universidad de Cantabria |
| dc.subject.none.fl_str_mv |
Cosmic background radiation Cosmology: observations Cosmological parameters Galaxy: general Methods: data analysis |
| topic |
Cosmic background radiation Cosmology: observations Cosmological parameters Galaxy: general Methods: data analysis |
| description |
We present the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LFI) and High Frequency Instrument (HFI) using high-performance computers. NPIPE represents a natural evolution of previous Planck analysis efforts, and combines some of the most powerful features of the separate LFI and HFI analysis pipelines. For example, following the LFI 2018 processing procedure, NPIPE uses foreground polarization priors during the calibration stage in order to break scanning-induced degeneracies. Similarly, NPIPE employs the HFI 2018 time-domain processing methodology to correct for bandpass mismatch at all frequencies. In addition, NPIPE introduces several improvements, including, but not limited to: inclusion of the 8% of data collected during repointing manoeuvres; smoothing of the LFI reference load data streams; in-flight estimation of detector polarization parameters; and construction of maximally independent detector-set split maps. For component-separation purposes, important improvements include: maps that retain the CMB Solar dipole, allowing for high-precision relative calibration in higher-level analyses; well-defined single-detector maps, allowing for robust CO extraction; and HFI temperature maps between 217 and 857 GHz that are binned into 0?.9 pixels (Nside = 4096), ensuring that the full angular information in the data is represented in the maps even at the highest Planck resolutions. The net effect of these improvements is lower levels of noise and systematics in both frequency and component maps at essentially all angular scales, as well as notably improved internal consistency between the various frequency channels. Based on the NPIPE maps, we present the first estimate of the Solar dipole determined through component separation across all nine Planck frequencies. The amplitude is (3366.6?±?2.7) ?K, consistent with, albeit slightly higher than, earlier estimates. From the large-scale polarization data, we derive an updated estimate of the optical depth of reionization of ??=?0.051?±?0.006, which appears robust with respect to data and sky cuts. There are 600 complete signal, noise and systematics simulations of the full-frequency and detector-set maps. As a Planck first, these simulations include full time-domain processing of the beam-convolved CMB anisotropies. The release of NPIPE maps and simulations is accompanied with a complete suite of raw and processed time-ordered data and the software, scripts, auxiliary data, and parameter files needed to improve further on the analysis and to run matching simulations. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020 2020-01-01 |
| 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/10902/24980 |
| url |
http://hdl.handle.net/10902/24980 |
| 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 |
EDP Sciences |
| publisher.none.fl_str_mv |
EDP Sciences |
| dc.source.none.fl_str_mv |
Astronomy & Astrophysics. Vol. 643, Nov. 2020. A42 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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|
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|
| _version_ |
1869411831307567104 |
| spelling |
Planck intermediate results: LVII. Joint Planck LFI and HFI data processingAkrami, Y.Casaponsa Galí, BiuseDiego Rodríguez, José María|||0000-0001-9065-3926Fernández Cobos, Raúl|||0000-0001-6185-7903Herranz Muñoz, Diego|||0000-0003-4540-1417Marcos Caballero, Airam EduardoMartínez González, EnriqueVielva Martínez, Patricio|||0000-0003-0051-272XCosmic background radiationCosmology: observationsCosmological parametersGalaxy: generalMethods: data analysisWe present the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LFI) and High Frequency Instrument (HFI) using high-performance computers. NPIPE represents a natural evolution of previous Planck analysis efforts, and combines some of the most powerful features of the separate LFI and HFI analysis pipelines. For example, following the LFI 2018 processing procedure, NPIPE uses foreground polarization priors during the calibration stage in order to break scanning-induced degeneracies. Similarly, NPIPE employs the HFI 2018 time-domain processing methodology to correct for bandpass mismatch at all frequencies. In addition, NPIPE introduces several improvements, including, but not limited to: inclusion of the 8% of data collected during repointing manoeuvres; smoothing of the LFI reference load data streams; in-flight estimation of detector polarization parameters; and construction of maximally independent detector-set split maps. For component-separation purposes, important improvements include: maps that retain the CMB Solar dipole, allowing for high-precision relative calibration in higher-level analyses; well-defined single-detector maps, allowing for robust CO extraction; and HFI temperature maps between 217 and 857 GHz that are binned into 0?.9 pixels (Nside = 4096), ensuring that the full angular information in the data is represented in the maps even at the highest Planck resolutions. The net effect of these improvements is lower levels of noise and systematics in both frequency and component maps at essentially all angular scales, as well as notably improved internal consistency between the various frequency channels. Based on the NPIPE maps, we present the first estimate of the Solar dipole determined through component separation across all nine Planck frequencies. The amplitude is (3366.6?±?2.7) ?K, consistent with, albeit slightly higher than, earlier estimates. From the large-scale polarization data, we derive an updated estimate of the optical depth of reionization of ??=?0.051?±?0.006, which appears robust with respect to data and sky cuts. There are 600 complete signal, noise and systematics simulations of the full-frequency and detector-set maps. As a Planck first, these simulations include full time-domain processing of the beam-convolved CMB anisotropies. The release of NPIPE maps and simulations is accompanied with a complete suite of raw and processed time-ordered data and the software, scripts, auxiliary data, and parameter files needed to improve further on the analysis and to run matching simulations.The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This work has received funding from the European Union’s Horizon 2020 research and innovation programme under grant numbers 776282, 772253 and 819478. This research would not have been possible without the resources of the National Energy Research Scientific Computing Center (NERSC), a US Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231.EDP SciencesUniversidad de Cantabria20202020-01-01journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articlehttp://hdl.handle.net/10902/24980Astronomy & Astrophysics. Vol. 643, Nov. 2020. A42reponame: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:10902/249802026-06-02T12:39:31Z |
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15,300724 |