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arXiv 2023年

作者： Coulombe, Louis-Philippe Benneke, Björn Challener, Ryan Piette, Anjali A.A. Wiser, Lindsey S. Mansfield, Megan MacDonald, Ryan J. Beltz, Hayley Feinstein, Adina D. Radica, Michael Savel, Arjun B. Dos Santos, Leonardo A. Bean, Jacob L. Parmentier, Vivien Wong, Ian Rauscher, Emily Komacek, Thaddeus D. Kempton, Eliza M.-R. Tan, Xianyu Hammond, Mark Lewis, Neil T. Line, Michael R. Lee, Elspeth K.H. Shivkumar, Hinna Crossfield, Ian J.M. Nixon, Matthew C. Rackham, Benjamin V. Wakeford, Hannah R. Welbanks, Luis Zhang, Xi Batalha, Natalie M. Berta-Thompson, Zachory K. Changeat, Quentin Désert, Jean-Michel Espinoza, Néstor Goyal, Jayesh M. Harrington, Joseph Knutson, Heather A. Kreidberg, Laura López-Morales, Mercedes Shporer, Avi Sing, David K. Stevenson, Kevin B. Aggarwal, Keshav Ahrer, Eva-Maria Alam, Munazza K. Bell, Taylor J. Blecic, Jasmina Caceres, Claudio Carter, Aarynn L. Casewell, Sarah L. Crouzet, Nicolas Cubillos, Patricio E. Decin, Leen Fortney, Jonathan J. Gibson, Neale P. Heng, Kevin Henning, Thomas Iro, Nicolas Kendrew, Sarah Lagage, Pierre-Olivier Leconte, Jérémy Lendl, Monika Lothringer, Joshua D. Mancini, Luigi Mikal-Evans, Thomas Molaverdikhani, Karan Nikolov, Nikolay K. Ohno, Kazumasa Palle, Enric Piaulet, Caroline Redfield, Seth Roy, Pierre-Alexis Tsai, Shang-Min Venot, Olivia Wheatley, Peter J. Department of Physics Trottier Institute for Research on Exoplanets Université de Montréal MontréalQC Canada Department of Astronomy University of Michigan Ann ArborMI United States Earth and Planets Laboratory Carnegie Institution for Science WashingtonDC United States School of Earth and Space Exploration Arizona State University TempeAZ United States Steward Observatory University of Arizona TucsonAZ United States NHFP Sagan Fellow United States Department of Astronomy Carl Sagan Institute Cornell University NY United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL United States NSF Graduate Research Fellow United States Department of Astronomy University of Maryland College ParkMD United States Center for Computational Astrophysics Flatiron Institute New YorkNY United States Space Telescope Science Institute BaltimoreMD United States Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Laboratoire Lagrange France NASA Goddard Space Flight Center GreenbeltMD United States NASA Postdoctoral Program Fellow United States Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai China School of Physics and Astronomy Shanghai Jiao Tong University Shanghai China Atmospheric Oceanic and Planetary Physics Department of Physics University of Oxford Oxford United Kingdom Department of Mathematics and Statistics Faculty of Environment Science and Economy University of Exeter Exeter United Kingdom Center for Space and Habitability University of Bern Bern Switzerland Anton Pannekoek Institute for Astronomy University of Amsterdam Amsterdam Netherlands Department of Physics & Astronomy University of Kansas LawrenceKS United States Department of Earth Atmospheric and Planetary Sciences Massachusetts Institute of Technology CambridgeMA United States Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA United States 51 Pegasi b Fellow France School of

Close-in giant exoplanets with temperatures greater than 2,000 K ("ultra-hot Jupiters") have been the subject of extensive efforts to determine their atmospheric properties using thermal emission measurements from the Hubble and Spitzer Space Telescopes1;2;3. However, previous studies have yielded inconsistent results because the small sizes of the spectral features and the limited information content of the data resulted in high sensitivity to the varying assumptions made in the treatment of instrument systematics and the atmospheric retrieval analysis3;4;5;6;7;8;9;10;11;12. Here we present a dayside thermal emission spectrum of the ultrahot Jupiter WASP-18b obtained with the NIRISS13 instrument on JWST. The data span 0.85 to 2.85 µm in wavelength at an average resolving power of 400 and exhibit minimal systematics. The spectrum shows three water emission features (at >6σ confidence) and evidence for optical opacity, possibly due to H−, TiO, and VO (combined significance of 3.8σ). Models that fit the data require a thermal inversion, molecular dissociation as predicted by chemical equilibrium, a solar heavy element abundance ("metallicity", M/H = 1.03+1.11−0.51 × solar), and a carbon-to-oxygen (C/O) ratio less than unity. The data also yield a dayside brightness temperature map, which shows a peak in temperature near the sub-stellar point that decreases steeply and symmetrically with longitude toward the terminators. © 2023, CC BY.

关键词： Molecular oxygen

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Strong detection of the CMB lensingxgalaxy weak lensingcross-correlation from ACT-DR4,plancklegacy and KiDS-1000

arXiv

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arXiv 2020年

作者： Robertson, Naomi Clare Alonso, David Harnois-Déraps, Joachim Darwish, Omar Kannawadi, Arun Amon, Alexandra Asgari, Marika Bilicki, Maciej Calabrese, Erminia Choi, Steve K. Devlin, Mark J. Dunkley, Jo Dvornik, Andrej Erben, Thomas Ferraro, Simone Fortuna, Maria Cristina Giblin, Benjamin Han, Dongwon Heymans, Catherine Hildebrandt, Hendrik Colin Hill, J. Hilton, Matt Ho, Shuay-Pwu P. Hoekstra, Henk Hubmayr, Johannes Hughes, Jack Joachimi, Benjamin Joudaki, Shahab Knowles, Kenda Kuijken, Konrad Madhavacheril, Mathew S. Moodley, Kavilan Miller, Lance Namikawa, Toshiya Nati, Federico Niemack, Michael D. Page, Lyman A. Partridge, Bruce Schaan, Emmanuel Schillaci, Alessandro Schneider, Peter Sehgal, Neelima Sherwin, Blake D. Sifón, Cristóbal Staggs, Suzanne T. Tröster, Tilman van Engelen, Alexander Valentijn, Edwin Wollack, Edward J. Wright, Angus H. Xu, Zhilei Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Sub-department of Astrophysics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Department of Applied Mathematics and Theoretical Physics University of Cambridge Wilberforce Road CambridgeCB3 0WA United Kingdom Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P.O. Box 2450 StanfordCA94305 United States Center for Theoretical Physics Polish Academy of Sciences al. Lotników 32/46 Warsaw02-668 Poland School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Department of Physics Cornell University IthacaNY14853 United States Department of Astronomy Cornell University IthacaNY14853 United States Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States German Centre for Cosmological Lensing Bochum44780 Germany Argelander-Institut für Astronomie Auf dem Hügel 71 Bonn53121 Germany Lawrence Berkeley National Laboratory One Cyclotron Road BerkeleyCA94720 United States Berkeley Center for Cosmological Physics UC Berkeley CA94720 United States Leiden Observatory Leiden University P.O.Box 9513 Leiden2300RA Netherlands Physics and Astronomy Department Stony Brook University Stony BrookNY11794 United States Department of Physics Columbia University New YorkNY10027 United States Center for Comp

We measure the cross-correlation between galaxy weak lensing data from the Kilo Degree Survey (KiDS-1000, DR4) and cosmic microwave background (CMB) lensing data from the Atacama Cosmology Telescope (ACT, DR4) and the Planck Legacy survey. We use two samples of source galaxies, selected with photometric redshifts, (0.1 B B m, and the matter fluctuation amplitude parameter, σ8, marginalising over three nuisance parameters that model our uncertainty in the redshift and shear calibration, and the intrinsic alignment of galaxies. We find our measurement to be consistent with the best-fitting flat ΛCDM cosmological models from both Planck and KiDS-1000. We demonstrate the capacity of CMB-weak lensing cross-correlations to set constraints on either the redshift or shear calibration, by analysing a previously unused high-redshift KiDS galaxy sample (1.2 B Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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Journeys from quantum optics to quantum technology

arXiv

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arXiv 2017年

作者： Barnett, Stephen M. Beige, Almut Ekert, Artur Garraway, Barry M. Keitel, Christoph H. Kendon, Viv Lein, Manfred Milburn, Gerard J. Moya-Cessa, Héctor M. Murao, Mio Pachos, Jiannis K. Palma, G. Massimo Paspalakis, Emmanuel Phoenix, Simon J.D. Piraux, Bernard Plenio, Martin B. Sanders, Barry C. Twamley, Jason Vidiella-Barranco, A. Kim, M.S. School of Physics and Astronomy University of Glasgow GlasgowG12 8QQ United Kingdom School of Physics and Astronomy University of Leeds LeedsLS2 9JT United Kingdom Mathematical Institute University of Oxford Centre for Quantum Technologies National University of Singapore Department of Physics and Astronomy University of Sussex Falmer BrightonBN1 9QH United Kingdom Max-Planck-Institut für Kernphysik Saupfercheckweg 1 Heidelberg69117 Germany Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Institute for Theoretical Physics Leibniz Universität Hannover Hannover30167 Germany Centre for Engineered Quantum Systems School of Mathematics and Physics University of Queensland 4072 Australia Instituto Nacional de Astrofísica Óptica y Electrónica Calle Luis Enrique Erro No. 1 Sta. Ma. Tonantzintla Pue.CP 72840 Mexico Department of Physics Graduate School of Science University of Tokyo Japan NEST Istituto Nanoscienze CNR Dipartimento di Fisica e Chimica Università degli Studi di Palermo via Archirafi 36 PalermoI-90123 Italy Materials Science Department School of Natural Sciences University of Patras Patras265 04 Greece Department of Applied Mathematics and Sciences Khalifa University P.O. Box: 127788 Abu Dhabi United Arab Emirates Universite Catholique de Louvain Louvain-la-NeuveB-1348 Belgium Universität Ulm Albert-Einstein-Allee 11 Ulm89069 Germany Institute for Quantum Science and Technology University of Calgary ABT2N 1N4 Canada Hefei National Laboratory for Physical Sciences at Microscale University of Science and Technology of China Hefei Anhui230026 China Shanghai Branch CAS Center for Excellence Synergetic Innovation Center in Quantum Information and Quantum Physics University of Science and Technology of China Shanghai201315 China Program in Quantum Information Science Canadian Institute for Advanced Research TorontoONM5G 1Z8 Canada Centre for Engineered Quantum Systems Department of Physics and

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Rotation in Event Horizon Telescope Movies

arXiv

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arXiv 2023年

作者： Conroy, Nicholas S. Bauböck, Michi Dhruv, Vedant Lee, Daeyoung Broderick, Avery E. Chan, Chi-Kwan Georgiev, Boris Joshi, Abhishek V. Prather, Ben Gammie, Charles F. Department of Astronomy University of Illinois at Urbana-Champaign 1002 West Green Street UrbanaIL61801 United States Department of Physics University of Illinois at Urbana-Champaign 1110 West Green Street UrbanaIL61801 United States Illinois Center for the Advanced Study of the Universe University of Illinois at Urbana-Champaign 1110 West Green St. UrbanaIL61801 United States 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 Steward Observatory Department of Astronomy University of Arizona 933 N. Cherry Ave. TucsonAZ85721 United States Data Science Institute University of Arizona 1230 N. Cherry Ave. TucsonAZ85721 United States Program in Applied Mathematics University of Arizona 617 N. Santa Rita TucsonAZ85721 United States Los Alamos National Lab Los AlamosNM87545 United States NCSA University of Illinois at Urbana-Champaign 1205 W. Clark St. UrbanaIL61801 United States

The Event Horizon Telescope (EHT) has produced images of M87* and Sagittarius A*, and will soon produce time sequences of images, or movies. In anticipation of this, we describe a technique to measure the rotation rate, or pattern speed Ωp, from movies using an autocorrelation technique. We validate the technique on Gaussian random field models with a known rotation rate and apply it to a library of synthetic images of Sgr A* based on general relativistic magnetohydrodynamics simulations. We predict that EHT movies will have Ωp ≈ 1◦ per GMc−3, which is of order 15% of the Keplerian orbital frequency in the emitting region. We can plausibly attribute the slow rotation seen in our models to the pattern speed of inward-propagating spiral shocks. We also find that Ωp depends strongly on inclination. Application of this technique will enable us to compare future EHT movies with the clockwise rotation of Sgr A* seen in near-infrared flares by GRAVITY. Pattern speed analysis of future EHT observations of M87* and Sgr A* may also provide novel constraints on black hole inclination and spin, as well as an independent measurement of black hole mass. © 2023, CC BY.

关键词： Black holes

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Measurements of jet quenching using semi-inclusive hadron+jet distributions in pp and central Pb-Pb collisions at sNN=5.02 TeV

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Physical Review C 2024年第1期110卷 014906-014906页

作者： S. Acharya D. Adamová G. Aglieri Rinella M. Agnello N. Agrawal Z. Ahammed S. Ahmad S. U. Ahn I. Ahuja A. Akindinov M. Al-Turany D. Aleksandrov B. Alessandro H. M. Alfanda R. Alfaro Molina B. Ali A. Alici N. Alizadehvandchali A. Alkin J. Alme G. Alocco T. Alt A. R. Altamura I. Altsybeev J. R. Alvarado M. N. Anaam C. Andrei N. Andreou A. Andronic V. Anguelov F. Antinori P. Antonioli N. Apadula L. Aphecetche H. Appelshäuser C. Arata S. Arcelli M. Aresti R. Arnaldi J. G. M. C. A. Arneiro I. C. Arsene M. Arslandok A. Augustinus R. Averbeck M. D. Azmi H. Baba A. Badalà J. Bae Y. W. Baek X. Bai R. Bailhache Y. Bailung A. Balbino A. Baldisseri B. Balis D. Banerjee Z. Banoo R. Barbera F. Barile L. Barioglio M. Barlou B. Barman G. G. Barnaföldi L. S. Barnby V. Barret L. Barreto C. Bartels K. Barth E. Bartsch N. Bastid S. Basu G. Batigne D. Battistini B. Batyunya D. Bauri J. L. Bazo Alba I. G. Bearden C. Beattie P. Becht D. Behera I. Belikov A. D. C. Bell Hechavarria F. Bellini R. Bellwied S. Belokurova Y. A. V. Beltran G. Bencedi S. Beole Y. Berdnikov A. Berdnikova L. Bergmann M. G. Besoiu L. Betev P. P. Bhaduri A. Bhasin M. A. Bhat B. Bhattacharjee L. Bianchi N. Bianchi J. Bielčík J. Bielčíková J. Biernat A. P. Bigot A. Bilandzic G. Biro S. Biswas N. Bize J. T. Blair D. Blau M. B. Blidaru N. Bluhme C. Blume G. Boca F. Bock T. Bodova A. Bogdanov S. Boi J. Bok L. Boldizsár M. Bombara P. M. Bond G. Bonomi H. Borel A. Borissov A. G. Borquez Carcamo H. Bossi E. Botta Y. E. M. Bouziani L. Bratrud P. Braun-Munzinger M. Bregant M. Broz G. E. Bruno M. D. Buckland D. Budnikov H. Buesching S. Bufalino P. Buhler N. Burmasov Z. Buthelezi A. Bylinkin S. A. Bysiak M. Cai H. Caines A. Caliva E. Calvo Villar J. M. M. Camacho P. Camerini F. D. M. Canedo S. L. Cantway M. Carabas A. A. Carballo F. Carnesecchi R. Caron L. A. D. Carvalho J. Castillo Castellanos F. Catalano C. Ceballos Sanchez I. Chakaberia P. Chakraborty S. Chandra S. Chapeland M. Chartier S. Chattopadhyay T. Cheng C. Cheshkov B. Cheynis V. Chibante Barroso D. D. Chinellato E. CNRS/IN2P3 LPC Clermont-Ferrand France Nuclear Physics Institute of the Czech Academy of Sciences Husinec-Řež Czech Republic Geneva Switzerland Turin Italy Bologna Italy Homi Bhabha National Institute Kolkata India Department of Physics Daejeon Republic of Korea Faculty of Science Affiliated with an institute covered by a cooperation agreement with CERN Research Division and ExtreMe Matter Institute EMMI Wuhan China Instituto de Física and Sezione INFN Bologna Italy Houston Texas USA Department of Physics and Technology Cagliari Italy Institut für Kernphysik Bari Italy Physik Department Technische Universität München Munich Germany High Energy Physics Group Bucharest Romania University of Derby Derby United Kingdom Institut für Kernphysik Münster Germany Physikalisches Institut Padova Italy Berkeley California USA SUBATECH IMT Atlantique Université Grenoble-Alpes CNRS-IN2P3 Grenoble France and Sezione INFN Cagliari Italy São Paulo Brazil New Haven Connecticut USA Tokyo Japan Catania Italy Sungkyunkwan University Suwon City Republic of Korea Gangneung Republic of Korea Hefei China Indore India Université Paris-Saclay Centre d'Etudes de Saclay (CEA) IRFU Départment de Physique Nucléaire (DPhN) Saclay France Cracow Poland Department of Physics and Centre for Astroparticle Physics and Space Science (CAPSS) Kolkata India Physics Department and Sezione INFN Catania Italy and Sezione INFN Bari Italy School of Science Department of Physics Athens Greece Department of Physics Guwahati India Budapest Hungary Nuclear Physics Group STFC Liverpool United Kingdom Department of Physics Division of Particle Physics Lund Sweden Affiliated with an international laboratory covered by a cooperation agreement with CERN Mumbai India Sección Física Departamento de Ciencias Niels Bohr Institute CNRS IPHC UMR 7178 F-67000 Strasbourg France Strasbourg France and Sezione INFN Turin Italy INFN

The ALICE Collaboration reports measurements of the semi-inclusive distribution of charged-particle jets recoiling from a high transverse momentum (high pT) charged hadron, in pp and central Pb-Pb collisions at center-of-mass energy per nucleon–nucleon collision sNN=5.02 TeV. The large uncorrelated background in central Pb-Pb collisions is corrected using a data-driven statistical approach which enables precise measurement of recoil jet distributions over a broad range in pT,chjet and jet resolution parameter R. Recoil jet yields are reported for R=0.2, 0.4, and 0.5 in the range 7

关键词： Jet quenching Quark & gluon jets Quark-gluon plasma Relativistic heavy-ion collisions Strong interaction

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Circular Polarization of Simulated Images of Black Holes

arXiv

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arXiv 2024年

作者： Joshi, Abhishek V. Prather, Ben S. Chan, Chi-Kwan Wielgus, Maciek Gammie, Charles F. Department of Physics University of Illinois 1110 West Green Street UrbanaIL61801 United States Illinois Center for Advanced Study of the Universe 1110 West Green Street UrbanaIL61801 United States Los Alamos National Lab Los AlamosNM87545 United States Steward Observatory Department of Astronomy University of Arizona 933 N. Cherry Ave. TucsonAZ85721 United States Data Science Institute University of Arizona 1230 N. Cherry Ave. TucsonAZ85721 United States Program in Applied Mathematics University of Arizona 617 N. Santa Rita TucsonAZ85721 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Department of Astronomy University of Illinois 1002 West Green Street UrbanaIL61801 United States National Center for Supercomputing Applications 605 East Springfield Avenue ChampaignIL61820 United States

Models of the resolved Event Horizon Telescope (EHT) sources Sgr A* and M87* are constrained by observations at multiple wavelengths, resolutions, polarizations, and time cadences. In this paper we compare unresolved circular polarization (CP) measurements to a library of models, where each model is characterized by a distribution of CP over time. In the library we vary the spin of the black hole, the magnetic field strength at the horizon (i.e. both SANE and MAD models), the observer inclination, a parameter for the maximum ion-electron temperature ratio assuming a thermal plasma, and the direction of the magnetic field dipole moment. We find that ALMA observations of Sgr A* are inconsistent with all edge-on (i = 90◦) models. Restricting attention to the magnetically arrested disk (MAD) models favored by earlier EHT studies of Sgr A*, we find that only models with magnetic dipole moment pointing away from the observer are consistent with ALMA data. We also note that in 26 of the 27 passing MAD models the accretion flow rotates clockwise on the sky. We provide a table of the mean and standard deviation of the CP distributions for all model parameters along with their trends. © 2024, CC BY.

关键词： Stars

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Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck. II. Cross-correlation measurements and cosmological constraints

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Physical Review D 2023年第2期107卷 023530-023530页

作者： C. Chang Y. Omori E. J. Baxter C. Doux A. Choi S. Pandey A. Alarcon O. Alves A. Amon F. Andrade-Oliveira K. Bechtol M. R. Becker G. M. Bernstein F. Bianchini J. Blazek L. E. Bleem H. Camacho A. Campos A. Carnero Rosell M. Carrasco Kind R. Cawthon R. Chen J. Cordero T. M. Crawford M. Crocce C. Davis J. DeRose S. Dodelson A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole S. Everett X. Fang A. Ferté P. Fosalba O. Friedrich M. Gatti G. Giannini D. Gruen R. A. Gruendl I. Harrison K. Herner H. Huang E. M. Huff D. Huterer M. Jarvis A. Kovacs E. Krause N. Kuropatkin P.-F. Leget P. Lemos A. R. Liddle N. MacCrann J. McCullough J. Muir J. Myles A. Navarro-Alsina Y. Park A. Porredon J. Prat M. Raveri R. P. Rollins A. Roodman R. Rosenfeld A. J. Ross E. S. Rykoff C. Sánchez J. Sanchez L. F. Secco I. Sevilla-Noarbe E. Sheldon T. Shin M. A. Troxel I. Tutusaus T. N. Varga N. Weaverdyck R. H. Wechsler W. L. K. Wu B. Yanny B. Yin Y. Zhang J. Zuntz T. M. C. Abbott M. Aguena S. Allam J. Annis D. Bacon B. A. Benson E. Bertin S. Bocquet D. Brooks D. L. Burke J. E. Carlstrom J. Carretero C. L. Chang R. Chown M. Costanzi L. N. da Costa A. T. Crites M. E. S. Pereira T. de Haan J. De Vicente S. Desai H. T. Diehl M. A. Dobbs P. Doel W. Everett I. Ferrero B. Flaugher D. Friedel J. Frieman J. García-Bellido E. Gaztanaga E. M. George T. Giannantonio N. W. Halverson S. R. Hinton G. P. Holder D. L. Hollowood W. L. Holzapfel K. Honscheid J. D. Hrubes D. J. James L. Knox K. Kuehn O. Lahav A. T. Lee M. Lima D. Luong-Van M. March J. J. McMahon P. Melchior F. Menanteau S. S. Meyer R. Miquel L. Mocanu J. J. Mohr R. Morgan T. Natoli S. Padin A. Palmese F. Paz-Chinchón A. Pieres A. A. Plazas Malagón C. Pryke C. L. Reichardt M. Rodríguez-Monroy A. K. Romer J. E. Ruhl E. Sanchez K. K. Schaffer M. Schubnell S. Serrano E. Shirokoff M. Smith Z. Staniszewski A. A. Stark E. Suchyta G. Tarle D. Thomas C. To J. D. Vieira J. Weller R. Williamson Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA Kavli Institute for Particle Astrophysics & Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Institute for Astronomy University of Hawai‘i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA California Institute of Technology 1200 East California Blvd MC 249-17 Pasadena California 91125 USA Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ - 20921-400 Brazil Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 School of Physics University of Melbourne Parkville Victoria 3010 Australia Department of Physics Northeastern University Boston Massachusetts 02115 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Department of Physics Carnegie Mellon University Pittsburgh Pennsylvania 15312 USA Instituto de Astrofisica de Canarias E-38205 La Laguna Tenerife Spain Universidad de La Laguna Dpto. Astrofísica E-38206 La Laguna Tenerife Spain Center for Astrophysical Surveys National Center for Supercomputing Applications 1205 West Clark St. Urbana Illinois 61801 USA Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street Urbana Illinois 61801 USA Physics Department William Jewell College Liberty Missouri 6

Cross-correlations of galaxy positions and galaxy shears with maps of gravitational lensing of the cosmic microwave background (CMB) are sensitive to the distribution of large-scale structure in the Universe. Such cross-correlations are also expected to be immune to some of the systematic effects that complicate correlation measurements internal to galaxy surveys. We present measurements and modeling of the cross-correlations between galaxy positions and galaxy lensing measured in the first three years of data from the Dark Energy Survey with CMB lensing maps derived from a combination of data from the 2500 deg2 SPT-SZ survey conducted with the South Pole Telescope and full-sky data from the Planck satellite. The CMB lensing maps used in this analysis have been constructed in a way that minimizes biases from the thermal Sunyaev Zel’dovich effect, making them well suited for cross-correlation studies. The total signal-to-noise of the cross-correlation measurements is 23.9 (25.7) when using a choice of angular scales optimized for a linear (nonlinear) galaxy bias model. We use the cross-correlation measurements to obtain constraints on cosmological parameters. For our fiducial galaxy sample, which consist of four bins of magnitude-selected galaxies, we find constraints of Ωm=0.272−0.052+0.032 and S8≡σ8Ωm/0.3=0.736−0.028+0.032 (Ωm=0.245−0.044+0.026 and S8=0.734−0.028+0.035) when assuming linear (nonlinear) galaxy bias in our modeling. Considering only the cross-correlation of galaxy shear with CMB lensing, we find Ωm=0.270−0.061+0.043 and S8=0.740−0.029+0.034. Our constraints on S8 are consistent with recent cosmic shear measurements, but lower than the values preferred by primary CMB measurements from Planck.

关键词： Cosmic microwave background Cosmological parameters Large scale structure of the Universe

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The Effect of Mission Duration on LISA Science Objectives

arXiv

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arXiv 2021年

作者： Seoane, Pau Amaro Sedda, Manuel Arca Babak, Stanislav Berry, Christopher P. L. Berti, Emanuele Bertone, Gianfranco Blas, Diego Bogdanović, Tamara Bonetti, Matteo Breivik, Katelyn Brito, Richard Caldwell, Robert Capelo, Pedro R. Caprini, Chiara Cardoso, Vitor Carson, Zack Chen, Hsin-Yu Chua, Alvin J. K. Dvorkin, Irina Haiman, Zoltan Heisenberg, Lavinia Isi, Maximiliano Karnesis, Nikolaos Kavanagh, Bradley J. Littenberg, Tyson B. Mangiagli, Alberto Marcoccia, Paolo Maselli, Andrea Nardini, Germano Pani, Paolo Peloso, Marco Pieroni, Mauro Ricciardone, Angelo Sesana, Alberto Tamanini, Nicola Toubiana, Alexandre Valiante, Rosa Vretinaris, Stamatis Weir, David J. Yagi, Kent Zimmerman, Aaron Institute of Multidisciplinary Mathematics Universitat Politécnica de Valéncia Spain DESY Zeuthen Germany Institute of Applied Mathematics Academy of Mathematics and Systems Science CAS Beijing China Kavli Institute for Astronomy and Astrophysics Beijing China Astronomisches Rechen-Institut Zentrüm für Astronomie Universität Heidelberg Mönchofstr. 12-14 Heidelberg Germany Université de Paris CNRS Astroparticule et Cosmologie ParisF-75006 France Moscow Institute of Physics and Technology Moscow region Dolgoprudny Russia Department of Physics and Astronomy Northwestern University 1800 Sherman Ave EvanstonIL60201 United States SUPA School of Physics and Astronomy University of Glasgow Kelvin Building University Ave GlasgowG12 8QQ United Kingdom Department of Physics and Astronomy Johns Hopkins University 3400 N. Charles St BaltimoreMD21218 United States Institute for Theoretical Physics University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Theoretical Particle Physics and Cosmology Group Department of Physics King's College London Strand LondonWC2R 2LS United Kingdom Grup de Física Teòrica Departament de Física Universitat Autònoma de Barcelona Bellaterra 08193 Spain The Barcelona Institute of Science and Technology Campus UAB Bellaterra 08193 Spain Center for Relativistic Astrophysics School of Physics Georgia Institute of Technology AtlantaGA30332 United States Università degli Studi di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States CENTRA Departamento de Física Instituto Superior Técnico - IST Universidade de Lisboa - UL Avenida Rovisco Pais 1 Lisboa 1049 France Department of Physics and Astronomy HB6127 Wilder Lab Dartmouth College HanoverNH03755 United States Center for Theoretical Astrophysics and Cosmology Institute for Computational Science University of Zurich Winterthurerstrasse 190 ZürichCH-8057

The science objectives of the LISA mission have been defined under the implicit assumption of a 4-yr continuous data stream. Based on the performance of LISA Pathfinder, it is now expected that LISA will have a duty cycle of ≈ 0.75, which would reduce the effective span of usable data to 3 yr. This paper reports the results of a study by the LISA Science Group, which was charged with assessing the additional science return of increasing the mission lifetime. We explore various observational scenarios to assess the impact of mission duration on the main science objectives of the mission. We find that the science investigations most affected by mission duration concern the search for seed black holes at cosmic dawn, as well as the study of stellar-origin black holes and of their formation channels via multi-band and multi-messenger observations. We conclude that an extension to 6 yr of mission operations is recommended. Copyright © 2021, The Authors. All rights reserved.

关键词： Black holes

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2022 Review of Data-Driven Plasma Science

arXiv

引用

arXiv 2022年

作者： Anirudh, Rushil Archibald, Rick Asif, M. Salman Becker, Markus M. Benkadda, Sadruddin Bremer, Peer-Timo Budé, Rick H.S. Chang, C.S. Chen, Lei Churchill, R.M. Citrin, Jonathan Gaffney, Jim A. Gainaru, Ana Gekelman, Walter Gibbs, Tom Hamaguchi, Satoshi Hill, Christian Humbird, Kelli Jalas, Sören Kawaguchi, Satoru Kim, Gon-Ho Kirchen, Manuel Klasky, Scott Kline, John L. Krushelnick, Karl Kustowski, Bogdan Lapenta, Giovanni Li, Wenting Ma, Tammy Mason, Nigel J. Mesbah, Ali Michoski, Craig Munson, Todd Murakami, Izumi Najm, Habib N. Erik J. Olofsson, K. Park, Seolhye Peterson, J. Luc Probst, Michael Pugmire, David Sammuli, Brian Sawlani, Kapil Scheinker, Alexander Schissel, David P. Shalloo, Rob J. Shinagawa, Jun Seong, Jaegu Spears, Brian K. Tennyson, Jonathan Thiagarajan, Jayaraman Ticoş, Catalin M. Trieschmann, Jan van Dijk, Jan Van Essen, Brian Ventzek, Peter Wang, Haimin Wang, Jason T.L. Wang, Zhehui Wende, Kristian Xu, Xueqiao Yamada, Hiroshi Yokoyama, Tatsuya Zhang, Xinhua Lawrence Livermore National Laboratory LivermoreCA94550 United States Oak Ridge National Laboratory Oak RidgeTN37830 United States University of California Riverside RiversideCA92521 United States Felix-Hausdorff-Str. 2 Greifswald17489 Germany Aix Marseille University CNRS PIIM UMR 7345 Marseille France Department of Applied Physics Eindhoven University of Technology Netherlands Princeton Plasma Physics Laboratory Princeton NJ08540 United States Institute of Ion Physics and Applied Physics University of Innsbruck Technikerstrasse 25 Innsbruck6020 Austria DIFFER - Dutch Institute for Fundamental Energy Research Eindhoven Netherlands Science and Technology of Nuclear Fusion Group Eindhoven University of Technology Eindhoven Netherlands Department of Physics and Astronomy University of California Los AngelesCA90095 United States NVIDIA 2788 San Tomas Expressway Santa ClaraCA95051 United States Center for Atomic and Molecular Technologies Graduate School of Engineering Osaka University 2-1 Yamadaoka Suita Osaka Japan Department of Nuclear Sciences and Applications International Atomic Energy Agency Wagramer Strasse 5 PO Box 100 Vienna1400 Austria Center for Free-Electron Laser Science Department of Physics Universität Hamburg Luruper Chaussee 149 Hamburg22761 Germany Division of Information and Electronic Engineering Graduate School of Engineering Muroran Institute of Technology Hokkaido Muroran050-8585 Japan Seoul National University Seoul151-741 Korea Republic of Deutsches Elektronen-Synchrotron DESY Notkestr. 85 Hamburg22607 Germany Los Alamos National Laboratory Los AlamosNM87545 United States Center for Ultrafast Optical Science University of Michigan Ann ArborMI48109-2099 United States Department of Mathematics KULeuven University of Leuven Belgium Department of Physical Sciences The University of Kent CanterburyCT2 7NH United Kingdom Department of Chemical and Biomolecular Engineering University of California Berk

Data science and technology offer transformative tools and methods to science. This review article highlights latest development and progress in the interdisciplinary field of data-driven plasma science (DDPS). A large amount of data and machine learning algorithms go hand in hand. Most plasma data, whether experimental, observational or computational, are generated or collected by machines today. It is now becoming impractical for humans to analyze all the data manually. Therefore, it is imperative to train machines to analyze and interpret (eventually) such data as intelligently as humans but far more efficiently in quantity. Despite the recent impressive progress in applications of data science to plasma science and technology, the emerging field of DDPS is still in its infancy. Fueled by some of the most challenging problems such as fusion energy, plasma-processing of materials, and fundamental understanding of the universe through observable plasma phenomena, it is expected that DDPS continues to benefit significantly from the interdisciplinary marriage between plasma science and data science into the foreseeable future. Copyright © 2022, The Authors. All rights reserved.

关键词： Machine learning

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Interacting Dark Sector (ETHOS n = 0): Cosmological Constraints from SPT Cluster Abundance with DES and HST Weak Lensing Data

arXiv

引用

arXiv 2024年

作者： Mazoun, Asmaa Bocquet, Sebastian Mohr, Joseph J. Garny, Mathias Rubira, Henrique Klein, Matthias Bleem, Lindsey E. Grandis, Sebastian Schrabback, Tim Aguena, M. Allam, S. Allen, S.W. Alves, O. Andrade-Oliveira, F. Brooks, D. Carnero Rosell, A. Carrasco Kind, M. Carretero, J. Costanzi, M. da Costa, L.N. Davis, T.M. Desai, S. De Vicente, J. Diehl, H.T. Dodelson, S. Doel, P. Everett, S. Flaugher, B. Frieman, J. García-Bellido, J. Giannini, G. Grün, D. Gutierrez, G. Hinton, S.R. Hollowood, D.L. James, D.J. Khullar, G. Kim, K. Knox, L. Kraft, R. Krause, E. Kuehn, K. Lahav, O. Lee, S. Lima, M. MacCrann, N. Mahler, G. Mantz, A. Marshall, J.L. Mena-Fernández, J. Miquel, R. Myles, J. Ogando, R.L.C. Pereira, M.E.S. Pieres, A. Plazas Malagón, A.A. Porredon, A. Reichardt, C.L. Romer, A.K. Samuroff, S. Sanchez, E. Sanchez Cid, D. Sevilla-Noarbe, I. Schubnell, M. Smith, M. Suchyta, E. Swanson, M.E.C. Tamošiūnas, A. Tarle, G. Tucker, D.L. Vikram, V. Weaverdyck, N. Weller, J. Wiseman, P. Physik Department T31 Technische Universität München James-Franck-Straße 1 GarchingD-85748 Germany University Observatory Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 MünchenD-81679 Germany Excellence Cluster ORIGINS Boltzmannstr. 2 GarchingD-85748 Germany Max Planck Institute for Extraterrestrial Physics Gießenbachstr. 1 GarchingD-85748 Germany Kavli Institute for Cosmology Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Department of Applied Mathematics and Theoretical Physics University of Cambridge CambridgeCB3 0WA United Kingdom High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstr. 25/8 Innsbruck6020 Austria Argelander-Institut für Astronomie Auf dem Hügel 71 Bonn53121 Germany Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Department of Physics University of Michigan Ann ArborMI48109 United States Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Instituto de Astrofisica de Canarias Tenerife La LagunaE-38205 Spain Universidad de La Laguna Dpto. Astrofísica Tenerife La LagunaE-38206 Spain The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Astronomy Unit Department of Physics University of Trieste via Tiepolo 11 TriesteI-34131 Italy INAF-Osservatorio Astronomico di Trieste via G. B. Tiepolo 11 TriesteI-34143 Italy Institute for Fundamental Physics of the Universe Via Beirut 2 Trieste34014 Italy School of Mathematics and Physics University of Queensland BrisbaneQLD4072 Australia Department of Physics

We use galaxy cluster abundance measurements from the South Pole Telescope (SPT) enhanced by Multi-Component Matched Filter (MCMF) confirmation and complemented with mass information obtained using weak-lensing data from Dark Energy Survey Year 3 (DES Y3) and targeted Hubble Space Telescope (HST) observations for probing deviations from the cold dark matter paradigm. Concretely, we consider a class of dark sector models featuring interactions between dark matter (DM) and a dark radiation (DR) component within the framework of the Effective Theory of Structure Formation (ETHOS). We focus on scenarios that lead to power suppression over a wide range of scales, and thus can be tested with data sensitive to large scales, as realized for example for DM−DR interactions following from an unbroken non-Abelian SU(N) gauge theory (interaction rate with power-law index n = 0 within the ETHOS parameterization). Cluster abundance measurements are mostly sensitive to the amount of DR interacting with DM, parameterized by the ratio of DR temperature to the cosmic microwave background (CMB) temperature, ξDR = TDR/TCMB. We find an upper limit ξDR © 2024, CC BY.

关键词： Matched filters

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