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arXiv 2024年

作者： Evans, Matthew L. Bergsma, Johan Merkys, Andrius Andersen, Casper W. Andersson, Oskar B. Beltrán, Daniel Blokhin, Evgeny Boland, Tara M. Balderas, Rubén Castañeda Choudhary, Kamal Díaz, Alberto Díaz García, Rodrigo Domínguez Eckert, Hagen Eimre, Kristjan Montero, María Elena Fuentes Krajewski, Adam M. Mortensen, Jens Jørgen Duarte, José Manuel Nápoles Pietryga, Jacob Qi, Ji de Jesús Trejo Carrillo, Felipe Vaitkus, Antanas Yu, Jusong Zettel, Adam de Castro, Pedro Baptista Carlsson, Johan Cerqueira, Tiago F.T. Divilov, Simon Hajiyani, Hamidreza Hanke, Felix Jose, Kevin Oses, Corey Riebesell, Janosh Schmidt, Jonathan Winston, Donald Xie, Christen Yang, Xiaoyu Bonella, Sara Botti, Silvana Curtarolo, Stefano Draxl, Claudia Cobas, Luis Edmundo Fuentes Hospital, Adam Liu, Zi-Kui Marques, Miguel A.L. Marzari, Nicola Morris, Andrew J. Ong, Shyue Ping Orozco, Modesto Persson, Kristin A. Thygesen, Kristian S. Wolverton, Chris Scheidgen, Markus Toher, Cormac Conduit, Gareth J. Pizzi, Giovanni Gražulis, Saulius Rignanese, Gian-Marco Armiento, Rickard Chemin des Étoiles 8 Louvain-la-Neuve1348 Belgium Matgenix SRL 185 Rue Armand Bury Gozée6534 Belgium École Polytechnique Fédérale de Lausanne Avenue de Forel 3 Lausanne1015 Switzerland Institute of Biotechnology Life Sciences Center Vilnius University Sauletekio av. 7 VilniusLT-10257 Lithuania SINTEF P.O. Box 4760 Torgarden TrondheimNO-7465 Norway Materials Design and Informatics unit Department of Physics Chemistry and Biology Linköping University Sweden Baldiri i Reixac 10-12 Barcelona08028 Spain Tilde Materials Informatics Straßmannstraße 25 Berlin10249 Germany Materials Platform for Data Science Sepapaja 6 Tallinn15551 Estonia Computational Atomic-Scale Materials Design Technical University of Denmark Kgs. Lyngby Denmark Av. Miguel de Cervantes 120 Complejo Industrial Chihuahua Chihuahua Chih. 31136 Mexico Material Measurement Laboratory National Institute of Standards and Technology GaithersburgMD20899 United States Department of Mechanical Engineering and Materials Science Duke University DurhamNC27708 United States Center for Extreme Materials Duke University DurhamNC27708 United States École Polytechnique Fédérale de Lausanne Lausanne1015 Switzerland Universidad Autónoma de Chihuahua Facultad de Ciencias Quimicas Chihuahua31125 Mexico Department of Materials Science and Engineering The Pennsylvania State University University ParkPA16802 United States Department of Materials Science and Engineering Northwestern University EvanstonIL60208 United States Department of NanoEngineering University of California 9500 Gilman Drive La Jolla San DiegoCA92093-0448 United States National Institute for Materials Science 1-2-1 Sengen Ibaraki Tsukuba305-0047 Japan Dassault Systèmes Germany GmbH Am Kabellager 11-13 Cologne51063 Germany CFisUC Department of Physics University of Coimbra Rua Larga Coimbra3004-516 Portugal Dassault Systèmes 22 Science Park CB4 0FJ United Kingdom Theory of Condensed Matter Cavendis

The Open databases Integration for Materials Design (OPTIMADE) application programming interface (API) empowers users with holistic access to a growing federation of databases, enhancing the accessibility and discoverability of materials and chemical data. Since the first release of the OPTIMADE specification (v1.0), the API has undergone significant development, leading to the v1.2 release, and has underpinned multiple scientific studies. In this work, we highlight the latest features of the API format, accompanying software tools, and provide an update on the implementation of OPTIMADE in contributing materials databases. We end by providing several use cases that demonstrate the utility of the OPTIMADE API in materials research that continue to drive its ongoing development. © 2024, CC BY.

关键词： Electronic data interchange

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LiteBIRD Science Goals and Forecasts: Improving Sensitivity to Inflationary Gravitational Waves with Multitracer Delensing

arXiv

引用

arXiv 2023年

作者： Namikawa, T. Lonappan, A.I. Baccigalupi, C. Bartolo, N. Beck, D. Benabed, K. Challinor, A. Diego-Palazuelos, P. Errard, J. Farrens, S. Gruppuso, A. Krachmalnicoff, N. Migliaccio, M. Martínez-González, E. Pettorino, V. Piccirilli, G. Ruiz-Granda, M. Sherwin, B. Starck, J. Vielva, P. Akizawa, R. Anand, A. Aumont, J. Aurlien, R. Azzoni, S. Ballardini, M. Banday, A.J. Barreiro, R.B. Bersanelli, M. Blinov, D. Bortolami, M. Brinckmann, T. Calabrese, E. Campeti, P. Carones, A. Carralot, F. Casas, F.J. Cheung, K. Clermont, L. Columbro, F. Conenna, G. Coppolecchia, A. Cuttaia, F. D'Alessandro, G. de Bernardis, P. de Haan, T. De Petris, M. Torre, S. Della Di Giorgi, E. Eriksen, H.K. Finelli, F. Franceschet, C. Fuskeland, U. Galloni, G. Galloway, M. Georges, M. Gerbino, M. Gervasi, M. Ghigna, T. Giardiello, S. Gimeno-Amo, C. Gjerløw, E. Hazumi, M. Henrot-Versillé, S. Hergt, L.T. Hivon, E. Kohri, K. Komatsu, E. Lamagna, L. Lattanzi, M. Leloup, C. Lembo, M. López-Caniego, M. Luzzi, G. Maffei, B. Masi, S. Massa, M. Matarrese, S. Matsumura, T. Micheli, S. Moggi, A. Monelli, M. Montier, L. Morgante, G. Mot, B. Mousset, L. Nagata, R. Natoli, P. Novelli, A. Obata, I. Occhiuzzi, A. Pagano, L. Paiella, A. Paoletti, D. Pascual-Cisneros, G. Pavlidou, V. Piacentini, F. Pinchera, M. Pisano, G. Polenta, G. Puglisi, G. Remazeilles, M. Ritacco, A. Rizzieri, A. Rubino-Martin, J. Sakurai, Y. Scott, D. Shiraishi, M. Signorelli, G. Stever, S.L. Takase, Y. Tanimura, H. Tartari, A. Tassis, K. Terenzi, L. Tristram, M. Vacher, L. van Tent, B. Wehus, I.K. Weymann-Despres, G. Zannoni, M. Zhou, Y. UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Dipartimento di Fisica Università di Roma Tor Vergata Via della Ricerca Scientifica 1 Roma00133 Italy Via Bonomea 265 Trieste34136 Italy INFN Sezione di Trieste via Valerio 2 Trieste34127 Italy IFPU Via Beirut 2 Grignano Trieste34151 Italy Avenida los Castros SN Santander39005 Spain Dipartimento di Fisica e Astronomia "G. Galilei" Universita‘degli Studi di Padova via Marzolo 8 PadovaI-35131 Italy INFN Sezione di Padova via Marzolo 8 PadovaI-35131 Italy INAF Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Stanford University Department of Physics CA94305-4060 United States Institut d’Astrophysique de Paris CNRS Sorbonne Université Paris France DAMTP Centre for Mathematical Sciences Wilberforce Road CambridgeCB3 0WA United Kingdom Institute of Astronomy Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Dpto. de Física Moderna Universidad de Cantabria Avda. los Castros s/n SantanderE-39005 Spain Université de Paris CNRS Astroparticule et Cosmologie ParisF-75013 France AIM CEA CNRS Université Paris-Saclay Université de Paris Gif-sur-YvetteF-91191 France INAF - OAS Bologna via Piero Gobetti 93/3 Bologna40129 Italy INFN Sezione di Bologna Viale C. Berti Pichat 6/2 Bologna40127 Italy INFN Sezione di Roma2 Università di Roma Tor Vergata via della Ricerca Scientifica 1 Roma00133 Italy Physics Division BerkeleyCA94720 United States The University of Tokyo Department of Physics Tokyo113-0033 Japan IRAP Université de Toulouse CNRS CNES UPS Toulouse France Institute of Theoretical Astrophysics University of Oslo Blindern Oslo Norway Department of Astrophysical Sciences Peyton Hall Princeton University PrincetonNJ08544 United States Dipartimento di Fisica e Scienze della Terra Università di Ferrara Via Saragat 1 Ferrara44122

We estimate the efficiency of mitigating the lensing B-mode polarization, the so-called delensing, for the LiteBIRD experiment with multiple external data sets of lensing-mass tracers. The current best bound on the tensor-to-scalar ratio, r, is limited by lensing rather than Galactic foregrounds. Delensing will be a critical step to improve sensitivity to r as measurements of r become more and more limited by lensing. In this paper, we extend the analysis of the recent LiteBIRD forecast paper to include multiple mass tracers, i.e., the CMB lensing maps from LiteBIRD and CMB-S4-like experiment, cosmic infrared background, and galaxy number density from Euclid- and LSST-like survey. We find that multi-tracer delensing will further improve the constraint on r by about 20%. In LiteBIRD, the residual Galactic foregrounds also significantly contribute to uncertainties of the B-modes, and delensing becomes more important if the residual foregrounds are further reduced by an improved component separation method. © 2023, CC BY.

关键词： Cosmology

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LiteBIRD Science Goals and Forecasts: A full-sky measurement of gravitational lensing of the CMB

arXiv

引用

arXiv 2023年

作者： Lonappan, A.I. Namikawa, T. Piccirilli, G. Diego-Palazuelos, P. Ruiz-Granda, M. Migliaccio, M. Baccigalupi, C. Bartolo, N. Beck, D. Benabed, K. Challinor, A. Errard, J. Farrens, S. Gruppuso, A. Krachmalnicoff, N. Martínez-González, E. Pettorino, V. Sherwin, B. Starck, J. Vielva, P. Akizawa, R. Anand, A. Aumont, J. Aurlien, R. Azzoni, S. Ballardini, M. Banday, A.J. Barreiro, R.B. Bersanelli, M. Blinov, D. Bortolami, M. Brinckmann, T. Calabrese, E. Campeti, P. Carones, A. Carralot, F. Casas, F.J. Cheung, K. Clermont, L. Columbro, F. Conenna, G. Coppolecchia, A. Cuttaia, F. D'Alessandro, G. de Bernardis, P. De Petris, M. Torre, S. Della Di Giorgi, E. Eriksen, H.K. Finelli, F. Franceschet, C. Fuskeland, U. Galloni, G. Galloway, M. Georges, M. Gerbino, M. Gervasi, M. Génova-Santos, R.T. Ghigna, T. Giardiello, S. Gimeno-Amo, C. Gjerløw, E. Hazumi, M. Henrot-Versillé, S. Hergt, L.T. Hivon, E. Kohri, K. Komatsu, E. Lamagna, L. Lattanzi, M. Leloup, C. Lembo, M. López-Caniego, M. Luzzi, G. Macias-Perez, J. Maffei, B. Masi, S. Massa, M. Matarrese, S. Matsumura, T. Micheli, S. Moggi, A. Monelli, M. Montier, L. Morgante, G. Mot, B. Mousset, L. Nagata, R. Natoli, P. Novelli, A. Obata, I. Occhiuzzi, A. Pagano, L. Paiella, A. Paoletti, D. Pascual-Cisneros, G. Pavlidou, V. Piacentini, F. Pinchera, M. Pisano, G. Polenta, G. Puglisi, G. Remazeilles, M. Ritacco, A. Rizzieri, A. Sakurai, Y. Scott, D. Shiraishi, M. Signorelli, G. Stever, S.L. Takase, Y. Tanimura, H. Tartari, A. Tassis, K. Terenzi, L. Tristram, M. Vacher, L. van Tent, B. Wehus, I.K. Weymann-Despres, G. Zannoni, M. Zhou, Y. Dipartimento di Fisica Università di Roma Tor Vergata Via della Ricerca Scientifica 1 Roma00133 Italy UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Avenida los Castros SN Santander39005 Spain Dpto. de Física Moderna Universidad de Cantabria Avda. los Castros s/n SantanderE-39005 Spain INFN Sezione di Roma2 Università di Roma Tor Vergata via della Ricerca Scientifica 1 Roma00133 Italy Via Bonomea 265 Trieste34136 Italy INFN Sezione di Trieste via Valerio 2 Trieste34127 Italy IFPU Via Beirut 2 Grignano Trieste34151 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Universita‘degli Studi di Padova via Marzolo 8 PadovaI-35131 Italy INFN Sezione di Padova via Marzolo 8 PadovaI-35131 Italy INAF Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Stanford University Department of Physics CA94305-4060 United States Institut d’Astrophysique de Paris CNRS Sorbonne Université Paris France DAMTP Centre for Mathematical Sciences Wilberforce Road CambridgeCB3 0WA United Kingdom Institute of Astronomy Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Université de Paris CNRS Astroparticule et Cosmologie ParisF-75013 France AIM CEA CNRS Université Paris-Saclay Université de Paris Gif-sur-YvetteF-91191 France INAF - OAS Bologna via Piero Gobetti 93/3 Bologna40129 Italy INFN Sezione di Bologna Viale C. Berti Pichat 6/2 Bologna40127 Italy Physics Division BerkeleyCA94720 United States The University of Tokyo Department of Physics Tokyo113-0033 Japan IRAP Université de Toulouse CNRS CNES UPS Toulouse France Institute of Theoretical Astrophysics University of Oslo Blindern Oslo Norway Department of Astrophysical Sciences Peyton Hall Princeton University PrincetonNJ08544 United States Dipartimento di Fisica e Scienze della Terra Università di Ferrara Via Saragat 1 Ferrara44122

We explore the capability of measuring lensing signals in LiteBIRD full-sky polarization maps. With a 30 arcmin beam width and an impressively low polarization noise of 2.16 µK-arcmin, LiteBIRD will be able to measure the full-sky polarization of the cosmic microwave background (CMB) very precisely. This unique sensitivity also enables the reconstruction of a nearly full-sky lensing map using only polarization data, even considering its limited capability to capture small-scale CMB anisotropies. In this paper, we investigate the ability to construct a full-sky lensing measurement in the presence of Galactic foregrounds, finding that several possible biases from Galactic foregrounds should be negligible after component separation by harmonic-space internal linear combination. We find that the signal-to-noise ratio of the lensing is approximately 40 using only polarization data measured over 90% of the sky. This achievement is comparable to Planck’s recent lensing measurement with both temperature and polarization and represents a four-fold improvement over Planck’s polarization-only lensing measurement. The LiteBIRD lensing map will complement the Planck lensing map and provide several opportunities for cross-correlation science, especially in the northern hemisphere. Copyright © 2023, The Authors. All rights reserved.

关键词： Signal to noise ratio

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Common Limitations of Image processing Metrics: A Picture Story

arXiv

引用

arXiv 2021年

作者： Reinke, Annika Tizabi, Minu D. Sudre, Carole H. Eisenmann, Matthias Rädsch, Tim Baumgartner, Michael Acion, Laura Antonelli, Michela Arbel, Tal Bakas, Spyridon Bankhead, Peter Benis, Arriel Blaschko, Matthew Buettner, Florian Cardoso, M. Jorge Chen, Jianxu Cheplygina, Veronika Christodoulou, Evangelia Cimini, Beth A. Collins, Gary S. Engelhardt, Sandy Farahani, Keyvan Ferrer, Luciana Galdran, Adrian van Ginneken, Bram Glocker, Ben Godau, Patrick Haase, Robert Hamprecht, Fred Hashimoto, Daniel A. Heckmann-Nötzel, Doreen Hirsch, Peter Hoffman, Michael M. Huisman, Merel Isensee, Fabian Jannin, Pierre Kahn, Charles E. Kainmueller, Dagmar Kainz, Bernhard Karargyris, Alexandros Karthikesalingam, Alan Kavur, A. Emre Kenngott, Hannes Kleesiek, Jens Kleppe, Andreas Koehler, Sven Kofler, Florian Kopp-Schneider, Annette Kooi, Thijs Kozubek, Michal Kreshuk, Anna Kurc, Tahsin Landman, Bennett A. Litjens, Geert Madani, Amin Maier-Hein, Klaus Martel, Anne L. Mattson, Peter Meijering, Erik Menze, Bjoern Moher, David Moons, Karel G.M. Müller, Henning Nichyporuk, Brennan Nickel, Felix Noyan, M. Alican Petersen, Jens Polat, Gorkem Rafelski, Susanne M. Rajpoot, Nasir Reyes, Mauricio Rieke, Nicola Riegler, Michael A. Rivaz, Hassan Saez-Rodriguez, Julio Sánchez, Clara I. Schroeter, Julien Saha, Anindo Selver, M. Alper Sharan, Lalith Shetty, Shravya Smeden, Maarten V.A.N. Stieltjes, Bram Summers, Ronald M. Taha, Abdel A. Tiulpin, Aleksei Tsaftaris, Sotirios A. Calster, Ben V.A.N. Varoquaux, Gaël Wiesenfarth, Manuel Yaniv, Ziv R. Jäger, Paul Maier-Hein, Lena Division of Intelligent Medical Systems and HI Helmholtz Imaging Heidelberg Germany Faculty of Mathematics and Computer Science Heidelberg University Heidelberg Germany Division of Intelligent Medical Systems Heidelberg Germany NCT Heidelberg DKFZ University Medical Center Heidelberg Germany MRC Unit for Lifelong Health and Ageing UCL Centre for Medical Image Computing Department of Computer Science University College London London United Kingdom School of Biomedical Engineering and Imaging Science King’s College London London United Kingdom Division of Medical Image Computing Heidelberg Germany Instituto de Cálculo CONICET – Universidad de Buenos Aires Buenos Aires Argentina Centre for Medical Image Computing University College London London United Kingdom McGill University Montréal Canada Division of Computational Pathology Dept of Pathology & Laboratory Medicine Indiana University School of Medicine IU Health Information and Translational Sciences Building Indianapolis United States University of Pennsylvania Richards Medical Research Laboratories FL7 PhiladelphiaPA United States Institute of Genetics and Cancer University of Edinburgh Edinburgh United Kingdom Department of Digital Medical Technologies Holon Institute of Technology Holon Israel European Federation for Medical Informatics Le Mont-sur-Lausanne Switzerland Center for Processing Speech and Images Department of Electrical Engineering KU Leuven Kasteelpark Arenberg 10 - box 2441 Leuven3001 Belgium Frankfurt/Mainz DKFZ UCT Frankfurt-Marburg Germany Heidelberg Germany Goethe University Frankfurt Department of Medicine Germany Goethe University Frankfurt Department of Informatics Germany Frankfurt Cancer Insititute Germany Leibniz-Institut für Analytische Wissenschaften – ISAS – e.V. Dortmund Germany Department of Computer Science IT University of Copenhagen Copenhagen Denmark Imaging Platform Broad Institute of MIT and Harvard CambridgeMA United States Centre for St

While the importance of automatic image analysis is continuously increasing, recent meta-research revealed major flaws with respect to algorithm validation. Performance metrics are particularly key for meaningful, objective, and transparent performance assessment and validation of the used automatic algorithms, but relatively little attention has been given to the practical pitfalls when using specific metrics for a given image analysis task. These are typically related to (1) the disregard of inherent metric properties, such as the behaviour in the presence of class imbalance or small target structures, (2) the disregard of inherent data set properties, such as the non-independence of the test cases, and (3) the disregard of the actual biomedical domain interest that the metrics should reflect. This living dynamically document has the purpose to illustrate important limitations of performance metrics commonly applied in the field of image analysis. In this context, it focuses on biomedical image analysis problems that can be phrased as image-level classification, semantic segmentation, instance segmentation, or object detection task. The current version is based on a Delphi process on metrics conducted by an international consortium of image analysis experts from more than 60 institutions worldwide. © 2021, CC BY.

关键词： Medical imaging

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Planck 2018 results. XII. Galactic astrophysics using polarized dust emission

arXiv

引用

arXiv 2018年

作者： Aghanim, N. Akrami, Y. Alves, M.I.R. Ashdown, M. Aumont, J. Baccigalupi, C. Ballardini, M. Banday, A.J. Barreiro, R.B. Bartolo, N. Basak, S. Benabed, K. Bernard, J.-P. Bersanelli, M. Bielewicz, P. Bock, J.J. Bond, J.R. Borrill, J. Bouchet, F.R. Boulanger, F. Bracco, A. Bucher, M. Burigana, C. Calabrese, E. Cardoso, J.-F. Carron, J. Chary, R.-R. Chiang, H.C. Colombo, L.P.L. Combet, C. Crill, B.P. Cuttaia, F. de Bernardis, P. de Zotti, G. Delabrouille, J. Delouis, J.-M. Di Valentino, E. Dickinson, C. Diego, J.M. Doré, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Enßlin, T.A. Eriksen, H.K. Falgarone, E. Fantaye, Y. Fernandez-Cobos, R. Ferrière, K. Finelli, F. Forastieri, F. Frailis, M. Fraisse, A.A. Franceschi, E. Frolov, A. Galeotta, S. Galli, S. Ganga, K. Génova-Santos, R.T. Gerbino, M. Ghosh, T. González-Nuevo, J. Górski, K.M. Gratton, S. Green, G. Gruppuso, A. Gudmundsson, J.E. Guillet, V. Handley, W. Hansen, F.K. Helou, G. Herranz, D. Hivon, E. Huang, Z. Jaffe, A.H. Jones, W.C. Keihänen, E. Keskitalo, R. Kiiveri, K. Kim, J. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J.-M. Lasenby, A. Lattanzi, M. Lawrence, C.R. Le Jeune, M. Levrier, F. Liguori, M. Lilje, P.B. Lindholm, V. López-Caniego, M. Lubin, P.M. Ma, Y.-Z. Macías-Pérez, J.F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Marcos-Caballero, A. Maris, M. Martin, P.G. Martínez-González, E. Matarrese, S. Mauri, N. McEwen, J.D. Melchiorri, A. Mennella, A. Migliaccio, M. Miville-Deschênes, M.-A. Molinari, D. Moneti, A. Montier, L. Morgante, G. Moss, A. Natoli, P. Pagano, L. Paoletti, D. Patanchon, G. Perrotta, F. Pettorino, V. Piacentini, F. Polastri, L. Polenta, G. Puget, J.-L. Rachen, J.P. Reinecke, M. Remazeilles, M. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rubiño-Martín, J.A. Ruiz-Granados, B. Salvati, L. Sandri, M. Savelainen, M. Scott, D. Sirignano, C. AIM CEA CNRS Université Paris-Saclay Université Paris-Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France APC AstroParticule et Cosmologie Université Paris Diderot CNRS IN2P3 CEA Lrfu Observatoire de Paris Sorbonne Paris Cité 10 rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France African Institute for Mathematical Sciences 6-8 Melrose Road Muizenberg Cape Town South Africa Aix Marseille Univ CNRS CNES LAM Marseille France Astrophysics Group Cavendish Laboratory University of Cambridge J J Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Private Bag X54001 Durban4000 South Africa CITA University of Toronto 60 St. George St. TorontoONM5S 3H8 Canada CNRS IRAP 9 Av. colonel Roche BP 44346 Toulouse Cedex 4F-31028 France Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91125 United States California Institute of Technology PasadenaCA United States Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA United States Département de Physique Théorique Université de Genève 24 Quai E. Ansermet Genève 41211 Switzerland Département de Physique École Normale Supérieure PSL Research University CNRS 24 rue Lhomond Paris75005 France La Laguna TenerifeE-38206 Spain Departamento de Física Universidad de Oviedo C/ Federico García Lorca 18 Oviedo Spain Department of Astrophysics IMAPP Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of Mathematics University of Stellenbosch Stellenbosch7602 South Africa Department of Physics & Astronomy University of British Columbia 6224 Agricultural Road VancouverBC Canada Department of Physics & Astronomy University of the Western Cape Cape Town7535 South Africa Department of Physics and Astronomy University of Sussex BrightonBN1 9QH United Kingdom Depar

Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle ψ, and dispersion function of polarization angles S. The joint distribution (one-point statistics) of p and NH confirms that the mean and maximum polarization fractions decrease with increasing NH. The uncertainty on the maximum observed polarization fraction, pmax = 22.0+−31..54 % at 353 GHz and 800 resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and S found earlier is seen to be present at high latitudes. This follows the S ∝ p−1 relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, ψ, and S for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map S × p, looking for residual trends. While the polarization fraction p decreases by a factor of 3-4 between NH = 1020 cm−2 and NH = 2 × 1022 cm−2, out of the Galactic plane, this product S × p only decreases by about 25 %. Because S is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with NH is determined mostly by the magnetic-field stru

关键词： Polarization

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No random transits in CHEOPS observations of HD 139139

arXiv

引用

arXiv 2023年

作者： Alonso, R. Hoyer, S. Deleuil, M. Simon, A.E. Beck, M. Benz, W. Florén, H.-G. Guterman, P. Borsato, L. Brandeker, A. Gandolfi, D. Wilson, T.G. Zingales, T. Alibert, Y. Anglada, G. Bárczy, T. Navascues, D. Barrado Barros, S.C.C. Baumjohann, W. Beck, T. Billot, N. Bonfils, X. Broeg, Ch. Charnoz, S. Cameron, A. Collier van Damme, C. Corral Csizmadia, Sz. Cubillos, P.E. Davies, M.B. Deline, A. Delrez, L. Demangeon, O.D.S. Demory, B.-O. Ehrenreich, D. Erikson, A. Fortier, A. Fossati, L. Fridlund, M. Gillon, M. Güdel, M. Günther, M.N. Heitzmann, A. Helling, Ch. Isaak, K.G. Kiss, L.L. Kopp, E. Lam, K.W.F. Laskar, J. des Etangs, A. Lecavelier Lendl, M. Magrin, D. Maxted, P.F.L. Mordasini, Ch. Nascimbeni, V. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Santos, N.C. Scandariato, G. Ségransan, D. Smith, A.M.S. Sousa, S.G. Stalport, M. Szabó, Gy.M. Thomas, N. Udry, S. Ulmer, B. Van Grootel, V. Venturini, J. Verrecchia, F. Walton, N.A. Instituto de Astrofísica de Canarias Vía Láctea s/n Tenerife La Laguna38200 Spain Departamento de Astrofísica Universidad de La Laguna As-trofísico Francisco Sanchez s/n Tenerife La Laguna38206 Spain Aix Marseille Univ CNRS CNES LAM 38 rue Frédéric Joliot-Curie Marseille13388 France Physikalisches Institut University of Bern Gesellschaftsstrasse 6 Bern3012 Switzerland Observatoire Astronomique de l’Université de Genève Chemin Pegasi 51 VersoixCH-1290 Switzerland Center for Space and Habitability University of Bern Gesellschaftsstrasse 6 Bern3012 Switzerland Department of Astronomy Stockholm University AlbaNova University Center Stockholm10691 Sweden Division Technique INSU CS20330 La Seyne sur Mer83507 cedex France INAF Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Dipartimento di Fisica Universita degli Studi di Torino via Pietro Giuria 1 TorinoI-10125 Italy Centre for Exoplanet Science SUPA School of Physics and Astronomy University of St Andrews North Haugh St AndrewsKY16 9SS United Kingdom Dipartimento di Fisica e Astronomia "Galileo Galilei" Universita degli Studi di Padova Vicolo dell’Osservatorio 3 Padova35122 Italy Campus UAB Can Magrans s/n Bellaterra08193 Spain Gran Capità 2-4 Barcelona08034 Spain Admatis 5. Kandó Kálmán Street Miskolc3534 Hungary ESAC campus Villanueva de la Cañada Madrid28692 Spain Instituto de Astrofisica e Ciencias do Espaco Universidade do Porto CAUP Rua das Estrelas Porto4150-762 Portugal Departamento de Fisica e Astronomia Faculdade de Ciencias Universidade do Porto Rua do Campo Alegre Porto4169-007 Portugal Space Research Institute Austrian Academy of Sciences Schmiedlstrasse 6 GrazA-8042 Austria Observatoire astronomique de l’Université de Genève Chemin Pegasi 51 Versoix1290 Switzerland Université Grenoble Alpes CNRS IPAG Grenoble38000 France Université de Paris Cité Institut de physique du globe de Paris CNRS 1 Rue Jussieu ParisF-7

Context. The star HD 139139 (a.k.a. ‘the Random Transiter’) is a star that exhibited enigmatic transit-like features with no apparent periodicity in K2 data. The shallow depth of the events (∼200 ppm – equivalent to transiting objects with radii of ∼1.5 R in front of a Sun-like star) and their non-periodicity constitute a challenge for the photometric follow-up of this star. Aims. The goal of this study is to confirm with independent measurements the presence of shallow, non-periodic transit-like features on this object. Methods. We performed observations with CHEOPS for a total accumulated time of 12.75 d, distributed in visits of roughly 20 h in two observing campaigns in years 2021 and 2022. The precision of the data is sufficient to detect 150 ppm features with durations longer than 1.5 h. We used the duration and times of the events seen in the K2 curve to estimate how many events should have been detected in our campaigns, under the assumption that their behaviour during the CHEOPS observations would be the same as in the K2 data of 2017. Results. We do not detect events with depths larger than 150 ppm in our data set. If the frequency, depth, and duration of the events were the same as in the K2 campaign, we estimate the probability of having missed all events due to our limited observing window would be 4.8%. Conclusions. We suggest three different scenarios to explain our results: 1) Our observing window was not long enough, and the events were missed with the estimated 4.8% probability. 2) The events recorded in the K2 observations were time critical, and the mechanism producing them was either not active in the 2021 and 2022 campaigns or created shallower events under our detectability level. 3) The enigmatic events in the K2 data are the result of an unidentified and infrequent instrumental noise in the original data set or its data treatment. © 2023, CC BY.

关键词： Stars

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Euclid: Forecasts for k-cut 3 × 2 point statistics

arXiv

引用

arXiv 2020年

作者： Taylor, Peter L. Kitching, T. Cardone, V.F. Ferté, A. Huff, E.M. Bernardeau, F. Rhodes, J. Deshpande, A.C. Tutusaus, I. Pourtsidou, A. Camera, S. Carbone, C. Casas, S. Martinelli, M. Pettorino, V. Sakr, Z. Sapone, D. Yankelevich, V. Auricchio, N. Balestra, A. Bodendorf, C. Bonino, D. Boucaud, A. Branchini, E. Brescia, M. Capobianco, V. Carretero, J. Castellano, M. Cavuoti, S. Cimatti, A. Cledassou, R. Congedo, G. Conversi, L. Corcione, L. Cropper, M. Franceschi, E. Garilli, B. Gillis, B. Giocoli, C. Guzzo, L. Haugan, S.V.H. Holmes, W. Hormuth, F. Jahnke, K. Kermiche, S. Kilbinger, M. Kunz, M. Kurki-Suonio, H. Ligori, S. Lilje, P.B. Lloro, I. Marggraf, O. Markovic, K. Massey, R. Medinaceli, E. Mei, S. Meneghetti, M. Meylan, G. Moresco, M. Morin, B. Moscardini, L. Niemi, S. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Percival, W.J. Pires, S. Polenta, G. Poncet, M. Popa, L. Raison, F. Roncarelli, M. Rossetti, E. Saglia, R. Schneider, P. Secroun, A. Seidel, G. Serrano, S. Sirignano, C. Sirri, G. Sureau, F. Crespí, P. Tallada Tavagnacco, D. Taylor, A.N. Teplitz, H.I. Tereno, I. Toledo-Moreo, R. Valentijn, E.A. Valenziano, L. Vassallo, T. Wang, Y. Weller, J. Zacchei, A. Zoubian, J. Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Mullard Space Science Laboratory University College London Holmbury St Mary Dorking SurreyRH5 6NT United Kingdom INAF-Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio CatoneI-00078 Italy Institut de Physique Théorique CEA CNRS Université Paris-Saclay Gif-sur-Yvette CedexF-91191 France Institut d'Astrophysique de Paris 98bis Boulevard Arago ParisF-75014 France Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Carrer Gran Capitá 2-4 Barcelona08034 Spain School of Physics and Astronomy Queen Mary University of London Mile End Road LondonE1 4NS United Kingdom INFN-Sezione di Torino Via P. Giuria 1 TorinoI-10125 Italy Dipartimento di Fisica Universitá degli Studi di Torino Via P. Giuria 1 TorinoI-10125 Italy INAF-IASF Milano Via Alfonso Corti 12 MilanoI-20133 Italy AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France Instituto de Física Téorica UAM-CSIC Campus de Cantoblanco MadridE-28049 Spain Université St Joseph UR EGFEM Faculty of Sciences Beirut Lebanon Université de Toulouse CNRS UPS CNES 14 Av. Edouard Belin ToulouseF-31400 France Departamento de Física FCFM Universidad de Chile Blanco Encalada 2008 Santiago Chile Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 BolognaI-40129 Italy INAF-Osservatorio Astronomico di Padova Via dell'Osservatorio 5 PadovaI-35122 Italy Max Planck Institute for Extraterrestrial Physics Giessenbachstr. 1 GarchingD-85748 Germany INAF-Osservatorio Astrofisico di Torino Via Osservatorio 20 TO Pino TorineseI-10025 Italy Université de Paris CNRS Astroparticule et Cosmologie ParisF-75006 France INFN-Sezione di Roma Tre Via della Vasca Nava

Modelling uncertainties at small scales, i.e. high k in the power spectrum P(k), due to baryonic feedback, nonlinear structure growth and the fact that galaxies are biased tracers poses a significant obstacle to fully leverage the constraining power of the Euclid wide-field survey. k-cut cosmic shear has recently been proposed as a method to optimally remove sensitivity to these scales while preserving usable information. In this paper we generalise the k-cut cosmic shear formalism to 3 × 2 point statistics and estimate the loss of information for different k-cuts in a 3 × 2 point analysis of the Euclid data. Extending the Fisher matrix analysis of Euclid Collaboration: Blanchard et al. (2019), we assess the degradation in constraining power for different k-cuts. We work in the idealised case and assume the galaxy bias is linear, the covariance is Gaussian, while neglecting uncertainties due to photo-z errors and baryonic feedback. We find that taking a k-cut at 2.6 h Mpc-1 yields a dark energy Figure of Merit (FOM) of 1018. This is comparable to taking a weak lensing cut at = 5000 and a galaxy clustering and galaxy-galaxy lensing cut at = 3000 in a traditional 3 ×2 point analysis. We also find that the fraction of the observed galaxies used in the photometric clustering part of the analysis is one of the main drivers of the FOM. Removing 50% (90%) of the clustering galaxies decreases the FOM by 19% (62%). Given that the FOM depends so heavily on the fraction of galaxies used in the clustering analysis, extensive efforts should be made to handle the real-world systematics present when extending the analysis beyond the luminous red galaxy (LRG) sample. © 2020, CC BY.

关键词： Galaxies

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Correction for Rando et al., "Pathogenesis, Symptomatology, and Transmission of SARS-CoV-2 through Analysis of Viral Genomics and Structure"

引用

mSystems 2022年第1期7卷 e0144721页

作者： Halie M Rando Adam L MacLean Alexandra J Lee Ronan Lordan Sandipan Ray Vikas Bansal Ashwin N Skelly Elizabeth Sell John J Dziak Lamonica Shinholster Lucy D'Agostino McGowan Marouen Ben Guebila Nils Wellhausen Sergey Knyazev Simina M Boca Stephen Capone Yanjun Qi YoSon Park David Mai Yuchen Sun Joel D Boerckel Christian Brueffer James Brian Byrd Jeremy P Kamil Jinhui Wang Ryan Velazquez Gregory L Szeto John P Barton Rishi Raj Goel Serghei Mangul Tiago Lubiana Anthony Gitter Casey S Greene Department of Systems Pharmacology and Translational Therapeutics University of Pennsylvania Philadelphia Pennsylvania USA. Department of Biochemistry and Molecular Genetics University of Colorado School of Medicine Aurora Colorado USA. Center for Health AI University of Colorado School of Medicine Aurora Colorado USA. Department of Quantitative and Computational Biology University of Southern California Los Angeles California USA. Institute for Translational Medicine and Therapeutics Perelman School of Medicine University of Pennsylvania Philadelphia Pennsylvania USA. Department of Biotechnology Indian Institute of Technology Hyderabad Sangareddy Telangana India. Biomedical Data Science and Machine Learning Group German Center for Neurodegenerative Diseases Tübingen Germany. Perelman School of Medicine University of Pennsylvania Philadelphia Pennsylvania USA. Institute for Immunology Perelman School of Medicine University of Pennsylvania Philadelphia Pennsylvania USA. Edna Bennett Pierce Prevention Research Center The Pennsylvania State University University Park Pennsylvania USA. Mercer University Macon Georgia USA. Department of Mathematics and Statistics Wake Forest University Winston-Salem North Carolina USA. Department of Biostatistics Harvard School of Public Health Boston Massachusetts USA. Georgia State University Atlanta Georgia USA. Innovation Center for Biomedical Informatics Georgetown University Medical Center Washington DC USA. St. George's University School of Medicine St. George's Grenada. Department of Computer Science University of Virginiagrid.27755.32 Charlottesville Virginia USA. Department of Bioengineering University of Pennsylvania Philadelphia Pennsylvania USA. Department of Orthopaedic Surgery Perelman School of Medicine University of Pennsylvania Philadelphia Pennsylvania USA. Department of Clinical Sciences Lund University Lund Sweden. University of Michigan School of Medicine Ann Arbor Michigan USA. Depar

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Euclid Preparation. The Cosmic Dawn Survey (DAWN) of the Euclid Deep and Auxiliary Fields

arXiv

引用

arXiv 2024年

作者： McPartland, C.J.R. Zalesky, L. Weaver, J.R. Toft, S. Sanders, D.B. Mobasher, B. Suzuki, N. Szapudi, I. Valdes, I. Murphree, G. Chartab, N. Allen, N. Taamoli, S. Eisenhardt, P.R.M. Arnouts, S. Atek, H. Brinchmann, J. Castellano, M. Chary, R. Ortiz, O. Chávez Cuby, J.-G. Finkelstein, S.L. Goto, T. Gwyn, S. Inoue, A.K. McCracken, H.J. Mohr, J.J. Oesch, P.A. Ouchi, M. Oguri, M. Rhodes, J. Rottgering, H.J.A. Sawicki, M. Scaramella, R. Scarlata, C. Silverman, J.D. Stern, D. Teplitz, H.I. Shuntov, M. Altieri, B. Amara, A. Andreon, S. Auricchio, N. Aussel, H. Baccigalupi, C. Baldi, M. Bardelli, S. Bender, R. Bonino, D. Branchini, E. Brescia, M. Camera, S. Capobianco, V. Carbone, C. Carretero, J. Casas, S. Castander, F.J. Castignani, G. Cavuoti, S. Cimatti, A. Colodro-Conde, C. Congedo, G. Conselice, C.J. Conversi, L. Copin, Y. Courbin, F. Courtois, H.M. Da Silva, A. Degaudenzi, H. De Lucia, G. Di Giorgio, A.M. Dinis, J. Douspis, M. Dubath, F. Dupac, X. Dusini, S. Fabricius, M. Farina, M. Farrens, S. Ferriol, S. Fotopoulou, S. Frailis, M. Franceschi, E. Fumana, M. Galeotta, S. Garilli, B. George, K. Gillis, B. Giocoli, C. Grazian, A. Grupp, F. Guzzo, L. Hoekstra, H. Holmes, W. Hook, I. Hormuth, F. Hornstrup, A. Hudelot, P. Jahnke, K. Keihänen, E. Kermiche, S. Kiessling, A. Kilbinger, M. Kitching, T. Kubik, B. Kunz, M. Kurki-Suonio, H. Lilje, P.B. Lindholm, V. Lloro, I. Mainetti, G. Maiorano, E. Mansutti, O. Marggraf, O. Markovic, K. Martinelli, M. Martinet, N. Marulli, F. Massey, R. Maurogordato, S. Medinaceli, E. Mei, S. Melchior, M. Mellier, Y. Meneghetti, M. Merlin, E. Meylan, G. Moresco, M. Moscardini, L. Munari, E. Nakajima, R. Neissner, C. Niemi, S.-M. Nightingale, J.W. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Percival, W.J. Pettorino, V. Polenta, G. Poncet, M. Popa, L.A. Pozzetti, L. Raison, F. Rebolo, R. Renzi, A. Riccio, G. Romelli, E. Roncarelli, M. Rossetti, E. Saglia, R. Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Physics and Astronomy Department University of California 900 University Ave. RiversideCA92521 United States Denmark Department of Astronomy University of Massachusetts AmherstMA01003 United States Lawrence Berkeley National Laboratory One Cyclotron Road BerkeleyCA94720 United States Carnegie Observatories PasadenaCA91101 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Aix-Marseille Université CNRS CNES LAM Marseille France Institut d’Astrophysique de Paris UMR 7095 CNRS Sorbonne Université 98 bis boulevard Arago Paris75014 France Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas PortoPT4150-762 Portugal INAF-Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone00078 Italy Infrared Processing and Analysis Center California Institute of Technology PasadenaCA91125 United States The University of Texas at Austin AustinTX78712 United States Canada-France-Hawaii Telescope 65-1238 Mamalahoa Hwy KamuelaHI96743 United States Center for Frontier Science Chiba University 1-33 Yayoi-cho Inage-ku Chiba263-8522 Japan NRC Herzberg 5071 West Saanich Rd VictoriaBCV9E 2E7 Canada Department of Physics School of Advanced Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Universitäts-Sternwarte München Fakultät für Physik Ludwig-Maximilians-Universität München Scheinerstrasse 1 München81679 Germany Max Planck Institute for Extraterrestrial Physics Giessenbachstr. 1 Garching85748 Germany Department of

Euclid will provide deep NIR imaging to ∼26.5 AB magnitude over ∼59 deg2 in its deep and auxiliary fields. The Cosmic DAWN survey complements the deep Euclid data with matched depth multiwavelength imaging and spectroscopy in the UV–IR to provide consistently processed Euclid selected photometric catalogs, accurate photometric redshifts, and measurements of galaxy properties to a redshift of z ∼ 10. In this paper, we present an overview of the survey, including the footprints of the survey fields, the existing and planned observations, and the primary science goals for the combined data set. © 2024, CC BY.

关键词： Galaxies

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Planck intermediate results. LVII. Joint Planck LFI and HFI data processing

arXiv

引用

arXiv 2020年

作者： Akrami, Y. Andersen, K.J. Ashdown, M. Baccigalupi, C. Ballardini, M. Banday, A.J. Barreiro, R.B. Bartolo, N. Basak, S. Benabed, K. Bernard, J.-P. Bersanelli, M. Bielewicz, P. Bond, J.R. Borrill, J. Burigana, C. Butler, R.C. Calabrese, E. Casaponsa, B. Chiang, H.C. Colombo, L.P.L. Combet, C. Crill, B.P. Cuttaia, F. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Di Valentino, E. Diego, J.M. Doré, O. Douspis, M. Dupac, X. Eriksen, H.K. Fernandez-Cobos, R. Finelli, F. Frailis, M. Fraisse, A.A. Franceschi, E. Frolov, A. Galeotta, S. Galli, S. Ganga, K. Gerbino, M. Ghosh, T. González-Nuevo, J. Górski, K.M. Gruppuso, A. Gudmundsson, J.E. Handley, W. Helou, G. Herranz, D. Hildebrandt, S.R. Hivon, E. Huang, Z. Jaffe, A.H. Jones, W.C. Keihänen, E. Keskitalo, R. Kiiveri, K. Kim, J. Kisner, T.S. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lasenby, A. Lattanzi, M. Lawrence, C.R. Le Jeune, M. Levrier, F. Liguori, M. Lilje, P.B. Lilley, M. Lindholm, V. López-Caniego, M. Lubin, P.M. Macías-Pérez, J.F. Maino, D. Mandolesi, N. Marcos-Caballero, A. Maris, M. Martin, P.G. Martínez-González, E. Matarrese, S. Mauri, N. McEwen, J.D. Meinhold, P.R. Mennella, A. Migliaccio, M. Mitra, S. Molinari, D. Montier, L. Morgante, G. Moss, A. Natoli, P. Paoletti, D. Partridge, B. Patanchon, G. Pearson, D. Pearson, T.J. Perrotta, F. Piacentini, F. Polenta, G. Rachen, J.P. Reinecke, M. Remazeilles, M. Renzi, A. Rocha, G. Rosset, C. Roudier, G. Rubiño-Martín, J.A. Ruiz-Granados, B. Salvati, L. Savelainen, M. Scott, D. Sirignano, C. Sirri, G. Spencer, L.D. Suur-Uski, A.-S. Svalheim, T.L. Tauber, J.A. Tavagnacco, D. Tenti, M. Terenzi, L. Thommesen, H. Toffolatti, L. Tomasi, M. Tristram, M. Trombetti, T. Valiviita, J. van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wandelt, B.D. Wehus, I.K. Zacchei, A. Zonca, A. APC AstroParticule et Cosmologie Université Paris Diderot CNRS/IN2P3 CEA/lrfu Observatoire de Paris Sorbonne Paris Cité 10 rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France African Institute for Mathematical Sciences 6-8 Melrose Road Muizenberg Cape Town South Africa Astrophysics Group Cavendish Laboratory University of Cambridge J J Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Private Bag X54001 Durban4000 South Africa CITA University of Toronto 60 St. George St. TorontoONM5S 3H8 Canada CNRS IRAP 9 Av. colonel Roche BP 44346 Toulouse cedex 4F-31028 France Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91125 United States California Institute of Technology PasadenaCA United States Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA United States Département de Physique Théorique Université de Genève 24 Quai E. Ansermet Genève 41211 Switzerland Département de Physique École normale supérieure PSL Research University CNRS 24 rue Lhomond Paris75005 France La Laguna TenerifeE-38206 Spain Departamento de Física Universidad de Oviedo C/ Federico García Lorca 18 Oviedo Spain Department of Astrophysics IMAPP Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of Physics & Astronomy University of British Columbia 6224 Agricultural Road VancouverBC Canada Department of Physics & Astronomy University of the Western Cape Cape Town7535 South Africa Department of Physics Gustaf Hällströmin katu 2a University of Helsinki Helsinki Finland Department of Physics Princeton University PrincetonNJ United States Department of Physics University of California Santa BarbaraCA United States Dipartimento di Fisica e Astronomia G. Galilei Università degli Studi di Padova via Marzolo 8 Padova35131 It

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 0.09 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) µK, consistent with, albeit slightly higher than, earlier estimates.

关键词： Cosmology

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