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2 results on '"Fernandez-Cobos, Raul"'

1. Astro2020 APC White Paper: The need for better tools to design future CMB experiments

Author

Rocha, G., Banday, A.J., Barreiro, R. Belen, Challinor, Anthony, Górski, Krzysztof M., Hensley, Brandon, Jaffe, Tess, Jewell, Jeff, Keating, Brian, Kogut, Alan, Lawrence, Charles, Panopoulou, Georgia, Partridge, Bruce, Pearson, Tim, Silk, Joe, Steinhardt, Paul, Wehus, Ingunn, Bock, Jamie, Crill, Brendan, Delabrouille, Jacques, Doré, Olivier, Fernandez-Cobos, Raul, Ijjas, Anna, Keskitalo, Reijo, Kritsuk, Alexei, Mangilli, Anna, Moncelsi, Lorenzo, Myers, Steve, Steinbach, Bryan, Tristram, Matthieu, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This white paper addresses key challenges for the design of next-decade Cosmic Microwave Background (CMB) experiments, and for assessing their capability to extract cosmological information from CMB polarization. We focus here on the challenges posed by foreground emission, CMB lensing, and instrumental systematics to detect the signal that arises from gravitational waves sourced by inflation and parameterized by $r$, at the level of $r \sim 10^{-3}$ or lower, as proposed for future observational efforts. We argue that more accurate and robust analysis and simulation tools are required for these experiments to realize their promise. We are optimistic that the capability to simulate the joint impact of foregrounds, CMB lensing, and systematics can be developed to the level necessary to support the design of a space mission at $r \sim 10^{-4}$ in a few years. We make the case here for supporting such work. Although ground-based efforts present additional challenges (e.g., atmosphere, ground pickup), which are not addressed here, they would also benefit from these improved simulation capabilities., Comment: 10 pages + references, 4 figures; Submitted to the Astro2020 call for APC white papers

Published
2019

2. Exploring cosmic origins with CORE: Gravitational lensing of the CMB

Author

Challinor , Anthony, Allison , Rupert, Carron , Julien, Errard , Josquin, Feeney , Stephen, Kitching , Thomas, Lesgourgues , Julien, Lewis , Antony, Zubeldía , Íñigo, Achucarro , Ana, Ade , Peter, Ashdown , Mark, Ballardini , Mario, Banday , A.J., Banerji , Ranajoy, Bartlett , James, Bartolo , Nicola, Basak , Soumen, Baumann , Daniel, Bersanelli , Marco, Bonaldi , Anna, Bonato , Matteo, Borrill , Julian, Bouchet , François, Boulanger , François, Brinckmann , Thejs, Bucher , Martin, Burigana , Carlo, Buzzelli , Alessandro, Cai , Zhen-Yi, Calvo , Martino, Carvalho , Carla-Sofia, Castellano , Gabriella, Chluba , Jens, Clesse , Sebastien, Colantoni , Ivan, Coppolecchia , Alessandro, Crook , Martin, D'Alessandro , Giuseppe, De Bernardis , Paolo, De Gasperis , Giancarlo, De Zotti , Gianfranco, Delabrouille , Jacques, Di Valentino , Eleonora, Diego , Jose-Maria, Fernandez-Cobos , Raul, Ferraro , Simone, Finelli , Fabio, Forastieri , Francesco, Galli , Silvia, Genova-Santos , Ricardo, Gerbino , Martina, González-Nuevo , Joaquin, Grandis , Sebastian, Greenslade , Joshua, Hagstotz , Steffen, Hanany , Shaul, Handley , Will, Hernandez-Monteagudo , Carlos, Hervías-Caimapo , Carlos, Hills , Matthew, Luzzi , Gemma, Maffei , Bruno, Martinez-González , Enrique, Martins , C.J.A.P., Masi , Silvia, McCarthy , Darragh, Melchiorri , Alessandro, Melin , Jean-Baptiste, Molinari , Diego, Monfardini , Alessandro, Natoli , Paolo, Negrello , Mattia, Notari , Alessio, Paiella , Alessandro, Paoletti , Daniela, Patanchon , Guillaume, Piat , Michel, Pisano , Giampaolo, Polastri , Linda, Polenta , Gianluca, Pollo , Agnieszka, Poulin , Vivian, Quartin , Miguel, Remazeilles , Mathieu, Roman , Matthieu, Rubino-Martin , Jose-Alberto, Salvati , Laura, Tartari , Andrea, Tomasi , Maurizio, Tramonte , Denis, Trappe , Neil, Trombetti , Tiziana, Tucker , Carole, Valiviita , Jussi, Van De Weijgaert , Rien, Van Tent , Bartjan, Vennin , Vincent, Vielva , Patricio, Vittorio , Nicola, Young , Karl, Zannoni , Mario, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Lagrange de Paris, Sorbonne Universités, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), and CORE

Subjects
noise, deflection, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], B-mode: lens, gravitational radiation: primordial, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, redshift, calibration, estimator, gravitation: lens, non-Gaussianity, galaxy: cluster, neutrino: oscillation, neutrino: mass, gravitational radiation: power spectrum, halo: mass
Abstract

International audience; Lensing of the cosmic microwave background (CMB) is now a well-developed probe of the clustering of the large-scale mass distribution over a broad range of redshifts. By exploiting the non-Gaussian imprints of lensing in the polarization of the CMB, the CORE mission will allow production of a clean map of the lensing deflections over nearly the full-sky. The number of high-S/N modes in this map will exceed current CMB lensing maps by a factor of 40, and the measurement will be sample-variance limited on all scales where linear theory is valid. Here, we summarise this mission product and discuss the science that will follow from its power spectrum and the cross-correlation with other clustering data. For example, the summed mass of neutrinos will be determined to an accuracy of 17 meV combining CORE lensing and CMB two-point information with contemporaneous measurements of the baryon acoustic oscillation feature in the clustering of galaxies, three times smaller than the minimum total mass allowed by neutrino oscillation measurements. Lensing has applications across many other science goals of CORE, including the search for B-mode polarization from primordial gravitational waves. Here, lens-induced B-modes will dominate over instrument noise, limiting constraints on the power spectrum amplitude of primordial gravitational waves. With lensing reconstructed by CORE, one can "delens" the observed polarization internally, reducing the lensing B-mode power by 60 %. This can be improved to 70 % by combining lensing and measurements of the cosmic infrared background from CORE, leading to an improvement of a factor of 2.5 in the error on the amplitude of primordial gravitational waves compared to no delensing (in the null hypothesis of no primordial B-modes). Lensing measurements from CORE will allow calibration of the halo masses of the tens of thousands of galaxy clusters that it will find, with constraints dominated by the clean polarization-based estimators. The 19 frequency channels proposed for CORE will allow accurate removal of Galactic emission from CMB maps. We present initial findings that show that residual Galactic foreground contamination will not be a significant source of bias for lensing power spectrum measurements with CORE.

Published
2018

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