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arXiv 2024年

作者： Cooper, Olivia R. Brammer, Gabriel Heintz, Kasper E. Toft, Sune Casey, Caitlin M. Setton, David J. de Graaff, Anna Boogaard, Leindert Cleri, Nikko J. Gillman, Steven Gottumukkala, Rashmi Greene, Jenny E. Gullberg, Bitten Hirschmann, Michaela Hviding, Raphael E. Lambrides, Erini Leja, Joel Long, Arianna S. Manning, Sinclaire M. Maseda, Michael V. McConachie, Ian McKinney, Jed Narayanan, Desika Price, Sedona H. Strait, Victoria Weibel, Andrea Williams, Christina C. Department of Astronomy The University of Texas at Austin AustinTX United States Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen N2200 Denmark Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany Leiden Observatory Leiden University PO Box 9513 LeidenNL-2300 RA Netherlands Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States DTU-Space Technical University of Denmark Elektrovej 327 Kgs. LyngbyDK-2800 Denmark Institute of Physics Laboratory for Galaxy Evolution Ecole Polytechnique Federale de Lausanne Observatoire de Sauverny Chemin Pegasi 51 Versoix1290 Switzerland NASA-Goddard Space Flight Center Code 662 GreenbeltMD20771 United States Department of Astronomy The University of Washington SeattleWA United States Department of Astronomy University of Massachusetts Amherst 710 N Pleasant Street AmherstMA01003 United States Department of Astronomy University of Wisconsin-Madison MadisonWI53706 United States Department of Astronomy University of Florida 211 Bryant Space Sciences Center GainesvilleFL United States Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States NSF’s National Optical-Infrared Astronomy Research Laboratory 950 North Cherry Avenue TucsonAZ85719 United States Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States

The dearth of high quality spectroscopy of dusty star-forming galaxies (DSFGs) — the main drivers of the assembly of dust and stellar mass at the peak of activity in the Universe — greatly hinders our ability to interpret their physical processes and evolutionary pathways. We present JWST/NIRSpec observations from RUBIES of four submillimeter-selected, ALMA-detected DSFGs at cosmic noon, z ∼ 2.3 − 2.7. While photometry uniformly suggests vigorous ongoing star formation for the entire sample in line with canonical DSFGs, the spectra differ: one source has spectroscopic evidence of an evolved stellar population, indicating a recent transition to a post-starburst phase, while the remainder show strong spectroscopic signatures of ongoing starbursts. All four galaxies are infrared-luminous (log10 LIR/L☉ > 12.4), massive (log10 M★/M☉ > 11), and very dust-obscured (AV ∼ 3 − 4 ABmag). Leveraging detections of multiple Balmer and Paschen lines, we derive an optical attenuation curve consistent with Calzetti overall, yet an optical extinction ratio RV ∼ 2.5, potentially indicating smaller dust grains or differences in star-dust geometry. This case study provides some of the first detailed spectroscopic evidence that the DSFGs encompass a heterogeneous sample spanning a range of star formation properties and evolutionary stages, and illustrates the advantages of synergistic JWST and ALMA analysis of DSFGs. © 2024, CC BY.

关键词： Galaxies

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The strength of the dynamical spiral perturbation in the galactic disk

arXiv

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arXiv 2020年

作者： Eilers, Anna-Christina Hogg, David W. Rix, Hans-Walter Hunt, Jason A.S. Fouvry, Jean-Baptiste Buck, Tobias MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave. CambridgeMA02139 United States Max Planck Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany Center for Cosmology and Particle Physics Department of Physics New York University 726 Broadway New YorkNY10003 United States Center for Data Science New York University 60 Fifth Ave New YorkNY10011 Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY United States Sorbonne Universit CNRS UMR 7095 Institut dAstrophysique de Paris 98 bis Bd. Arago Paris75014 France An der Sternwarte 16 Potsdam14482 Germany

The mean Galactocentric radial velocities hvRi(R, φ) of luminous red giant stars within the mid-plane of the Milky Way reveal a spiral signature, which could plausibly reflect the response to a non-axisymmetric perturbation of the gravitational potential in the Galactic disk. We apply a simple steady-state toy model of a logarithmic spiral to interpret these observations, and find a good qualitative and quantitative match. Presuming that the amplitude of the gravitational potential perturbation is proportionate to that in the disk’s surface mass density, we estimate the surface mass density amplitude to be Σmax(R) = 14 ± 5 M pc−2 at the solar radius. Combined with the local disk density, this implies a surface mass density contrast between the arm and inter-arm regions of approximately ±20% at the solar radius, with an increase towards larger Galactocentric radii. Our model constrains the pitch angle of the dynamical spiral arms to be 12.7◦ ± 1.2◦. Copyright © 2020, The Authors. All rights reserved.

关键词： Gravitation

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Exploiting dynamic nonlinearity in upconversion nanoparticles for super-resolution imaging

arXiv

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arXiv 2022年

作者： Chen, Chaohao Ding, Lei Liu, Baolei Du, Ziqin Liu, Yongtao Di, Xiangjun Shan, Xuchen Lin, Chenxiao Zhang, Min Xu, Xiaoxue Zhong, Xiaolan Wang, Jianfeng Chang, Lingqian Halkon, Ben J. Chen, Xin Cheng, Faliang Wang, Fan Guangdong Engineering and Technology Research Center for Advanced Nanomaterials School of Environment and Civil Engineering Dongguan University of Technology Dongguan523808 China Department of Chemical Engineering Shaanxi Key Laboratory of Energy Chemical Process Intensification Institute of Polymer Science in Chemical Engineering School of Chemical Engineering and Technology Xi'an Jiaotong University Xi'An710049 China School of Mathematical and Physical Sciences Faculty of Science University of Technology SydneyNSW2007 Australia School of Physics Beihang University Beijing100191 China Smart Computational Imaging Laboratory Nanjing University of Science and Technology Jiangsu Province Nanjing210094 China Department for Electrochemical Energy Storage Helmholtz-Zentrum Berlin für Materialien und Energie Hahn-Meitner-Platz Berlin14109 Germany School of Biomedical Engineering Faculty of Engineering and Information Technology University of Technology SydneyNSW2007 Australia Beijing Advanced Innovation Center for Biomedical Engineering School of Biological Science and Medical Engineering Beihang University Beijing100191 China Centre for Audio Acoustics & Vibration Faculty of Engineering & IT University of Technology Sydney UltimoNSW2007 Australia School of Electrical and Data Engineering Faculty of Engineering and Information Technology University of Technology SydneyNSW2007 Australia

Single-beam super-resolution microscopy, also known as superlinear microscopy, exploits the nonlinear response of fluorescent probes in confocal microscopy. The technique requires no complex purpose-built system, light field modulation, or beam shaping. Here, we present a strategy to enhance this technique's spatial resolution by modulating excitation intensity during image acquisition. This modulation induces dynamic optical nonlinearity in upconversion nanoparticles (UCNPs), resulting in variations of higher spatial-frequency information in the obtained images. The high-order information can be extracted with a proposed weighted finite difference imaging algorithm from raw fluorescence images, to generate an image with a higher resolution than superlinear microscopy images. We apply this approach to resolve two adjacent nanoparticles within a diffraction-limited area, improving the resolution to 130 nm. This work suggests a new scope for developing dynamic nonlinear fluorescent probes in super-resolution nanoscopy. © 2022, CC BY.

关键词： Nanoparticles

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A "Black Hole Star" Reveals the Remarkable Gas-Enshrouded Hearts of the Little Red Dots

arXiv

引用

arXiv 2025年

作者： Naidu, Rohan P. Matthee, Jorryt Katz, Harley de Graaff, Anna Oesch, Pascal Smith, Aaron Greene, Jenny E. Brammer, Gabriel Weibel, Andrea Hviding, Raphael Chisholm, John Labbé, Ivo Simcoe, Robert A. Witten, Callum Atek, Hakim Baggen, Josephine F.W. Belli, Sirio Bezanson, Rachel Boogaard, Leindert A. Bose, Sownak Covelo-Paz, Alba Dayal, Pratika Fudamoto, Yoshinobu Furtak, Lukas J. Giovinazzo, Emma Goulding, Andy Gronke, Max Heintz, Kasper E. Hirschmann, Michaela Illingworth, Garth Inoue, Akio K. Johnson, Benjamin D. Leja, Joel Leonova, Ecaterina McConachie, Ian Maseda, Michael V. Natarajan, Priyamvada Nelson, Erica Setton, David J. Shivaei, Irene Sobral, David Stefanon, Mauro Tacchella, Sandro Toft, Sune Torralba, Alberto van Dokkum, Pieter van der Wel, Arjen Volonteri, Marta Walter, Fabian Wang, Bingjie Watson, Darach MIT Kavli Institute for Astrophysics and Space Research 70 Vassar Street CambridgeMA02139 United States Am Campus 1 Klosterneuburg3400 Austria Department of Astronomy & Astrophysics University of Chicago 5640 S Ellis Avenue ChicagoIL60637 United States Max-Planck-Institut f"ur Astronomie K"onigstuhl 17 HeidelbergD-69117 Germany Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Copenhagen Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen Denmark Department of Physics The University of Texas at Dallas RichardsonTX75080 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Department of Astronomy The University of Texas at Austin AustinTX78712 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Institut d’Astrophysique de Paris CNRS Sorbonne Universit’e 98bis Boulevard Arago Paris75014 France Department of Astronomy Yale University New HavenCT06511 United States Dipartimento di Fisica e Astronomia Università di Bologna Bologna Italy Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Center for Frontier Science Chiba University 1-33 Yayoi-cho Inage-ku Chiba263-8522 Japan Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Max Planck Institute for Astrophysics Karl-Schwarzschild-Str. 1 Garching85748 Germany Institute of Physics Lab for Galaxy Evolution and Spectral Modelling EPFL Observatory of Sauverny Chemin Pegasi 51 Versoix1290 Switzerland Department of

The physical processes that led to the formation of billion solar mass black holes within the first 700 million years of cosmic time remain a puzzle1–3. Several theoretical scenarios have been proposed to seed and rapidly grow black holes4–7, but direct observations of these mechanisms remain elusive. Here we present a source 660 million years after the Big Bang that displays singular properties: among the largest Hydrogen Balmer breaks reported at any redshift, broad multi-peaked Hβ emission, and Balmer line absorption in multiple transitions. We model this source as a "black hole star" (BH*) where the Balmer break and absorption features are a result of extremely dense, turbulent gas forming a dust-free "atmosphere" around a supermassive black hole8, 9. This source may provide evidence of an early black hole embedded in dense gas – a theoretical configuration proposed to rapidly grow black holes via super-Eddington accretion10–14. Radiation from the BH* appears to dominate almost all observed light, leaving limited room for contribution from its host galaxy. We demonstrate that the recently discovered "Little Red Dots" (LRDs)15–19 with perplexing spectral energy distributions20–26 can be explained as BH*s embedded in relatively brighter host galaxies. This source provides evidence that SMBH masses in the LRDs may be over-estimated by orders of magnitude – the BH* is effectively dust-free contrary to the steep dust corrections applied while modeling LRDs9, 16, 27, 28, and the physics that gives rise to the complex line shapes and luminosities may deviate from assumptions underlying standard scaling relations. © 2025, CC BY.

关键词： Cosmology

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The Lick Observatory Supernova Search follow-up program: photometry data release of 70 stripped-envelope supernovae

arXiv

引用

arXiv 2022年

作者： Zheng, WeiKang Stahl, Benjamin E. de Jaeger, Thomas Filippenko, Alexei V. Wang, Shan-Qin Gan, Wen-Pei Brink, Thomas G. Altunin, Ivan Baer-Way, Raphael Bigley, Andrew Blanchard, Kyle Blanchard, Peter K. Bradley, James Cargill, Samantha K. Casper, Chadwick Chapman, Teagan Chander, Vidhi Channa, Sanyum Choi, Byung Yun Choksi, Nick Chu, Matthew Clubb, Kelsey I. Cohen, Daniel P. Dalba, Paul A. deGraw, Asia de Kouchkovsky, Maxime Ellison, Michael Falcon, Edward Fox, Ori D. Fuller, Kiera Ganeshalingam, Mohan Girish, Nachiket Gould, Carolina Halevi, Goni Halle, Andrew Hayakawa, Kevin T. Hardy, Romain Hestenes, Julia Hoffman, Andrew M. Hyland, Michael Jeffers, Benjamin T. Jennings, Connor Kandrashoff, Michael T. Khodanian, Anthony Kim, Minkyu Kim, Haejung Kislak, Michelle E. Krishnan, Daniel Kumar, Sahana Kumar, Snehaa Ganesh Leja, Joel Leonard, Erin J. Li, Gary Z. Li, Weidong Lian, Ji-Shun Liu, Evelyn Lowe, Thomas B. Lu, Philip Ma, Emily Mason, Michelle N. May, Michael McAllister, Kyle McGinness, Emma Modak, Shaunak Molloy, Jeffrey Murakami, Yukei S. Nayak, Omnarayani Perera, Derek Pina, Kenia Punjabi, Druv Rikhter, Andrew Ross, Timothy W. Sipple, Jackson Soler, Costas Stegman, Samantha Stephens, Haynes Sunseri, James Tang, Kevin Taylor, Stephen Thrasher, Patrick van Dyk, Schuyler D. Wang, Xiang-Gao Wayland, Jeremy Wilkins, Andrew Yagubyan, Abel Yuk, Heechan Yunus, Sameen Zhang, Keto D. Department of Astronomy University of California BerkeleyCA94720-3411 United States Department of Physics University of California BerkeleyCA94720-7300 United States Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology Guangxi University Nanning530004 China Department of Physics and Astronomy Northwestern University 1800 Sherman Ave. EvanstonIL60201 United States Department of Physics Stanford University StanfordCA94305 United States Department of Physics and Astronomy University of California Los AngelesCA90095 United States Department of Astronomy and Astrophysics University of California Santa Cruz 1156 High St. Santa CruzCA95064 United States Department of Earth and Planetary Sciences University of California Riverside 900 University Ave. RiversideCA92521 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Lawrence Berkeley National Laboratory 1 Cyclotron Rd BerkeleyCA94720 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Netflix Inc. 100 Winchester Cir Los GatosCA95032 United States Department of Physics Florida State University TallahasseeFL32306 United States 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 Jet Propulsion Laboratory California Institute of Technology PasadenaCA91109 United States The Aerospace Corporation 2310 E. El Segundo Blvd. El SegundoCA90245 United States

We present BVRI and unfiltered (Clear) light curves of 70 stripped-envelope supernovae (SESNe), observed between 2003 and 2020, from the Lick Observatory Supernova Search (LOSS) follow-up program. Our SESN sample consists of 19 spectroscopically normal SNe Ib, two peculiar SNe Ib, six SNe Ibn, 14 normal SNe Ic, one peculiar SN Ic, ten SNe Ic-BL, 15 SNe IIb, one ambiguous SN IIb/Ib/c, and two superluminous SNe. Our follow-up photometry has (on a per-SN basis) a mean coverage of 81 photometric points (median of 58 points) and a mean cadence of 3.6 d (median of 1.2 d). From our full sample, a subset of 38 SNe have pre-maximum coverage in at least one passband, allowing for the peak brightness of each SN in this subset to be quantitatively determined. We describe our data collection and processing techniques, with emphasis toward our automated photometry pipeline, from which we derive publicly available data products to enable and encourage further study by the community. Using these data products, we derive host-galaxy extinction values through the empirical colour evolution relationship and, for the first time, produce accurate rise-time measurements for a large sample of SESNe in both optical and infrared passbands. By modeling multiband light curves, we find that SNe Ic tend to have lower ejecta masses and lower ejecta velocities than SNe Ib and IIb, but higher 56Ni masses. © 2022, CC BY.

关键词： Supernovae

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New measurement of double beta decays of 100Mo to excited states of 100Ru with the CUPID-Mo experiment

arXiv

引用

arXiv 2022年

作者： Augier, C. Barabash, A.S. Bellini, F. Benato, G. Beretta, M. Bergé, L. Billard, J. Borovlev, Yu.A. Cardani, L. Casali, N. Cazes, A. Chapellier, M. Chiesa, D. Dafinei, I. Danevich, F.A. De Jesus, M. Dixon, Toby Dumoulin, L. Eitel, K. Ferri, F. Fujikawa, B.K. Gascon, J. Gironi, L. Giuliani, A. Grigorieva, V.D. Gros, M. Helis, D.L. Huang, H.Z. Huang, R. Imbert, L. Johnston, J. Juillard, A. Khalife, H. Kleifges, M. Kobychev, V.V. Kolomensky, Yu.G. Konovalov, S.I. Kotilla, J. Loaiza, P. Ma, L. Makarov, E.P. de Marcillac, P. Mariam, R. Marini, L. Marnieros, S. Navick, X.-F. Nones, C. Norman, E.B. Olivieri, E. Ouellet, J.L. Pagnanini, L. Pattavina, L. Paul, B. Pavan, M. Peng, H. Pessina, G. Pirro, S. Poda, D.V. Polischuk, O.G. Pozzi, S. Previtali, E. Redon, Th. Rojas, A. Rozov, S. Sanglard, V. Scarpaci, J.A. Schmidt, B. Shen, Y. Shlegel, V.N. Singh, V. Tomei, C. Tretyak, V.I. Umatov, V.I. Vagneron, L. Velázquez, M. Welliver, B. Winslow, L. Xue, M. Yakushev, E. Zarytskyy, M. Zolotarova, A.S. Univ Lyon Université Lyon 1 CNRS IN2P3 IP2I-Lyon Villeurbanne F-69622 France National Research Centre Kurchatov Institute Institute of Theoretical and Experimental Physics Moscow117218 Russia Dipartimento di Fisica Sapienza Università di Roma P.le Aldo Moro 2 RomeI-00185 Italy INFN Sezione di Roma P.le Aldo Moro 2 RomeI-00185 Italy I-67100 Italy University of California BerkeleyCA94720 United States Université Paris-Saclay CNRS IN2P3 IJCLab Orsay 91405 France Nikolaev Institute of Inorganic Chemistry Novosibirsk630090 Russia Dipartimento di Fisica Università di Milano-Bicocca MilanoI-20126 Italy INFN Sezione di Milano-Bicocca MilanoI-20126 Italy Institute for Nuclear Research of NASU Kyiv03028 Ukraine IRFU CEA Université Paris-Saclay Gif-sur-Yvette F-91191 France Karlsruhe Institute of Technology Institute for Astroparticle Physics Karlsruhe76021 Germany Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Fudan University Shanghai200433 China Massachusetts Institute of Technology CambridgeMA02139 United States Karlsruhe Institute of Technology Institute for Data Processing and Electronics Karlsruhe76021 Germany Department of Physics University of Jyväskylä PO Box 35 JyväskyläFI-40014 Finland Finnish Institute for Educational Research University of Jyväskylä P.O. Box 35 JyvaäskyläFI-40014 Finland Center for Theoretical Physics Sloane Physics Laboratory Yale University New HavenCT06520-8120 United States INFN Gran Sasso Science Institute L'AquilaI-67100 Italy Physik Department Technische Universität München Garching D-85748 Germany Department of Modern Physics University of Science and Technology of China Hefei230027 China LSM Laboratoire Souterrain de Modane Modane 73500 France Laboratory of Nuclear Problems JINR Dubna Moscow region 141980 Russia Université Grenoble Alpes CNRS Grenoble INP SIMAP Saint Martin d'HWeieres 38420 France

The CUPID-Mo experiment, located at Laboratoire Souterrain de Modane (France), was a demonstrator experiment for CUPID. It consisted of an array of 20 Li1002 MoO4 (LMO) calorimeters each equipped with a Ge light detector (LD) for particle identification. In this work, we present the result of a search for two-neutrino and neutrinoless double beta decays of 100Mo to the first 0+ and 2+ excited states of 100Ru using the full CUPID-Mo exposure (2.71 kg×yr of LMO). We measure the half-life of 2νββ decay to the 0+1 state as (Equation presented). The bolometric technique enables measurement of the electron energies as well as the gamma rays from nuclear de-excitation and this allows us to set new limits on the two-neutrino decay to the 2+1 state of (Equation presented) yr (90% c.i.) and on the neutrinoless modes of (Equation presented) yr (90% c.i.), (Equation presented) yr (90% c.i.). Information on the electrons spectral shape is obtained which allows us to make the first comparison of the single state (SSD) and higher state (HSD) 2νββ decay models for the 0+1 excited state of 100Ru. © 2022, CC BY.

关键词： Excited states

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JARVIS-Leaderboard: A Large Scale Benchmark of Materials Design Methods

arXiv

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arXiv 2023年

作者： Choudhary, Kamal Wines, Daniel Garrity, Kevin F. Williams, Maureen Tavazza, Francesca Li, Kangming Hattrick-Simpers, Jason Gupta, Vishu Romero, Aldo H. Krogel, Jaron T. Saritas, Kayahan Fuhr, Addis Ganesh, Panchapakesan Kent, Paul R.C. Yan, Keqiang Lin, Yuchao Ji, Shuiwang Blaiszik, Ben Reiser, Patrick Friederich, Pascal Agrawal, Ankit Tiwary, Pratyush Beyerle, Eric Minch, Peter Rhone, Trevor David Takeuchi, Ichiro Wexler, Robert B. Mannodi-Kanakkithodi, Arun Ertekin, Elif Mishra, Avanish Mathew, Nithin Wood, Mitchell Rohskopf, Andrew Dale Wang, Shih-Han Achenie, Luke E.K. Xin, Hongliang Biacchi, Adam J. Material Measurement Laboratory National Institute of Standards and Technology MD20899 United States Department of Materials Science and Engineering University of Toronto 27 King’s College Cir TorontoON Canada Department of Electrical and Computer Engineering Northwestern University EvanstonIL60208 United States Lewis-Sigler Institute for Integrative Genomics Princeton University PrincetonNJ08544 United States Ludwig Institute for Cancer Research Princeton University PrincetonNJ08544 United States Department of Physics and Astronomy West Virginia University MorgantownWV26506 United States Materials Science and Technology Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Center for Nanophase Materials Science Oak Ridge National Laboratory Oak RidgeTN37831 United States Computational Sciences and Engineering Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Department of Computer Science and Engineering Texas A&M University College StationTX77843 United States Globus University of Chicago IL60637 United States Data Science Learning Division National Lab ArgonneIL60439 United States Institute of Nanotechnology Karlsruhe Institute of Technology Kaiserstraße 12 Karlsruhe76131 Germany Institute of Theoretical Informatics Karlsruhe Institute of Technology Kaiserstraße 12 Karlsruhe76131 Germany Department of Chemistry and Biochemistry Institute for Physical Science and Technology University of Maryland College ParkMD20742 United States Department of Physics Applied Physics and Astronomy Rensselaer Polytechnic Institute TroyNY12180 United States Department of Materials Science and Engineering University of Maryland College ParkMD20742 United States Department of Chemistry Institute of Materials Science and Engineering Washington University in St. Louis St. LouisMO63130 United States School of Materials Engineering Purdue University West LafayetteIN47907 United States Department of Mechan

Lack of rigorous reproducibility and validation are significant hurdles for scientific development across many fields. Materials science, in particular, encompasses a variety of experimental and theoretical approaches that require careful benchmarking. Leaderboard efforts have been developed previously to mitigate these issues. However, a comprehensive comparison and benchmarking on an integrated platform with multiple data modalities with perfect and defect materials data is still lacking. This work introduces JARVIS-Leaderboard, an open-source and community-driven platform that facilitates benchmarking and enhances reproducibility. The platform allows users to set up benchmarks with custom tasks and enables contributions in the form of dataset, code, and meta-data submissions. We cover the following materials design categories: Artificial Intelligence (AI), Electronic Structure (ES), Force-fields (FF), Quantum Computation (QC) and Experiments (EXP). For AI, we cover several types of input data, including atomic structures, atomistic images, spectra, and text. For ES, we consider multiple ES approaches, software packages, pseudopotentials, materials, and properties, comparing results to experiment. For FF, we compare multiple approaches for material property predictions. For QC, we benchmark Hamiltonian simulations using various quantum algorithms and circuits. Finally, for experiments, we use the inter-laboratory approach to establish benchmarks. There are 1281 contributions to 274 benchmarks using 152 methods with more than 8 million data-points, and the leaderboard is continuously expanding. The JARVIS-Leaderboard is available at the website: https://***/jarvis_leaderboard/ © 2023, CC BY.

关键词： Electronic structure

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Inhomogeneous terminators on the exoplanet WASP-39 b

arXiv

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arXiv 2024年

作者： Espinoza, Néstor Steinrueck, Maria E. Kirk, James MacDonald, Ryan J. Savel, Arjun B. Arnold, Kenneth Kempton, Eliza M.-R. Murphy, Matthew M. Carone, Ludmila Zamyatina, Maria Lewis, David A. Samra, Dominic Kiefer, Sven Rauscher, Emily Christie, Duncan Mayne, Nathan Helling, Christiane Rustamkulov, Zafar Parmentier, Vivien May, Erin M. Carter, Aarynn L. Zhang, Xi López-Morales, Mercedes Allen, Natalie Blecic, Jasmina Decin, Leen Mancini, Luigi Molaverdikhani, Karan Rackham, Benjamin V. Palle, Enric Tsai, Shang-Min Ahrer, Eva-Maria Bean, Jacob L. Crossfield, Ian J.M. Haegele, David Hébrard, Eric Kreidberg, Laura Powell, Diana Schneider, Aaron D. Welbanks, Luis Wheatley, Peter Brahm, Rafael Crouzet, Nicolas Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics & Astronomy Johns Hopkins University BaltimoreMD21218 United States Königstuhl 17 HeidelbergD-69117 Germany Department of Astronomy & Astrophysics University of Chicago ChicagoIL United States Department of Physics Imperial College London Prince Consort Road LondonSW7 2AZ United Kingdom Department of Astronomy University of Michigan 1085 S. University Ave. Ann ArborMI48109 United States Department of Astronomy University of Maryland College ParkMD20742 United States Department of Astronomy Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States Space Research Institute Austrian Academy of Sciences Schmiedlstrasse 6 GrazA-8042 Austria Department of Physics and Astronomy Faculty of Environment Science and Economy University of Exeter ExeterEX4 4QL United Kingdom Institute for Theoretical Physics and Computational Physics Graz University of Technology Petersgasse 16 Graz Austria Institute of Astronomy KU Leuven Celestijnenlaan 200D Leuven3001 Belgium Centre for Exoplanet Science University of St Andrews North Haugh St AndrewsKY169SS United Kingdom Fakultät für Mathematik Physik und Geodäsie TU Graz Petersgasse 16 GrazA-8010 Austria Observatoire de la Côte d'Azur Université Côte d'Azur CNRS Laboratoire Lagrange Nice France Johns Hopkins APL 11100 Johns Hopkins Rd LaurelMD20723 United States Department of Astronomy & Astrophysics University of California Santa Cruz 1156 High St Santa CruzCA95064 United States Department of Earth and Planetary Sciences University of California Santa Cruz 1156 High St Santa CruzCA95064 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Physics New York University Abu Dhabi PO Box 129188 Abu Dhabi United Arab Emirates New York University Abu Dhabi PO Box 129188 Abu

Transmission spectroscopy has been a workhorse technique over the past two decades to constrain the physical and chemical properties of exoplanet atmospheres 1-5. One of its classical key assumptions is that the portion of the atmosphere it probes - the terminator region - is homogeneous. Several works in the past decade, however, have put this into question for highly irradiated, hot (Teq 1000 K) gas giant exoplanets both empirically 6-10 and via 3-dimensional modelling 11-17. While models predict clear differences between the evening (day-to-night) and morning (night-to-day) terminators, direct morning/evening transmission spectra in a wide wavelength range has not been reported for an exoplanet to date. Under the assumption of precise and accurate orbital parameters on WASP-39 b, here we report the detection of inhomogeneous terminators on the exoplanet WASP-39 b, which allows us to retrieve its morning and evening transmission spectra in the near-infrared (2 − 5 µm) using JWST. We observe larger transit depths in the evening which are, on average, 405±88 ppm larger than the morning ones, also having qualitatively larger features than the morning spectrum. The spectra are best explained by models in which the evening terminator is hotter than the morning terminator by 177+65−57 K with both terminators having C/O ratios consistent with solar. General circulation models (GCMs) predict temperature differences broadly consistent with the above value and point towards a cloudy morning terminator and a clearer evening terminator. Copyright © 2024, The Authors. All rights reserved.

关键词： Infrared devices

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Scaling up the lattice dynamics of amorphous materials by orders of magnitude

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Physical Review B 2020年第2期102卷 024108-024108页

作者： Ivan Kriuchevskyi Vladimir V. Palyulin Rico Milkus Robert M. Elder Timothy W. Sirk Alessio Zaccone Department of Physics “A. Pontremoli” University of Milan via Celoria 16 20133 Milan Italy Centre for Computational and Data-Intensive Science and Engineering Skolkovo Institute of Science and Technology Nobelya Ulitsa 3 Moscow 121205 Russia Department of Chemical Engineering and Biotechnology University of Cambridge Cambridge CB3 0AS United Kingdom Polymers Branch U.S. Army Research Laboratory Aberdeen Proving Ground Maryland 20783 USA Bennett Aerospace Inc. Cary North Carolina 27518 USA Center for Devices and Radiological Health U.S. Food and Drug Administration Silver Spring Maryland 20903 USA

We generalize the nonaffine theory of viscoelasticity for use with large, well-sampled systems of arbitrary chemical complexity. Having in mind predictions of mechanical and vibrational properties of amorphous systems with atomistic resolution, we propose an extension of the kernel polynomial method (KPM) for the computation of the vibrational density of states and the eigenmodes, including the Γ correlator of the affine force field, which is a key ingredient of lattice-dynamic calculations of viscoelasticity. We show that the results converge well to the solution obtained by direct diagonalization (DD) of the Hessian (dynamical) matrix. As is well known, the DD approach has prohibitively high computational requirements for systems with N=104 atoms or larger. Instead, the KPM approach developed here allows one to scale up lattice dynamic calculations of real materials up to 106 atoms, with a hugely more favorable (linear) scaling of computation time and memory consumption with N.

关键词： Dissipative dynamics Lattice dynamics Mechanical deformation Amorphous materials Polydisperse materials Polymer glasses Random & disordered media Viscoelasticity Molecular dynamics Numerical techniques

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Common explanation of the behavior of some e+e− annihilation processes around s=1.9 GeV

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Physical Review D 2018年第11期98卷 113011-113011页

作者： Peter Lichard Institute of Physics and Research Centre for Computational Physics and Data Processing Silesian University in Opava 746 01 Opava Czech Republic and Institute of Experimental and Applied Physics Czech Technical University in Prague 128 00 Prague Czech Republic

We show that the behavior of the excitation curves of some e+e− annihilation processes close to the nucleon-antinucleon threshold can be explained either by the ρ(1900) resonance itself or by its interference with other resonances. Besides the six-pion annihilation and the e+e−→K+K−π+π− and e+e−→ϕπ0 processes, we also analyze the final states ηπ+π−, K+K−π+π−π0, and K+K−π0π0, the behavior of which around 1.9 GeV has not yet attracted attention. Analysis of the data on the e+e−→pp¯ and e+e−→nn¯ reactions clearly shows that the ρ(1900) resides above the nn¯ threshold.

关键词： Particle interactions

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