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arXiv 2021年

作者： Wang, Qinan Rest, Armin Zenati, Yossef Ridden-Harper, Ryan Dimitriadis, Georgios Narayan, Gautham Villar, V. Ashley Magee, Mark R. Foley, Ryan J. Shaya, Edward J. Garnavich, Peter Wang, Lifan Hu, Lei Bódi, Attila Armstrong, Patrick Auchettl, Katie Barclay, Thomas Barentsen, Geert Bognár, Zsófia Brimacombe, Joseph Bulger, Joanna Burke, Jamison Challis, Peter Chambers, Kenneth Coulter, David A. Csörnyei, Géza Cseh, Borbála Deckers, Maxime Dotson, Jessie L. Galbany, Lluís González-Gaitán, Santiago Gromadzki, Mariusz Gully-Santiago, Michael Hanyecz, Ottó Hedges, Christina Hiramatsu, Daichi Hosseinzadeh, Griffin Howell, D. Andrew Howell, Steve B. Huber, Mark E. Jha, Saurabh W. Jones, David O. Könyves-Tóth, Réka Kalup, Csilla Kilpatrick, Charles D. Kriskovics, Levente Li, Wenxiong Lowe, Thomas B. Margheim, Steven McCully, Curtis Mitra, Ayan Muñoz, Jose A. Nicholl, Matt Nordin, Jakob Pál, András Pan, Yen-Chen Piro, Anthony L. Rest, Sofia Rino-Silvestre, João Rojas-Bravo, César Sárneczky, Krisztián Siebert, Matthew R. Smartt, Stephen J. Smith, Ken Sódor, Ádám Stritzinger, Maximilian D. Szabó, Róbert Szakáts, Róbert Tucker, Brad E. Vinkó, József Wang, Xiaofeng Wheeler, J. Craig Young, David R. Zenteno, Alfredo Zhang, Kaicheng Zsidi, Gabriella Department of Physics and Astronomy The Johns Hopkins University BaltimoreMD21218 United States Space Telescope Science Institute BaltimoreMD21218 United States Israel Excellence Fellowship Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States School of Physics Trinity College Dublin The University of Dublin Dublin 2 Ireland Department of Astronomy University of Illinois 1002 W. Green St. Urbana-ChampaignIL61801 United States Center for Astrophysical Surveys National Center for Supercomputing Applications UrbanaIL61801 United States Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Astronomy Department University of Maryland College ParkMD20742 United States University of Notre Dame Notre DameIN46556 United States Mitchell Institute for Fundamental Physics Department of Physics and Astronomy Texas A&M University College StationTX77843 United States Purple Mountain Observatory Chinese Academy of Sciences 10 Yuanhua Road Nanjing210033 China Konkoly Observatory CSFK Konkoly-Thege M. ut 15-17 Budapest1121 Hungary MTA CSFK Lendület Near-Field Cosmology Research Group Konkoly Thege Miklós út 15-17 Budapest1121 Hungary Mt Stromlo Observatory The Research School of Astronomy and Astrophysics Australian National University ACT2601 Australia School of Physics The University of Melbourne VIC3010 Australia University of Maryland Baltimore County 1000 Hilltop Circle BaltimoreMD21250 United States Bay Area Environmental Research Institute P.O. Box 25 Moffett Field CA94035 United States Coral Towers Observatory Cairns Australia Institute for Astronomy University of Hawai'i 2680 Woodlawn Drive HonoluluHI96

We present the 30-min cadence Kepler/K2 light curve of the Type Ia supernova (SN Ia) SN 2018agk, covering approximately one week before explosion, the full rise phase and the decline until 40 days after peak. We additionally present ground-based observations in multiple bands within the same time range, including the 1-day cadence DECam observations within the first ~5 days after the first light. The Kepler early light curve is fully consistent with a single power-law rise, without evidence of any bump feature. We compare SN 2018agk with a sample of other SNe Ia without early excess flux from the literature. We find that SNe Ia without excess flux have slowly-evolving early colors in a narrow range (g - i ≈ -0.20±0.20 mag) within the first ~ 10 days. On the other hand, among SNe Ia detected with excess, SN 2017cbv and SN 2018oh tend to be bluer, while iPTF16abc's evolution is similar to normal SNe Ia without excess in g - i. We further compare the Kepler light curve of SN 2018agk with companion-interaction models, and rule out the existence of a typical non-degenerate companion undergoing Roche-lobe overflow at viewing angles smaller than 45°. © 2021, CC BY.

关键词： Supernovae

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Developments and applications of the OPTIMADE API for materials discovery, design, and data exchange

arXiv

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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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Polarimetric geometric modeling for mm-VLBI observations of black holes

arXiv

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arXiv 2023年

作者： Roelofs, Freek Johnson, Michael D. Chael, Andrew Janssen, Michael Wielgus, Maciek Broderick, Avery E. Akiyama, Kazunori Alberdi, Antxon Alef, Walter Algaba, Juan Carlos Anantua, Richard Asada, Keiichi Azulay, Rebecca Bach, Uwe Baczko, Anne-Kathrin Ball, David Baloković, Mislav Barrett, John Bauböck, Michi Benson, Bradford A. Bintley, Dan Blackburn, Lindy Blundell, Raymond Bouman, Katherine L. Bower, Geoffrey C. Boyce, Hope Bremer, Michael Brinkerink, Christiaan D. Brissenden, Roger Britzen, Silke Broguiere, Dominique Bronzwaer, Thomas Bustamante, Sandra Byun, Do-Young Carlstrom, John E. Ceccobello, Chiara Chan, Chi-Kwan Chang, Dominic O. Chatterjee, Koushik Chatterjee, Shami Chen, Ming-Tang Chen, Yongjun Cheng, Xiaopeng Cho, Ilje Christian, Pierre Conroy, Nicholas S. Conway, John E. Cordes, James M. Crawford, Thomas M. Crew, Geoffrey B. Cruz-Osorio, Alejandro Cui, Yuzhu Dahale, Rohan Davelaar, Jordy De Laurentis, Mariafelicia Deane, Roger Dempsey, Jessica Desvignes, Gregory Dexter, Jason Dhruv, Vedant Doeleman, Sheperd S. Dougal, Sean Dzib, Sergio A. Eatough, Ralph P. Emami, Razieh Falcke, Heino Farah, Joseph Fish, Vincent L. Fomalont, Ed Ford, H. Alyson Foschi, Marianna Fraga-Encinas, Raquel Freeman, William T. Friberg, Per Fromm, Christian M. Fuentes, Antonio Galison, Peter Gammie, Charles F. García, Roberto Gentaz, Olivier Georgiev, Boris Goddi, Ciriaco Gold, Roman Gómez-Ruiz, Arturo I. Gómez, José L. Gu, Minfeng Gurwell, Mark Hada, Kazuhiro Haggard, Daryl Haworth, Kari Hecht, Michael H. Hesper, Ronald Heumann, Dirk Ho, Luis C. Ho, Paul Honma, Mareki Huang, Chih-Wei L. Huang, Lei Hughes, David H. Ikeda, Shiro Impellizzeri, C.M. Violette Inoue, Makoto Issaoun, Sara James, David J. Jannuzi, Buell T. Jeter, Britton Jiang, Wu Jiménez-Rosales, Alejandra Jorstad, Svetlana Joshi, Abhishek V. Jung, Taehyun Karami, Mansour Karuppusamy, Ramesh Kawashima, Tomohisa Keating, Garrett K. Kettenis, Mark Kim, Dong-Jin Kim, Jae-Young Kim, Jongsoo Kim, Junhan Kino, Motoki Koay, Jun Yi Kocherlakota, Prashant Kofuji, Yutaro Koch, Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Black Hole Initiative Harvard University 20 Garden Street CambridgeMA02138 United States Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Black Hole Initiative Harvard University 20 Garden Street CambridgeMA02138 United States Princeton Gravity Initiative Princeton University Jadwin Hall PrincetonNJ08544 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Perimeter Institute for Theoretical Physics 31 Caroline Street North WaterlooONN2L 2Y5 Canada Department of Physics and Astronomy University of Waterloo 200 University Avenue West WaterlooONN2L 3G1 Canada Waterloo Centre for Astrophysics University of Waterloo WaterlooONN2L 3G1 Canada Massachusetts Institute of Technology Haystack Observatory 99 Millstone Road WestfordMA01886 United States National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n GranadaE-18008 Spain Department of Physics Faculty of Science Universiti Malaya Kuala Lumpur50603 Malaysia Department of Physics & Astronomy The University of Texas at San Antonio One UTSA Circle San AntonioTX78249 United States Institute of Astronomy and Astrophysics Academia Sinica 11F of Astronomy-Mathematics Building AS/NTU No. 1 Sec. 4 Roosevelt Rd. Taipei10617 Taiwan Departament d’Astronomia i Astrofísica Universitat de València C. Dr. Moliner 50 València BurjassotE-46100 Spain Observatori Astronòmic Universitat de València C. Catedrático José Beltrán 2 València PaternaE-46980 Spain Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory OnsalaSE-43992 Sweden Steward Observatory Department of Astronomy University of Arizona 933 N. Cherry Ave. TucsonAZ85721 United States Yale Center for Astronomy & Astrophysics Yale Universit

The Event Horizon Telescope (EHT) is a millimeter very-long-baseline interferometry (VLBI) array which has imaged the apparent shadows of the supermassive black holes M87∗ and Sagittarius A∗. Polarimetric data from these observations contain a wealth of information on the black hole and accretion flow properties. In this work, we develop polarimetric geometric modeling methods for mm-VLBI data, focusing on approaches that fit data products with differing degrees of invariance to broad classes of calibration errors. We establish a fitting procedure using a polarimetric "m-ring" model to approximate the image structure near a black hole. By fitting this model to synthetic EHT data from general relativistic magnetohydrodynamic (GRMHD) models, we show that the linear and circular polarization structure can be successfully approximated with relatively few model parameters. We then fit this model to EHT observations of M87∗ taken in 2017. In total intensity and linear polarization, the m-ring fits are consistent with previous results from imaging methods. In circular polarization, the m-ring fits indicate the presence of event-horizon-scale circular polarization structure, with a persistent dipolar asymmetry and orientation across several days. The same structure was recovered independently of observing band, used data products, and model assumptions. Despite this broad agreement, imaging methods do not produce similarly consistent results. Our circular polarization results, which imposed additional assumptions on the source structure, should thus be interpreted with some caution. Polarimetric geometric modeling provides a useful and powerful method to constrain the properties of horizon-scale polarized emission, particularly for sparse arrays like the EHT. © 2023, CC BY.

关键词： Polarimeters

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Three-dimensional general relativistic Poynting-Robertson effect II: Radiation field from a rigidly rotating spherical source

arXiv

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arXiv 2019年

作者： Bakala, Pavel de Falco, Vittorio Battista, Emmanuele Goluchová, Kateřina Lančová, Debora Falanga, Maurizio Stella, Luigi Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 OpavaCZ-74601 Czech Republic M. R. Štefánik Observatory Planetarium Sládkovičova 41 Hlohovec920 01 Slovakia International Space Science Institute Hallerstrasse 6 Bern3012 Switzerland International Space Science Institute Beijing No.1 Nanertiao Zhongguancun Haidian District Beijing100190 China INAF - Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone Roma00078 Italy

We investigate the three-dimensional, general relativistic Poynting-Robertson (PR) effect in the case of rigidly rotating spherical source which emits radiation radially in the local comoving frame. Such radiation field is meant to approximate the field produced by the surface of a rotating neutron star, or by the central radiating hot corona of accreting black holes;it extends the purely radial radiation field that we considered in a previous study. Its angular momentum is expressed in terms of the rotation frequency and radius of the emitting source. For the background we adopt a Kerr spacetime geometry. We derive the equations of motion for test particles influenced by such radiation field, recovering the classical and weak-field approximation for slow rotation. We concentrate on solutions consisting of particles orbiting along circular orbits off and parallel to the equatorial plane, which are stabilized by the balance between gravitational attraction, radiation force and PR drag. Such solutions are found to lie on a critical hypersurface, whose shape may morph from prolate to oblate depending on the Kerr spin parameter and the luminosity, rotation and radius of the radiating sphere. For selected parameter ranges, the critical hypersurface intersects the radiating sphere giving rise to a bulging equatorial region or, alternatively, two lobes above the poles. We calculate the trajectories of test particles in the close vicinity of the critical hypersurface for a selected set of initial parameters and analyze the spatial and angular velocity of test particles captured on the critical hypersurface. Copyright © 2019, The Authors. All rights reserved.

关键词： Rigidity

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End-to-end symmetry preserving inter-atomic potential energy model for finite and extended systems 18

End-to-end symmetry preserving inter-atomic potential energy...

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Proceedings of the 32nd International Conference on Neural Information processing Systems

作者： Linfeng Zhang Jiequn Han Han Wang Wissam A. Saidi Roberto Car E. Weinan Program in Applied and Computational Mathematics Princeton University Institute of Applied Physics and Computational Mathematics China and CAEP Software Center for High Performance Numerical Simulation China Department of Mechanical Engineering and Materials Science University of Pittsburgh Program in Applied and Computational Mathematics Princeton University and Department of Chemistry and Department of Physics Princeton University and Princeton Institute for the Science and Technology of Materials Princeton University Program in Applied and Computational Mathematics Princeton University and Department of Mathematics Princeton University and Beijing Institute of Big Data Research China

Machine learning models are changing the paradigm of molecular modeling, which is a fundamental tool for material science, chemistry, and computational biology. Of particular interest is the inter-atomic potential energy surface (PES). Here we develop Deep Potential - Smooth Edition (DeepPot-SE), an end-to-end machine learning-based PES model, which is able to efficiently represent the PES of a wide variety of systems with the accuracy of ab initio quantum mechanics models. By construction, DeepPot-SE is extensive and continuously differentiable, scales linearly with system size, and preserves all the natural symmetries of the system. Further, we show that DeepPot-SE describes finite and extended systems including organic molecules, metals, semiconductors, and insulators with high fidelity.

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Two Remarkably Luminous Galaxy Candidates at z ≈ 10 − 12 Revealed by JWST

arXiv

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arXiv 2022年

作者： Naidu, Rohan P. Oesch, Pascal A. van Dokkum, Pieter Nelson, Erica J. Suess, Katherine A. Brammer, Gabriel Whitaker, Katherine E. Illingworth, Garth Bouwens, Rychard Tacchella, Sandro Matthee, Jorryt Allen, Natalie Bezanson, Rachel Conroy, Charlie Labbe, Ivo Leja, Joel Leonova, Ecaterina Magee, Dan Price, Sedona H. Setton, David J. Strait, Victoria Stefanon, Mauro Toft, Sune Weaver, John R. Weibel, Andrea Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave. CambridgeMA02139 United States Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Astronomy Department Yale University 52 Hillhouse Ave New HavenCT06511 United States Department for Astrophysical and Planetary Science University of Colorado BoulderCO80309 United States Department of Astronomy and Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA95064 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Department of Astronomy University of Massachusetts AmherstMA01003 United States Denmark Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Leiden Observatory Leiden University LeidenNL-2300 RA Netherlands Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Cavendish Laboratory University of Cambridge 19 JJ Thomson Avenue CambridgeCB3 0HE United Kingdom Department of Physics ETH Zürich Wolfgang-Pauli-Strasse 27 Zürich8093 Switzerland Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States GRAPPA Anton Pannekoek Institute for Astronomy Insti

The first few hundred Myrs at z > 10 mark the last major uncharted epoch in the history of the Universe, where only a single galaxy (GNz11 at z ≈ 11) is currently spectroscopically confirmed. Here we present a search for luminous z > 10 galaxies with JWST/NIRCam photometry spanning ≈ 1 − 5µm and covering 49 arcmin2 from the public JWST Early Release Science programs (CEERS and GLASS). Our most secure candidates are two MUV ≈ −21 systems: GLASS-z12 and GLASS-z10. These galaxies display abrupt & 1.8 mag breaks in their spectral energy distributions, consistent with complete absorption of flux bluewards of Lyman-α that is redshifted to z = 12.4+0.1−0.3 and z = 10.4+0.4−0.5. Lower redshift interlopers such as quiescent galaxies with strong Balmer breaks would be comfortably detected at > 5σ in multiple bands where instead we find no flux. From SED modeling we infer that these galaxies have already built up ∼ 109 solar masses in stars over the. 300−400 Myrs after the Big Bang. The brightness of these sources enable morphological constraints. Tantalizingly, GLASS-z10 shows a clearly extended exponential light profile, potentially consistent with a disk galaxy of r50 ≈ 0.7 kpc. These sources, if confirmed, join GNz11 in defying number density forecasts for luminous galaxies based on Schechter UV luminosity functions, which require a survey area > 10× larger than we have studied here to find such luminous sources at such high redshifts. They extend evidence from lower redshifts for little or no evolution in the bright end of the UV luminosity function into the cosmic dawn epoch, with implications for just how early these galaxies began forming. This, in turn, suggests that future deep JWST observations may identify relatively bright galaxies to much earlier epochs than might have been anticipated. © 2022, CC BY.

关键词： Galaxies

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Impact of beam far side-lobe knowledge in the presence of foregrounds for LiteBIRD

arXiv

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arXiv 2023年

作者： Leloup, C. Patanchon, G. Errard, J. Franceschet, C. Gudmundsson, J.E. Henrot-Versillé, S. Imada, H. Ishino, H. Matsumura, T. Puglisi, G. Wang, W. Adler, A. Aumont, J. Aurlien, R. Baccigalupi, C. Ballardini, M. Banday, A.J. Barreiro, R.B. Bartolo, N. Basyrov, A. Bersanelli, M. Blinov, D. Bortolami, M. Brinckmann, T. 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 Diego-Palazuelos, P. Eriksen, H.K. Finelli, F. 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. Gruppuso, A. Hazumi, M. Hergt, L.T. Herranz, D. Hivon, E. Hoang, T.D. Jost, B. Kohri, K. Krachmalnicoff, N. Lee, A.T. Lembo, M. Levrier, F. Lonappan, A.I. López-Caniego, M. Macias-Perez, J. Martínez-González, E. Masi, S. Matarrese, S. Micheli, S. Monelli, M. Montier, L. Morgante, G. Mot, B. Mousset, L. Namikawa, T. Natoli, P. Novelli, A. Noviello, F. Obata, I. Odagiri, K. Pagano, L. Paiella, A. Paoletti, D. Pascual-Cisneros, G. Pavlidou, V. Piacentini, F. Piccirilli, G. Pisano, G. Polenta, G. Raffuzzi, N. Remazeilles, M. Ritacco, A. Rizzieri, A. Ruiz-Granda, M. Sakurai, Y. Shiraishi, M. Stever, S.L. Takase, Y. Tassis, K. Terenzi, L. Thompson, K.L. Tristram, M. Vacher, L. Vielva, P. Wehus, I.K. Weymann-Despres, G. Zannoni, M. Zhou, Y. UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Université de Paris CNRS Astroparticule et Cosmologie ParisF-75013 France Dipartimento di Fisica Universita’ degli Studi di Milano Via Celoria 16 Milano20133 Italy INFN Sezione di Milano Via Celoria 16 Milano20133 Italy The Oskar Klein Centre Department of Physics Stockholm University StockholmSE-106 91 Sweden Université Paris-Saclay CNRS IN2P3 IJCLab Orsay91405 France National Astronomical Observatory of Japan Mitaka Tokyo181-8588 Japan Okayama University Department of Physics Okayama700-8530 Japan Dipartimento di Fisica e Astronomia Universitá degli Studi di Catania Via S. Sofia64 Catania95123 Italy INAF Osservatorio Astrofisico di Catania via S.Sofia 78 CataniaI-95123 Italy INFN Sezione di Catania via S.Sofia 64 CataniaI-95123 Italy IRAP Université de Toulouse CNRS CNES UPS Toulouse France Institute of Theoretical Astrophysics University of Oslo Blindern Oslo Norway 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 Scienze della Terra Università di Ferrara Via Saragat 1 Ferrara44122 Italy INFN Sezione di Ferrara Via Saragat 1 Ferrara44122 Italy INAF - OAS Bologna via Piero Gobetti 93/3 Bologna40129 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 Institute of Astrophysics Foundation for Research and Technology-Hellas Vasilika Vouton HeraklionGR-70013 Greece Department of Physics ITCP University of Crete HeraklionGR-70013 Greece Max Planck Institute for Astrophysics Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany Excellence Cluster ORIGINS Boltzmannstr. 2 Garc

We present a study of the impact of a beam far side-lobe lack of knowledge on the measurement of the Cosmic Microwave Background B-mode signal at large scale. Beam far side-lobes induce a mismatch in the transfer function of Galactic foregrounds between the dipole and higher multipoles which degrades the performances of component separation methods. This leads to foreground residuals in the CMB map. It is expected to be one of the main source of systematic effects in future CMB polarization observations. Thus, it becomes crucial for all-sky survey missions to take into account the interplays between beam systematic effects and all the data analysis steps. LiteBIRD is the ISAS/JAXA second strategic large-class satellite mission and is dedicated to target the measurement of CMB primordial B modes by reaching a sensitivity on the tensor-to-scalar ratio r of σ (r) ≤ 10−3 assuming r = 0. The primary goal of this paper is to provide the methodology and develop the framework to carry out the end-to-end study of beam far side-lobe effects for a space-borne CMB experiment. We introduce uncertainties in the beam model, and propagate the beam effects through all the steps of the analysis pipeline, most importantly including component separation, up to the cosmological results in the form of a bias δr. As a demonstration of our framework, we derive requirements on the calibration and modeling for the LiteBIRD’s beams under given assumptions on design, simulation, component separation method and allocated error budget. In particular, we assume a parametric method of component separation with no mitigation of the far side-lobes effect at any stage of the analysis pipeline. We show that δr is mostly due to the integrated fractional power difference between the estimated beams and the true beams in the far side-lobes region, with little dependence on the actual shape of the beams, for low enough δr. Under our set of assumptions, in particular considering the specific foreground cle

关键词： Pipelines

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Preliminary target selection for the desi bright galaxy survey (BGS)

arXiv

引用

arXiv 2020年

作者： Ruiz-Macias, Omar Zarrouk, Pauline Cole, Shaun Norberg, Peder Baugh, Carlton Brooks, David Dey, Arjun Duan, Yutong Eftekharzadeh, Sarah Eisenstein, Daniel J. Forero-Romero, Jaime E. Gaztañaga, Enrique Hahn, ChangHoon Kehoe, Robert Landriau, Martin Lang, Dustin Levi, Michael E. Lucey, John Meisner, Aaron M. Moustakas, John Myers, Adam D. Palanque-Delabrouille, Nathalie Poppett, Claire Prada, Francisco Raichoor, Anand Schlegel, David J. Schubnell, Michael Tarlé, Gregory Weinberg, David H. Wilson, M.J. Yèche, Christophe Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Institute for Data Science Durham University South Road DurhamDH1 3LE United Kingdom Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Department of Physics and Astromomy University College London Gower Street LondonWC1e 6BT United Kingdom NSF’s National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Physics Department Boston University BostonMA02215 United States Department of Physics and Astronomy University of Utah 115 South 1400 East Salt Lake CityUT84112 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Departamento de Física Universidad de los Andes Cra. 1 No. 18A-10 BogotáCP 111711 Colombia Barcelona08193 Spain Barcelona08034 Spain Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Berkeley Center for Cosmological Physics UC Berkeley CA94720 United States Department of Physics Southern Methodist University 3215 Daniel Avenue DallasTX75275 United States Perimeter Institute for Theoretical Physics 31 Caroline Street N WaterlooONN2L 2Y5 Canada Department of Physics and Astronomy University of Waterloo WaterlooONN2L 3G1 Canada Department of Physics and Astronomy Siena College 515 Loudon Road LoudonvilleNY12211 United States University of Wyoming 1000 E. University Ave. LaramieWY 82071 United States IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France Space Sciences Laboratory University of California 7 Gauss Way BerkeleyCA94720 United States Glorieta de la Astronomía GranadaE-18080 Spain Observatoire de Sauverny Versoix1290 Switzerland Department of Physics University of Michigan 450 Church St. Ann ArborMI48109 United States Department of Physics University of Michigan

The Dark Energy Spectroscopic Instrument (DESI) will execute a nearly magnitude-limited survey of low redshift galaxies (0.05 ≤ z ≤ 0.4, median z ≈ 0.2). Clustering analyses of this Bright Galaxy Survey (BGS) will yield the most precise measurements to date of baryon acoustic oscillations and redshift-space distortions at low redshift. DESI BGS will comprise two target classes: (i) BRIGHT (r 2 for the BRIGHT and ∼ 600 objects/deg2 for the FAINT selections. A full characterization of the BGS selection can be found in Ruiz-Macias et al. (2020). Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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Active learning of uniformly accurate inter-atomic potentials for materials simulation

arXiv

引用

arXiv 2018年

作者： Zhang, Linfeng Lin, De-Ye Wang, Han Car, Roberto Weinan, E. Program in Applied and Computational Mathematics Princeton University PrincetonNJ08544 United States Institute of Applied Physics and Computational Mathematics Huayuan Road 6 Beijing100088 China CAEP Software Center for High Performance Numerical Simulation Huayuan Road 6 Beijing100088 China Laboratory of Computational Physics Institute of Applied Physics and Computational Mathematics Huayuan Road 6 Beijing100088 China Department of Chemistry Department of Physics Program in Applied and Computational Mathematics Princeton Institute for the Science and Technology of Materials Princeton University PrincetonNJ08544 United States Department of Mathematics and Program in Applied and Computational Mathematics Princeton University PrincetonNJ08544 United States Beijing Institute of Big Data Research Beijing100871 China

An active learning procedure called Deep Potential Generator (DP-GEN) is proposed for the construction of accurate and transferable machine learning-based models of the potential energy surface (PES) for the molecular modeling of materials. This procedure consists of three main components: exploration, generation of accurate reference data, and training. Application to the sample systems of Al, Mg and Al-Mg alloys demonstrates that DP-GEN can produce uniformly accurate PES models with a minimal number of reference data. Copyright © 2018, The Authors. All rights reserved.

关键词： Potential energy

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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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