QUBIC I: Overview and Science Program
- Autores
- Hamilton, J. Ch.; Mousset, L.; Battistelli, E.S.; De Bernardis, P.; Bigot Sazy, M. A.; Chanial, P.; Charlassier, R.; D'Alessandro, G.; De Petris, M.; Gamboa Lerena, Martín Miguel; Grandsire, L.; Landau, Susana Judith; Mandelli, S.; Marnieros, S.; Masi, S.; Mennella, A.; O'Sullivan, C.; Piat, M.; Ricciardi, G.; Scoccola, Claudia Graciela; Stolpovskiy, M.; Tartari, A.; Torchinsky, S. A.; Voisin, F.; Zannoni, M.; Ade, P.; Alberro, J. G.; Almela, Daniel Alejandro; Amico, G.; Arnaldi, L. H.
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The Q & U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines the advantages of interferometry in terms of control of instrumental systematic effects with those of bolometric detectors in terms of wide-band, background-limited sensitivity. The QUBIC synthesized beam has a frequency-dependent shape that results in the ability to produce maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). These features make QUBIC complementary to other instruments and makes it particularly well suited to characterize and remove Galactic foreground contamination. In this article, first of a series of eight, we give an overview of the QUBIC instrument design, the main results of the calibration campaign, and present the scientific program of QUBIC including not only the measurement of primordial B-modes, but also the measurement of Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration on the sky and assuming perfect foreground removal as well as stable atmospheric conditions from our site in Argentina, our simulations show that we can achieve a statistical sensitivity to the effective tensor-to-scalar ratio (including primordial and foreground B-modes) σ(r)=0.015.
Fil: Hamilton, J. Ch.. Université de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Mousset, L.. Université de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Battistelli, E.S.. Università di Roma; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: De Bernardis, P.. Università di Roma; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Bigot Sazy, M. A.. Université de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Chanial, P.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Charlassier, R.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: D'Alessandro, G.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: De Petris, M.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Gamboa Lerena, Martín Miguel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Grandsire, L.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Landau, Susana Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina
Fil: Mandelli, S.. Università degli Studi di Milano; Italia
Fil: Marnieros, S.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Masi, S.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Mennella, A.. Università degli Studi di Milano; Italia. Istituto Nazionale di Fisica Nucleare; Italia
Fil: O'Sullivan, C.. National University of Ireland Galway; Irlanda
Fil: Piat, M.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Ricciardi, G.. Università degli Studi di Milano; Italia
Fil: Scoccola, Claudia Graciela. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Stolpovskiy, M.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Tartari, A.. Istituto Nazionale di Fisica Nucleare; Italia
Fil: Torchinsky, S. A.. Universite de Paris; Francia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Voisin, F.. Universite de Paris; Francia
Fil: Zannoni, M.. Istituto Nazionale di Fisica Nucleare; Italia. Università di Milano; Italia
Fil: Ade, P.. Cardiff University; Reino Unido
Fil: Alberro, J. G.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Almela, Daniel Alejandro. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Parque Centenario. Instituto de Tecnología en Detección y Astropartículas. Comisión Nacional de Energía Atómica. Instituto de Tecnología en Detección y Astropartículas. Universidad Nacional de San Martín. Instituto de Tecnología en Detección y Astropartículas; Argentina
Fil: Amico, G.. Università degli Studi di Roma "La Sapienza"; Italia
Fil: Arnaldi, L. H.. Comisión Nacional de Energía Atómica. Gerencia del Área de Energía Nuclear. Instituto Balseiro; Argentina - Materia
-
CMBR EXPERIMENTS
CMBR THEORY
COSMOLOGICAL PARAMETERS FROM CMBR
GRAVITATIONAL WAVES AND CMBR POLARIZATION - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/165613
Ver los metadatos del registro completo
| id |
CONICETDig_f9e9cc5031d3476c6a4c111ca40a8669 |
|---|---|
| oai_identifier_str |
oai:ri.conicet.gov.ar:11336/165613 |
| network_acronym_str |
CONICETDig |
| repository_id_str |
3498 |
| network_name_str |
CONICET Digital (CONICET) |
| spelling |
QUBIC I: Overview and Science ProgramHamilton, J. Ch.Mousset, L.Battistelli, E.S.De Bernardis, P.Bigot Sazy, M. A.Chanial, P.Charlassier, R.D'Alessandro, G.De Petris, M.Gamboa Lerena, Martín MiguelGrandsire, L.Landau, Susana JudithMandelli, S.Marnieros, S.Masi, S.Mennella, A.O'Sullivan, C.Piat, M.Ricciardi, G.Scoccola, Claudia GracielaStolpovskiy, M.Tartari, A.Torchinsky, S. A.Voisin, F.Zannoni, M.Ade, P.Alberro, J. G.Almela, Daniel AlejandroAmico, G.Arnaldi, L. H.CMBR EXPERIMENTSCMBR THEORYCOSMOLOGICAL PARAMETERS FROM CMBRGRAVITATIONAL WAVES AND CMBR POLARIZATIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The Q & U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines the advantages of interferometry in terms of control of instrumental systematic effects with those of bolometric detectors in terms of wide-band, background-limited sensitivity. The QUBIC synthesized beam has a frequency-dependent shape that results in the ability to produce maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). These features make QUBIC complementary to other instruments and makes it particularly well suited to characterize and remove Galactic foreground contamination. In this article, first of a series of eight, we give an overview of the QUBIC instrument design, the main results of the calibration campaign, and present the scientific program of QUBIC including not only the measurement of primordial B-modes, but also the measurement of Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration on the sky and assuming perfect foreground removal as well as stable atmospheric conditions from our site in Argentina, our simulations show that we can achieve a statistical sensitivity to the effective tensor-to-scalar ratio (including primordial and foreground B-modes) σ(r)=0.015.Fil: Hamilton, J. Ch.. Université de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Mousset, L.. Université de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Battistelli, E.S.. Università di Roma; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: De Bernardis, P.. Università di Roma; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Bigot Sazy, M. A.. Université de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Chanial, P.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Charlassier, R.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: D'Alessandro, G.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: De Petris, M.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Gamboa Lerena, Martín Miguel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; ArgentinaFil: Grandsire, L.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Landau, Susana Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; ArgentinaFil: Mandelli, S.. Università degli Studi di Milano; ItaliaFil: Marnieros, S.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Masi, S.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Mennella, A.. Università degli Studi di Milano; Italia. Istituto Nazionale di Fisica Nucleare; ItaliaFil: O'Sullivan, C.. National University of Ireland Galway; IrlandaFil: Piat, M.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Ricciardi, G.. Università degli Studi di Milano; ItaliaFil: Scoccola, Claudia Graciela. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; ArgentinaFil: Stolpovskiy, M.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Tartari, A.. Istituto Nazionale di Fisica Nucleare; ItaliaFil: Torchinsky, S. A.. Universite de Paris; Francia. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Voisin, F.. Universite de Paris; FranciaFil: Zannoni, M.. Istituto Nazionale di Fisica Nucleare; Italia. Università di Milano; ItaliaFil: Ade, P.. Cardiff University; Reino UnidoFil: Alberro, J. G.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; FranciaFil: Almela, Daniel Alejandro. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Parque Centenario. Instituto de Tecnología en Detección y Astropartículas. Comisión Nacional de Energía Atómica. Instituto de Tecnología en Detección y Astropartículas. Universidad Nacional de San Martín. Instituto de Tecnología en Detección y Astropartículas; ArgentinaFil: Amico, G.. Università degli Studi di Roma "La Sapienza"; ItaliaFil: Arnaldi, L. H.. Comisión Nacional de Energía Atómica. Gerencia del Área de Energía Nuclear. Instituto Balseiro; ArgentinaIOP Publishing2021-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/165613Hamilton, J. Ch.; Mousset, L.; Battistelli, E.S.; De Bernardis, P.; Bigot Sazy, M. A.; et al.; QUBIC I: Overview and Science Program; IOP Publishing; Journal of Cosmology and Astroparticle Physics; 2022; 4; 10-2021; 1-371475-7516CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/pdf/2011.02213.pdfinfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.1088/1475-7516/2022/04/034info:eu-repo/semantics/altIdentifier/doi/10.1088/1475-7516/2022/04/034info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:05:44Zoai:ri.conicet.gov.ar:11336/165613instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:05:44.772CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
QUBIC I: Overview and Science Program |
| title |
QUBIC I: Overview and Science Program |
| spellingShingle |
QUBIC I: Overview and Science Program Hamilton, J. Ch. CMBR EXPERIMENTS CMBR THEORY COSMOLOGICAL PARAMETERS FROM CMBR GRAVITATIONAL WAVES AND CMBR POLARIZATION |
| title_short |
QUBIC I: Overview and Science Program |
| title_full |
QUBIC I: Overview and Science Program |
| title_fullStr |
QUBIC I: Overview and Science Program |
| title_full_unstemmed |
QUBIC I: Overview and Science Program |
| title_sort |
QUBIC I: Overview and Science Program |
| dc.creator.none.fl_str_mv |
Hamilton, J. Ch. Mousset, L. Battistelli, E.S. De Bernardis, P. Bigot Sazy, M. A. Chanial, P. Charlassier, R. D'Alessandro, G. De Petris, M. Gamboa Lerena, Martín Miguel Grandsire, L. Landau, Susana Judith Mandelli, S. Marnieros, S. Masi, S. Mennella, A. O'Sullivan, C. Piat, M. Ricciardi, G. Scoccola, Claudia Graciela Stolpovskiy, M. Tartari, A. Torchinsky, S. A. Voisin, F. Zannoni, M. Ade, P. Alberro, J. G. Almela, Daniel Alejandro Amico, G. Arnaldi, L. H. |
| author |
Hamilton, J. Ch. |
| author_facet |
Hamilton, J. Ch. Mousset, L. Battistelli, E.S. De Bernardis, P. Bigot Sazy, M. A. Chanial, P. Charlassier, R. D'Alessandro, G. De Petris, M. Gamboa Lerena, Martín Miguel Grandsire, L. Landau, Susana Judith Mandelli, S. Marnieros, S. Masi, S. Mennella, A. O'Sullivan, C. Piat, M. Ricciardi, G. Scoccola, Claudia Graciela Stolpovskiy, M. Tartari, A. Torchinsky, S. A. Voisin, F. Zannoni, M. Ade, P. Alberro, J. G. Almela, Daniel Alejandro Amico, G. Arnaldi, L. H. |
| author_role |
author |
| author2 |
Mousset, L. Battistelli, E.S. De Bernardis, P. Bigot Sazy, M. A. Chanial, P. Charlassier, R. D'Alessandro, G. De Petris, M. Gamboa Lerena, Martín Miguel Grandsire, L. Landau, Susana Judith Mandelli, S. Marnieros, S. Masi, S. Mennella, A. O'Sullivan, C. Piat, M. Ricciardi, G. Scoccola, Claudia Graciela Stolpovskiy, M. Tartari, A. Torchinsky, S. A. Voisin, F. Zannoni, M. Ade, P. Alberro, J. G. Almela, Daniel Alejandro Amico, G. Arnaldi, L. H. |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
CMBR EXPERIMENTS CMBR THEORY COSMOLOGICAL PARAMETERS FROM CMBR GRAVITATIONAL WAVES AND CMBR POLARIZATION |
| topic |
CMBR EXPERIMENTS CMBR THEORY COSMOLOGICAL PARAMETERS FROM CMBR GRAVITATIONAL WAVES AND CMBR POLARIZATION |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
The Q & U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines the advantages of interferometry in terms of control of instrumental systematic effects with those of bolometric detectors in terms of wide-band, background-limited sensitivity. The QUBIC synthesized beam has a frequency-dependent shape that results in the ability to produce maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). These features make QUBIC complementary to other instruments and makes it particularly well suited to characterize and remove Galactic foreground contamination. In this article, first of a series of eight, we give an overview of the QUBIC instrument design, the main results of the calibration campaign, and present the scientific program of QUBIC including not only the measurement of primordial B-modes, but also the measurement of Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration on the sky and assuming perfect foreground removal as well as stable atmospheric conditions from our site in Argentina, our simulations show that we can achieve a statistical sensitivity to the effective tensor-to-scalar ratio (including primordial and foreground B-modes) σ(r)=0.015. Fil: Hamilton, J. Ch.. Université de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Mousset, L.. Université de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Battistelli, E.S.. Università di Roma; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: De Bernardis, P.. Università di Roma; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: Bigot Sazy, M. A.. Université de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Chanial, P.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Charlassier, R.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: D'Alessandro, G.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: De Petris, M.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: Gamboa Lerena, Martín Miguel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina Fil: Grandsire, L.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Landau, Susana Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina Fil: Mandelli, S.. Università degli Studi di Milano; Italia Fil: Marnieros, S.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Masi, S.. Università degli Studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: Mennella, A.. Università degli Studi di Milano; Italia. Istituto Nazionale di Fisica Nucleare; Italia Fil: O'Sullivan, C.. National University of Ireland Galway; Irlanda Fil: Piat, M.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Ricciardi, G.. Università degli Studi di Milano; Italia Fil: Scoccola, Claudia Graciela. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina Fil: Stolpovskiy, M.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Tartari, A.. Istituto Nazionale di Fisica Nucleare; Italia Fil: Torchinsky, S. A.. Universite de Paris; Francia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Voisin, F.. Universite de Paris; Francia Fil: Zannoni, M.. Istituto Nazionale di Fisica Nucleare; Italia. Università di Milano; Italia Fil: Ade, P.. Cardiff University; Reino Unido Fil: Alberro, J. G.. Universite de Paris; Francia. Centre National de la Recherche Scientifique; Francia Fil: Almela, Daniel Alejandro. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Parque Centenario. Instituto de Tecnología en Detección y Astropartículas. Comisión Nacional de Energía Atómica. Instituto de Tecnología en Detección y Astropartículas. Universidad Nacional de San Martín. Instituto de Tecnología en Detección y Astropartículas; Argentina Fil: Amico, G.. Università degli Studi di Roma "La Sapienza"; Italia Fil: Arnaldi, L. H.. Comisión Nacional de Energía Atómica. Gerencia del Área de Energía Nuclear. Instituto Balseiro; Argentina |
| description |
The Q & U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines the advantages of interferometry in terms of control of instrumental systematic effects with those of bolometric detectors in terms of wide-band, background-limited sensitivity. The QUBIC synthesized beam has a frequency-dependent shape that results in the ability to produce maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). These features make QUBIC complementary to other instruments and makes it particularly well suited to characterize and remove Galactic foreground contamination. In this article, first of a series of eight, we give an overview of the QUBIC instrument design, the main results of the calibration campaign, and present the scientific program of QUBIC including not only the measurement of primordial B-modes, but also the measurement of Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration on the sky and assuming perfect foreground removal as well as stable atmospheric conditions from our site in Argentina, our simulations show that we can achieve a statistical sensitivity to the effective tensor-to-scalar ratio (including primordial and foreground B-modes) σ(r)=0.015. |
| publishDate |
2021 |
| dc.date.none.fl_str_mv |
2021-10 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
| format |
article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/165613 Hamilton, J. Ch.; Mousset, L.; Battistelli, E.S.; De Bernardis, P.; Bigot Sazy, M. A.; et al.; QUBIC I: Overview and Science Program; IOP Publishing; Journal of Cosmology and Astroparticle Physics; 2022; 4; 10-2021; 1-37 1475-7516 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/165613 |
| identifier_str_mv |
Hamilton, J. Ch.; Mousset, L.; Battistelli, E.S.; De Bernardis, P.; Bigot Sazy, M. A.; et al.; QUBIC I: Overview and Science Program; IOP Publishing; Journal of Cosmology and Astroparticle Physics; 2022; 4; 10-2021; 1-37 1475-7516 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/pdf/2011.02213.pdf info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.1088/1475-7516/2022/04/034 info:eu-repo/semantics/altIdentifier/doi/10.1088/1475-7516/2022/04/034 |
| dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
| eu_rights_str_mv |
openAccess |
| rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
| dc.format.none.fl_str_mv |
application/pdf application/pdf |
| dc.publisher.none.fl_str_mv |
IOP Publishing |
| publisher.none.fl_str_mv |
IOP Publishing |
| dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
| reponame_str |
CONICET Digital (CONICET) |
| collection |
CONICET Digital (CONICET) |
| instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
| repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
| repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
| _version_ |
1846083200017760256 |
| score |
13.22299 |