Planck early results. II. The thermal performance of Planck
The performance of the Planck instruments in space is enabled by their low operating temperatures, 20 K for LFI and 0.1 K for HFI, achieved through a combination of passive radiative cooling and three active mechanical coolers. The scientific requirement for very broad frequency coverage led to two...
| Autores: | , , , , , , , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2011 |
| País: | España |
| Institución: | Universidad de Cantabria (UC) |
| Repositorio: | UCrea Repositorio Abierto de la Universidad de Cantabria |
| Idioma: | inglés |
| OAI Identifier: | oai:repositorio.unican.es:10902/28452 |
| Acceso en línea: | https://hdl.handle.net/10902/28452 |
| Access Level: | acceso abierto |
| Palabra clave: | Cosmic background radiation Space vehicles: instruments Instrumentation: detectors |
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| dc.title.none.fl_str_mv |
Planck early results. II. The thermal performance of Planck |
| title |
Planck early results. II. The thermal performance of Planck |
| spellingShingle |
Planck early results. II. The thermal performance of Planck Ade, Peter Anthony Robert Cosmic background radiation Space vehicles: instruments Instrumentation: detectors |
| title_short |
Planck early results. II. The thermal performance of Planck |
| title_full |
Planck early results. II. The thermal performance of Planck |
| title_fullStr |
Planck early results. II. The thermal performance of Planck |
| title_full_unstemmed |
Planck early results. II. The thermal performance of Planck |
| title_sort |
Planck early results. II. The thermal performance of Planck |
| dc.creator.none.fl_str_mv |
Ade, Peter Anthony Robert Aghanim, Nabila Arnaud, M. Ashdown, Mark Aumont, J. Baccigalupi, C. Baker, M. Balbi, A. Banday, A. J. Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Battaner, E. Benabed, K. Benoît, A. Bernard, J.-P. Bersanelli, M. Bhandari, P. Herranz Muñoz, Diego|||0000-0003-4540-1417 López-Caniego Alcarria, Marcos Martínez González, Enrique Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author |
Ade, Peter Anthony Robert |
| author_facet |
Ade, Peter Anthony Robert Aghanim, Nabila Arnaud, M. Ashdown, Mark Aumont, J. Baccigalupi, C. Baker, M. Balbi, A. Banday, A. J. Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Battaner, E. Benabed, K. Benoît, A. Bernard, J.-P. Bersanelli, M. Bhandari, P. Herranz Muñoz, Diego|||0000-0003-4540-1417 López-Caniego Alcarria, Marcos Martínez González, Enrique Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author_role |
author |
| author2 |
Aghanim, Nabila Arnaud, M. Ashdown, Mark Aumont, J. Baccigalupi, C. Baker, M. Balbi, A. Banday, A. J. Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Battaner, E. Benabed, K. Benoît, A. Bernard, J.-P. Bersanelli, M. Bhandari, P. Herranz Muñoz, Diego|||0000-0003-4540-1417 López-Caniego Alcarria, Marcos Martínez González, Enrique Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author2_role |
author author author author author 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 |
Cosmic background radiation Space vehicles: instruments Instrumentation: detectors |
| topic |
Cosmic background radiation Space vehicles: instruments Instrumentation: detectors |
| description |
The performance of the Planck instruments in space is enabled by their low operating temperatures, 20 K for LFI and 0.1 K for HFI, achieved through a combination of passive radiative cooling and three active mechanical coolers. The scientific requirement for very broad frequency coverage led to two detector technologies with widely different temperature and cooling needs. Active coolers could satisfy these needs; a helium cryostat, as used by previous cryogenic space missions (IRAS, COBE, ISO, Spitzer, AKARI), could not. Radiative cooling is provided by three V-groove radiators and a large telescope baffle. The active coolers are a hydrogen sorption cooler (<20 K), a 4He Joule-Thomson cooler (4.7 K), and a 3He-4He dilution cooler (1.4 K and 0.1 K). The flight system was at ambient temperature at launch and cooled in space to operating conditions. The HFI bolometer plate reached 93 mK on 3 July 2009, 50 days after launch. The solar panel always faces the Sun, shadowing the rest of Planck, and operates at a mean temperature of 384 K. At the other end of the spacecraft, the telescope baffle operates at 42.3 K and the telescope primary mirror operates at 35.9 K. The temperatures of key parts of the instruments are stabilized by both active and passive methods. Temperature fluctuations are driven by changes in the distance from the Sun, sorption cooler cycling and fluctuations in gas-liquid flow, and fluctuations in cosmic ray flux on the dilution and bolometer plates. These fluctuations do not compromise the science data. |
| publishDate |
2011 |
| dc.date.none.fl_str_mv |
2011 2011-12-01 |
| 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 |
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article |
| dc.identifier.none.fl_str_mv |
https://hdl.handle.net/10902/28452 |
| url |
https://hdl.handle.net/10902/28452 |
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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 |
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info:eu-repo/semantics/openAccess |
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open access http://purl.org/coar/access_right/c_abf2 |
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openAccess |
| dc.publisher.none.fl_str_mv |
EDP Sciences |
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EDP Sciences |
| dc.source.none.fl_str_mv |
Astronomy and Astrophysics, 2011, 536, A2 reponame:UCrea Repositorio Abierto de la Universidad de Cantabria instname:Universidad de Cantabria (UC) |
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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_ |
1869417326269431808 |
| spelling |
Planck early results. II. The thermal performance of PlanckAde, Peter Anthony RobertAghanim, NabilaArnaud, M.Ashdown, MarkAumont, J.Baccigalupi, C.Baker, M.Balbi, A.Banday, A. J.Barreiro Vilas, Rita Belén|||0000-0002-6139-4272Battaner, E.Benabed, K.Benoît, A.Bernard, J.-P.Bersanelli, M.Bhandari, P.Herranz Muñoz, Diego|||0000-0003-4540-1417López-Caniego Alcarria, MarcosMartínez González, EnriqueVielva Martínez, Patricio|||0000-0003-0051-272XCosmic background radiationSpace vehicles: instrumentsInstrumentation: detectorsThe performance of the Planck instruments in space is enabled by their low operating temperatures, 20 K for LFI and 0.1 K for HFI, achieved through a combination of passive radiative cooling and three active mechanical coolers. The scientific requirement for very broad frequency coverage led to two detector technologies with widely different temperature and cooling needs. Active coolers could satisfy these needs; a helium cryostat, as used by previous cryogenic space missions (IRAS, COBE, ISO, Spitzer, AKARI), could not. Radiative cooling is provided by three V-groove radiators and a large telescope baffle. The active coolers are a hydrogen sorption cooler (<20 K), a 4He Joule-Thomson cooler (4.7 K), and a 3He-4He dilution cooler (1.4 K and 0.1 K). The flight system was at ambient temperature at launch and cooled in space to operating conditions. The HFI bolometer plate reached 93 mK on 3 July 2009, 50 days after launch. The solar panel always faces the Sun, shadowing the rest of Planck, and operates at a mean temperature of 384 K. At the other end of the spacecraft, the telescope baffle operates at 42.3 K and the telescope primary mirror operates at 35.9 K. The temperatures of key parts of the instruments are stabilized by both active and passive methods. Temperature fluctuations are driven by changes in the distance from the Sun, sorption cooler cycling and fluctuations in gas-liquid flow, and fluctuations in cosmic ray flux on the dilution and bolometer plates. These fluctuations do not compromise the science data.Planck is too large a project to allow full acknowledgement of all contributions by individuals, institutions, industries, and funding agencies. The main entities involved in the mission operations are as follows. The European Space Agency operates the satellite via its Mission Operations Centre located at ESOC (Darmstadt, Germany) and coordinates scientific operations via the Planck Science Office located at ESAC (Madrid, Spain). Two Consortia, comprising around 50 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed the scientific instruments LFI and HFI, and continue to operate them via Instrument Operations Teams located in Trieste (Italy) and Orsay (France). The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J.-L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA’s US Planck Project, based at JPL and involving scientists at many US institutions, contributes significantly to the efforts of these two Consortia. 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.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaboration). 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, MICINN and JA (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); and DEISA (EU). We acknowledge the use of thermal models from Thales for the payload, IAS for the HFI, JPL for the sorption cooler, and Laben for the LFI. Some of the results in this paper have been derived using the HEALPix package (Górski et al. 2005). The HFI team wishes to thank warmly the Herschel-Planck project team under the leadership of Thomas Passvogel for their time, effort, and competence in solving the crises following failures of several parts of the cyrochain during Planck system tests. We acknowledge very useful discussions on the thermal behaviour of Planck during the system tests from the CSL team, who went far beyond their formal responsibilities.EDP SciencesUniversidad de Cantabria20112011-12-01journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articlehttps://hdl.handle.net/10902/28452Astronomy and Astrophysics, 2011, 536, A2reponame: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:10902/284522026-06-02T12:39:31Z |
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15,300724 |