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arXiv 2023年

作者： Huppenkothen, Daniela Ntampaka, Michelle Ho, Matthew Fouesneau, Morgan Nord, Brian Peek, J.E.G. Walmsley, Mike Wu, John F. Avestruz, C. Buck, Tobias Brescia, Massimo Finkbeiner, Douglas P. Goulding, Andy D. Kacprzak, T. Melchior, Peter Pasquato, Mario Ramachandra, Nesar Ting, Yuan-Sen van de Ven, Glenn Villar, Soledad Villar, V.A. Zinger, Elad SRON Netherlands Institute for Space Research Niels Bohrweg 4 Leiden2333CA Netherlands Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Space Telescope Science Institute BaltimoreMD21218 United States Department of Physics & Astronomy Johns Hopkins University BaltimoreMD21218 United States UMR 7095 98 bis bd Arago ParisF-75014 France Königstuhl 17 HeidelbergD-69117 Germany Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Jodrell Bank Centre for Astrophysics Department of Physics & Astronomy University of Manchester ManchesterM13 9PL United Kingdom Dunlap Institute for Astronomy & Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada Leinweber Center for Theoretical Physics University of Michigan Ann ArborMI48109 United States Department of Physics University of Michigan Ann ArborMI48109 United States Universität Heidelberg Interdisziplinäres Zentrum für Wissenschaftliches Rechnen Im Neuenheimer Feld 205 Heidelberg69120 Germany Universität Heidelberg Zentrum für Astronomie Institut für Theoretische Astrophysik Albert-Ueberle-Straße 2 Heidelberg69120 Germany Department of Physics "E. Pancini " University Federico II of Napoli Via Cinthia 21 NapoliI-80126 Italy INAF Astronomical Observatory of Capodimonte Salita Moiariello 16 NapoliI-80131 Italy Department of Physics Harvard University 17 Oxford St. CambridgeMA02138 United States Harvard-Smithsonian Center for Astrophysics 60 Garden St. CambridgeMA02138 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Swiss Data Science Center Paul Scherrer Institute Villigen5303 Switzerland Center for Statistics & Machine Learn

Machine learning has rapidly become a tool of choice for the astronomical community. It is being applied across a wide range of wavelengths and problems, from the classification of transients to neural network emulators of cosmological simulations, and is shifting paradigms about how we generate and report scientific results. At the same time, this class of method comes with its own set of best practices, challenges, and drawbacks, which, at present, are often reported on incompletely in the astrophysical literature. With this paper, we aim to provide a primer to the astronomical community, including authors, reviewers, and editors, on how to implement machine learning models and report their results in a way that ensures the accuracy of the results, reproducibility of the findings, and usefulness of the method. Copyright © 2023, The Authors. All rights reserved.

关键词： Machine learning

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Warm dense matter simulation via electron temperature dependent deep potential molecular dynamics

arXiv

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arXiv 2019年

作者： Zhang, Yuzhi Gao, Chang Zhang, Linfeng Wang, Han Chen, Mohan Center for Applied Physics and Technology HEDPS College of Engineering Peking University Beijing100871 China Beijing Institute of Big Data Research Beijing100871 China Program in Applied and Computational Mathematics Princeton University PrincetonNJ United States Laboratory of Computational Physics Institute of Applied Physics and Computational Mathematics Huayuan Road 6 Beijing100088 China

Simulating warm dense matter that undergoes a wide range of temperatures and densities is challenging. Predictive theoretical models, such as quantum-mechanics-based first-principles molecular dynamics (FPMD), require a huge amount of computational resources. Herein, we propose a deep learning based scheme, called electron temperature dependent deep potential molecular dynamics (TDDPMD), for efficiently simulating warm dense matter with the accuracy of FPMD. The TDDPMD simulation is several orders of magnitudes faster than FPMD, and, unlike FPMD, its efficiency is not affected by the electron temperature. We apply the TDDPMD scheme to beryllium (Be) in a wide range of temperatures (0.4 to 2500 eV) and densities (3.50 to 8.25 g/cm3). Our results demonstrate that the TDDPMD method not only accurately reproduces the structural properties of Be along the principal Hugoniot curve at the FPMD level, but also yields even more reliable diffusion coefficients than typical FPMD simulations due to its ability to simulate larger systems with longer time. Copyright © 2019, The Authors. All rights reserved.

关键词： Molecular dynamics

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Metric assisted stochastic sampling search for gravitational waves from binary black hole mergers

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Physical Review D 2022年第8期106卷 084033-084033页

作者： Chad Hanna Prathamesh Joshi Rachael Huxford Kipp Cannon Sarah Caudill Chiwai Chan Bryce Cousins Jolien D. E. Creighton Becca Ewing Miguel Fernandez Heather Fong Patrick Godwin Ryan Magee Duncan Meacher Cody Messick Soichiro Morisaki Debnandini Mukherjee Hiroaki Ohta Alexander Pace Stephen Privitera Surabhi Sachdev Shio Sakon Divya Singh Ron Tapia Leo Tsukada Daichi Tsuna Takuya Tsutsui Koh Ueno Aaron Viets Leslie Wade Madeline Wade Jonathan Wang Department of Physics Pennsylvania State University University Park Pennsylvania 16802 USA Institute for Gravitation and the Cosmos Pennsylvania State University University Park Pennsylvania 16802 USA Department of Astronomy and Astrophysics Pennsylvania State University University Park Pennsylvania 16802 USA Institute for Computational and Data Sciences Pennsylvania State University University Park Pennsylvania 16802 USA RESCEU The University of Tokyo Tokyo 113-0033 Japan Nikhef Science Park 1098 XG Amsterdam Netherlands Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin–Milwaukee Milwaukee Wisconsin 53201 USA Graduate School of Science The University of Tokyo Tokyo 113-0033 Japan LIGO Laboratory California Institute of Technology MS 100-36 Pasadena California 91125 USA LIGO Laboratory Massachusetts Institute of Technology Cambridge Massachusetts 02139 USA Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba 277-8582 Japan Albert-Einstein-Institut Max-Planck-Institut für Gravitationsphysik D-14476 Potsdam-Golm Germany Department of Physics Hayes Hall Kenyon College Gambier Ohio 43022 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA

We present a novel gravitational-wave detection algorithm that conducts a matched-filter search stochastically across the compact binary parameter space rather than relying on a fixed bank of template waveforms. This technique is competitive with standard template-bank-driven pipelines in both computational cost and sensitivity. However, the complexity of the analysis is simpler, allowing for easy configuration and horizontal scaling across heterogeneous grids of computers. To demonstrate the method we analyze approximately one month of public LIGO data from July 27 00:00 2017 UTC–Aug 25 22:00 2017 UTC and recover eight known confident gravitational-wave candidates. We also inject simulated binary black hole signals to demonstrate the sensitivity.

关键词： Classical black holes Gravitational wave detection Gravitational wave sources

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Emission-Line Diagnostics at z > 4: [O III]λ4363/Hγ

arXiv

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arXiv 2025年

作者： Backhaus, Bren E. Cleri, Nikko J. Trump, Jonathan R. Kirkpatrick, Allison Simons, Raymond C. Haro, Pablo Arrabal Bagley, Micaela B. Brooks, Madisyn Calabrò, Antonello Davis, Kelcey Dickinson, Mark Finkelstein, Steven L. Hirschmann, Michaela Kartaltepe, Jeyhan S. Koekemoer, Anton M. Llerena, Mario Pacucci, Fabio Pirzkal, Nor Papovich, Casey Wilkins, Stephen M. Department of Physics and Astronomy University of Kansas LawrenceKS66045 United States Department of Physics University of Connecticut 196A Auditorium Road Unit 3046 StorrsCT06269 United States 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 NSF’s National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Department of Astronomy The University of Texas at Austin AustinTX United States INAF Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone Rome00078 Italy Observatoire de Sauverny Versoix1290 Switzerland Laboratory for Multiwavelength Astrophysics School of Physics and Astronomy Rochester Institute of Technology 84 Lomb Memorial Drive RochesterNY14623 United States Space Telescope Science Institute 3700 San Martin Dr. BaltimoreMD21218 United States INAF - Osservatorio Astronomico di Roma via di Frascati 33 Monte Porzio Catone00078 Italy Center for Astrophysics | Harvard & Smithsonian 60 Garden St CambridgeMA02138 United States Black Hole Initiative Harvard University 20 Garden St CambridgeMA02138 United States ESA AURA Space Telescope Science Institute United States Department of Physics and Astronomy Texas A&M University College StationTX77843-4242 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University College StationTX77843-4242 United States Astronomy Centre University of Sussex Falmer BrightonBN1 9QH United Kingdom Institute of Space Sciences and Astronomy University of Malta MsidaMSD 2080 Malta

We use JWST Near-Infrared Spectrograph (NIRSpec) observations from the the Cosmic Evolution Early Release survey (CEERS), GLASS-JWST ERS (GLASS), and JWST Advanced Deep Extragalactic Survey (JADES) to measure rest-frame optical emission-line ratios of 90 galaxies at z > 4. The stacked spectra of galaxies with and without a broad-line feature reveal a difference in the [O III]λ 4363 and Hγ ratios. This motivated our investigation of the [O III]λ4363/Hγ vs [Ne III]/[O II] diagram. We define two AGN/SF classification lines based on 1869 SDSS galaxies at z ∼ 0. After applying a redshift correction to the AGN/SF lines we find 76.8% of BLAGN continue to land in the AGN region of the diagnostic largely due to the [Ne III]/[O II] ratio. However, 40.2% of non-BLAGN land in the AGN region as well, this could be due to star forming galaxies having harder ionization of there are narrow line AGN which are not accounted for. This indicates the potential of the [Ne III]/[O II]ratio to continue classifying galaxies to z ∼ 6. We further inspect galaxies without broad emission lines in each region of [O III]λ4363/Hγ vs [Ne III]/[O II] diagram and found that they have slightly stronger C III]λ1908 fluxes and equivalent width when landing in the BLAGN region. However, the cause of this higher ionization is unclear. Additionally, we find that BLAGN are characterized by a higher ionization (at constant electron temperature) compared to non-broad line galaxies. © 2025, CC BY.

关键词： Cosmology

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Waveform Modelling for the Laser Interferometer Space Antenna

arXiv

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arXiv 2023年

作者： Afshordi, Niayesh Akçay, Sarp Seoane, Pau Amaro Antonelli, Andrea Aurrekoetxea, Josu C. Barack, Leor Barausse, Enrico Benkel, Robert Bernard, Laura Bernuzzi, Sebastiano Berti, Emanuele Bonetti, Matteo Bonga, Béatrice Bozzola, Gabriele Brito, Richard Buonanno, Alessandra Cárdenas-Avendaño, Alejandro Casals, Marc Chernoff, David F. Chua, Alvin J.K. Clough, Katy Colleoni, Marta Compère, Geoffrey Dhesi, Mekhi Druart, Adrien Durkan, Leanne Faye, Guillaume Ferguson, Deborah Field, Scott E. Gabella, William E. García-Bellido, Juan Gracia-Linares, Miguel Gerosa, Davide Green, Stephen R. Haney, Maria Hannam, Mark Heffernan, Anna Hinderer, Tanja Helfer, Thomas Hughes, Scott A. Husa, Sascha Isoyama, Soichiro Katz, Michael L. Kavanagh, Chris Khanna, Gaurav Kidder, Larry E. Korol, Valeriya Küchler, Lorenzo Laguna, Pablo Larrouturou, François Le Tiec, Alexandre Leather, Benjamin Lim, Eugene A. Lim, Hyun Littenberg, Tyson B. Long, Oliver Lousto, Carlos O. Lovelace, Geoffrey Lukes-Gerakopoulos, Georgios Lynch, Philip Macedo, Rodrigo P. Markakis, Charalampos Maggio, Elisa Mandel, Ilya Maselli, Andrea Mathews, Josh Mourier, Pierre Neilsen, David Nagar, Alessandro Nichols, David A. Novák, Jan Okounkova, Maria O’Shaughnessy, Richard Oshita, Naritaka O’Toole, Conor Pan, Zhen Pani, Paolo Pappas, George Paschalidis, Vasileios Pfeiffer, Harald P. Pompili, Lorenzo Pound, Adam Pratten, Geraint Rüter, Hannes R. Ruiz, Milton Sam, Zeyd Sberna, Laura Shapiro, Stuart L. Shoemaker, Deirdre M. Sopuerta, Carlos F. Spiers, Andrew Sundar, Hari Tamanini, Nicola Thompson, Jonathan E. Toubiana, Alexandre Tsokaros, Antonios Upton, Samuel D. van de Meent, Maarten Vernieri, Daniele Wachter, Jeremy M. Warburton, Niels Wardell, Barry Witek, Helvi Witzany, Vojtěch Yang, Huan Zilhão, Miguel Albertini, Angelica Arun, K.G. Bezares, Miguel Bonilla, Alexander Chapman-Bird, Christian Cownden, Bradley Cunningham, Kevin Devitt, Chris Dolan, Sam Duque, Francisco Dyson, Conor Fryer, Chris L. Gair, Jonathan R. Giacomazzo, Bruno Gupta, Priti Han, Wen-Biao Haas, Roland Perimeter Institute for Theoretical Physics WaterlooONN2L 2Y5 Canada School of Mathematics and Statistics University College Dublin Belfield Dublin 4 Ireland Universitat Politècnica de València València Spain Max Planck Institute for Extraterrestrial Physics Garching Germany Higgs Centre for Theoretical Physics Edinburgh United Kingdom Kavli Institute for Astronomy and Astrophysics Beijing100871 China William H. Miller III Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Astrophysics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom School of Mathematical Sciences and STAG Research Centre University of Southampton SouthamptonSO17 1BJ United Kingdom SISSA Via Bonomea 265 Trieste34136 Italy INFN Sezione di Trieste IFPU Institute for Fundamental Physics of the Universe Via Beirut 2 Trieste34014 Italy Max Planck Institute for Gravitational Physics Albert Einstein Institute PotsdamD-14476 Germany Laboratoire Univers et Théories CNRS Observatoire de Paris Université PSL Université Paris Cité Meudon92190 France Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena Jena07743 Germany Dipartimento di Fisica "G. Occhialini" Universitá degli Studi di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy INFN Sezione di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy Institute for Mathematics Astrophysics and Particle Physics Radboud University Nijmegen6525 AJ Netherlands The University of Arizona Department of Astronomy TucsonAZ85721 United States CENTRA Departamento de Física Instituto Superior Técnico – IST Universidade de Lisboa – UL Avenida Rovisco Pais 1 Lisboa1049-001 Portugal Princeton Gravity Initiative Princeton University PrincetonNJ08544 United States Institut für Theoretische Physik Universität Leipzig Brüderstraße 16 Leipzig04103 Germany Rio de JaneiroCEP 22290-180 Brazil Department of Astronomy Cornell Univers

LISA, the Laser Interferometer Space Antenna, will usher in a new era in gravitational-wave astronomy. As the first anticipated space-based gravitational-wave detector, it will expand our view to the millihertz gravitational-wave sky, where a spectacular variety of interesting new sources abound: from millions of ultra-compact binaries in our Galaxy, to mergers of massive black holes at cosmological distances;from the beginnings of inspirals that will venture into the ground-based detectors’ view to the death spiral of compact objects into massive black holes, and many sources in between. Central to realising LISA’s discovery potential are waveform models, the theoretical and phenomenological predictions of the pattern of gravitational waves that these sources emit. This white paper is presented on behalf of the Waveform Working Group for the LISA Consortium. It provides a review of the current state of waveform models for LISA sources, and describes the significant challenges that must yet be overcome. © 2023, CC BY.

关键词： Gravity waves

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ASTRODEEP-JWST: NIRCam-HST multi-band photometry and redshifts for half a million sources in six extragalactic deep fields

arXiv

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arXiv 2024年

作者： Merlin, E. Santini, P. Paris, D. Castellano, M. Fontana, A. Treu, T. Finkelstein, S.L. Dunlop, J.S. Arrabal Haro, P. Bagley, M. Boyett, K. Calabrò, A. Correnti, M. Davis, K. Dickinson, M. Donnan, C.T. Ferguson, H.C. Fortuni, F. Giavalisco, M. Glazebrook, K. Grazian, A. Grogin, N.A. Hathi, N. Hirschmann, M. Kartaltepe, J.S. Kewley, L.J. Kirkpatrick, A. Kocevski, D.D. Koekemoer, A.M. Leung, G. Lotz, J.M. Lucas, R.A. Magee, D.K. Marchesini, D. Mascia, S. McLeod, D.J. McLure, R.J. Nanayakkara, T. Napolitano, L. Nonino, M. Papovich, C. Pentericci, L. Pérez-González, P.G. Pirzkal, N. Ravindranath, S. Roberts-Borsani, G. Somerville, R.S. Trenti, M. Trump, J.R. Vulcani, B. Wang, X. Watson, P.J. Wilkins, S.M. Yang, G. Yung, L.Y.A. INAF - Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone Rome00078 Italy Department of Physics and Astronomy University of California Los Angeles 430 Portola Plaza Los AngelesCA90095 United States Department of Astronomy The University of Texas at Austin AustinTX United States SUPA15 Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom NSF's National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States School of Physics University of Melbourne ParkvilleVIC3010 Australia Australia Space Science Data Center Italian Space Agency Via del Politecnico Roma00133 Italy Department of Physics University of Connecticut 196A Auditorium Road Unit 3046 StorrsCT06269 United States Space Telescope Science Institute BaltimoreMD United States University of Massachusetts 710 N. Pleasant St LGRB-520 AmherstMA01003 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia INAF - Osservatorio Astronomico di Padova Vicolo Osservatorio 5 Padova35122 Italy Institute of Physics Lab for Galaxy Evolution EPFL Observatoire de Sauverny Chemin Pegasi 51 Versoix1290 Switzerland Laboratory for Multiwavelength Astrophysics School of Physics and Astronomy Rochester Institute of Technology 84 Lomb Memorial Drive RochesterNY14623 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Physics and Astronomy University of Kansas LawrenceKS66045 United States Department of Physics and Astronomy Colby College WatervilleME04901 United States Department of Astronomy and Astrophysics UCO/Lick Observatory University of California Santa CruzCA95064 United States Department of Physics & Astronomy Tufts University MA02155 United States Dipartimento di Fisica Università di Roma Sapienza Città Universitaria di Roma - Sap

Aims. We present a set of photometric catalogues primarily aimed at providing the community with a comprehensive database for the study of galaxy populations in the high-redshift Universe. The set gathers data from eight JWST NIRCam observational programs, targeting the Abell 2744 (GLASS-JWST, UNCOVER, DDT2756, and GO3990), EGS (CEERS), COSMOS and UDS (PRIMER), and the GOODS North and South (JADES and NGDEEP) deep fields. This dataset covers a total area of 0.2 sq. degrees. Methods. We obtained photometric estimates by means of well-established techniques, including tailored improvements designed to enhance the performance on the specific dataset. We also included new measurements from HST archival data, spanning 16 bands from 0.44 to 4.44 µm. Results. A grand total of ∼530 thousand sources were detected on stacks of NIRCam 3.56 and 4.44 µm mosaics. We assessed the photometric accuracy by comparing fluxes and colours against archival catalogues. We also provide photometric redshift estimates, statistically validated against a large set of robust spectroscopic data. Conclusions. The catalogues are publicly available on the Astrodeep website. © 2024, CC BY-NC-ND.

关键词： Photometry

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Current and future directions in network biology

arXiv

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arXiv 2023年

作者： Zitnik, Marinka Li, Michelle M. Wells, Aydin Glass, Kimberly Gysi, Deisy Morselli Krishnan, Arjun Murali, T.M. Radivojac, Predrag Roy, Sushmita Baudot, Anaïs Bozdag, Serdar Chen, Danny Z. Cowen, Lenore Devkota, Kapil Gitter, Anthony Gosline, Sara Gu, Pengfei Guzzi, Pietro H. Huang, Heng Jiang, Meng Kesimoglu, Ziynet Nesibe Koyuturk, Mehmet Ma, Jian Pico, Alexander R. Pržulj, Nataša Przytycka, Teresa M. Raphael, Benjamin J. Ritz, Anna Sharan, Roded Shen, Yang Singh, Mona Slonim, Donna K. Tong, Hanghang Yang, Xinan Holly Yoon, Byung-Jun Yu, Haiyuan Milenković, Tijana Department of Biomedical Informatics Harvard University United States Department of Computer Science and Engineering University of Notre Dame United States Lucy Family Institute for Data and Society University of Notre Dame United States Eck Institute for Global Health University of Notre Dame United States Channing Division of Network Medicine Brigham and Women’s Hospital Harvard Medical School United States Department of Statistics Federal University of Paraná Brazil Department of Physics Northeastern University United States Department of Biomedical Informatics University of Colorado United States Department of Computer Science Virginia Tech United States Khoury College of Computer Sciences Northeastern University United States Department of Biostatistics and Medical Informatics University of Wisconsin-Madison United States Wisconsin Institute for Discovery United States Aix Marseille Université INSERM MMG Marseille France Department of Computer Science and Engineering University of North Texas United States Department of Mathematics University of North Texas United States Department of Computer Science Tufts University United States Morgridge Institute for Research United States Pacific Northwest National Laboratory United States Department of Medical and Surgical Sciences University Magna Graecia of Catanzaro Italy Department of Computer Science University of Maryland College Park United States National Center of Biotechnology Information National Library of Medicine National Institutes of Health Department of Computer and Data Sciences Case Western Reserve University United States Computational Biology Department School of Computer Science Carnegie Mellon University United States Institute of Data Science and Biotechnology Gladstone Institutes Department of Computer Science University College London United Kingdom ICREA Catalan Institution for Research and Advanced Studies Spain Department of Computer Science Princeton University United States Departmen

Network biology is an interdisciplinary field bridging computational and biological sciences that has proved pivotal in advancing the understanding of cellular functions and diseases across biological systems and scales. Although the field has been around for two decades, it remains nascent. It has witnessed rapid evolution, accompanied by emerging challenges. These challenges stem from various factors, notably the growing complexity and volume of data together with the increased diversity of data types describing different tiers of biological organization. We discuss prevailing research directions in network biology and highlight areas of inference and comparison of biological networks, multimodal data integration and heterogeneous networks, higher-order network analysis, machine learning on networks, and network-based personalized medicine. Following the overview of recent breakthroughs across these five areas, we offer a perspective on the future directions of network biology. Additionally, we offer insights into scientific communities, educational initiatives, and the importance of fostering diversity within the field. This paper establishes a roadmap for an immediate and long-term vision for network biology. © 2023, CC BY.

关键词： Machine learning

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PANDORA project: photo-nuclear reactions below A=60

arXiv

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arXiv 2022年

作者： Tamii, A. Pellegri, L. Söderström, P.-A. Allard, D. Goriely, S. Inakura, T. Khan, E. Kido, E. Kimura, M. Litvinova, E. Nagataki, S. von Neumann-Cosel, P. Pietralla, N. Shimizu, N. Tsoneva, N. Utsuno, Y. Adachi, S. Bahini, A. Balabanski, D. Baret, B. Bekker, J.A.C. Binda, S.D. Boicu, E. Bracco, A. Brandherm, I. Brezeanu, M. Brummer, J.W. Camera, F. Crespi, F.C.L. Dalal, R. Donaldson, L.M. Fujikawa, Y. Furuno, T. Haoning, H. Honda, Y. Gavrilescu, A. Inoue, A. Isaak, J. Jivan, H. Jones, P.M. Jongile, S. Kawabata, T. Khumalo, T. Kiener, J. Kleemann, J. Kobayashi, N. Koshio, Y. Kuşoğlu, A. Li, K.C.W. Malatji, K.L. Molaeng, R.E. Motoki, H. Murata, M. Netshiya, A. Neveling, R. Niina, R. Oliver, J. Okamoto, S. Ota, S. Papst, O. Parizot, E. Petruse, T. Reen, M.S. Ring, P. Sakanashi, K. Sideras-Haddad, E. Siem, S. Spall, M. Suda, T. Sudo, T. Taniguchi, Y. Tatischeff, V. Utsunomiya, H. Wang, H. Werner, V. Wibowo, H. Wiedeking, M. Wieland, O. Xu, Y. Osaka University Ibaraki567-0047 Japan School of Physics University of the Witwatersrand Johannesburg2050 South Africa iThemba Laboratory for Accelerator Based Sciences Somerset West7129 South Africa Str. Reactorului 30 Bucharest-Măgurele077125 Romania Laboratoire Astroparticule et Cosmologie Université Paris Cité CNRS ParisF-75013 France Institut d’Astronomie et d’Astrophysique Université Libre de Bruxelles Campus de la Plaine CP 226 Brussels1050 Belgium Tokyo Institute of Technology 2-12-1 Ookayama Meguro Tokyo152-8550 Japan IJCLab Université Paris-Saclay CNRS IN2P3 Orsay Cedex91405 France RIKEN 2-1 Hirosawa Saitama Wako351-0198 Japan Department of Physics Hokkaido University Sapporo060-0810 Japan Nuclear Reaction Data Centre Faculty of Science Hokkaido University Sapporo060-0810 Japan Department of Physics Western Michigan University KalamazooMI49008 United States Institut für Kernphysik Technische Universität Darmstadt Darmstadt64289 Germany Center for Computational Sciences University of Tsukuba Tsukuba305-8577 Japan Advanced Science Research Center Japan Atomic Energy Agency Ibaraki Tokai319-1195 Japan Cyclotron and Radioisotope Center Tohoku University 6-3 Aoba Aramaki Aoba Miyagi Sendai980-8578 Japan University of Bucharest Atomistilor 405 Bucharest-Măgurele077125 Romania Dipartimento di Fisica dell’Università degli Studi di Milano MilanoI-20133 Italy INFN Sezione di Milano MilanoI-20133 Italy Guru Jambheshwar University of Science and Technology Hisar125001 India Department of Physics Kyoto University Kitashirakawa Oiwake-Cho Kyoto606-8502 Japan Department of Physics Osaka University Toyonaka Osaka560-0043 Japan Politehnica University of Bucharest Bucharest Romania Department of Physics Faculty of Science Istanbul University Vezneciler/ Istanbul Fatih34134 Turkey Department of Physics University of Oslo P.O. Box 1048 Blindern OsloN-0316 Norway Department of Physics Akal University Punjab

Photo-nuclear reactions of light nuclei below a mass of A = 60 are studied experimentally and theoretically by the PANDORA (Photo-Absorption of Nuclei and Decay Observation for Reactions in Astrophysics) project. Two experimental methods, virtual-photon excitation by proton scattering and real-photo absorption by a high-brilliance gamma-ray beam produced by laser Compton scattering, will be applied to measure the photo-absorption cross sections and the decay branching ratio of each decay channel as a function of the photon energy. Several nuclear models, e.g. anti-symmetrized molecular dynamics, mean-field type models, a large-scale shell model, and ab initio models, will be employed to predict the photo-nuclear reactions. The uncertainty in the model predictions will be evaluated from the discrepancies between the model predictions and the experimental data. The data and the predictions will be implemented in a general reaction calculation code TALYS. The results will be applied to the simulation of the photo-disintegration process of ultra-high-energy cosmic rays in inter-galactic propagation. © 2022, CC BY-NC-ND.

关键词： Gamma rays

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Search for Lorentz-invariance violation with the first KATRIN data

引用

Physical Review D 2023年第8期107卷 082005-082005页

作者： M. Aker D. Batzler A. Beglarian J. Behrens A. Berlev U. Besserer B. Bieringer F. Block S. Bobien B. Bornschein L. Bornschein M. Böttcher T. Brunst T. S. Caldwell R. M. D. Carney S. Chilingaryan W. Choi K. Debowski M. Descher D. Díaz Barrero P. J. Doe O. Dragoun G. Drexlin F. Edzards K. Eitel E. Ellinger R. Engel S. Enomoto A. Felden J. A. Formaggio F. M. Fränkle G. B. Franklin F. Friedel A. Fulst K. Gauda A. S. Gavin W. Gil F. Glück R. Grössle R. Gumbsheimer V. Hannen N. Haußmann K. Helbing S. Hickford R. Hiller D. Hillesheimer D. Hinz T. Höhn T. Houdy A. Huber A. Jansen C. Karl J. Kellerer M. Kleifges M. Klein C. Köhler L. Köllenberger A. Kopmann M. Korzeczek A. Kovalík B. Krasch H. Krause L. La Cascio T. Lasserre T. L. Le O. Lebeda B. Lehnert A. Lokhov M. Machatschek E. Malcherek M. Mark A. Marsteller E. L. Martin C. Melzer S. Mertens J. Mostafa K. Müller H. Neumann S. Niemes P. Oelpmann D. S. Parno A. W. P. Poon J. M. L. Poyato F. Priester J. Ráliš S. Ramachandran R. G. H. Robertson W. Rodejohann C. Rodenbeck M. Röllig C. Röttele M. Ryšavý R. Sack A. Saenz R. Salomon P. Schäfer L. Schimpf M. Schlösser K. Schlösser L. Schlüter S. Schneidewind M. Schrank A. Schwemmer M. Šefčík V. Sibille D. Siegmann M. Slezák F. Spanier M. Steidl M. Sturm H. H. Telle L. A. Thorne T. Thümmler N. Titov I. Tkachev K. Urban K. Valerius D. Vénos A. P. Vizcaya Hernández C. Weinheimer S. Welte J. Wendel M. Wetter J. Wickles C. Wiesinger J. F. Wilkerson J. Wolf S. Wüstling J. Wydra W. Xu S. Zadoroghny G. Zeller Institute for Astroparticle Physics (IAP) Karlsruhe Institute of Technology (KIT) Hermann-von-Helmholtz-Platz 1 76344 Eggenstein-Leopoldshafen Germany Institute for Data Processing and Electronics (IPE) Karlsruhe Institute of Technology (KIT) Hermann-von-Helmholtz-Platz 1 76344 Eggenstein-Leopoldshafen Germany Institute for Nuclear Research of Russian Academy of Sciences 60th October Anniversary Prospect 7a 117312 Moscow Russia Institute for Nuclear Physics University of Münster Wilhelm-Klemm-Str. 9 48149 Münster Germany Institute of Experimental Particle Physics (ETP) Karlsruhe Institute of Technology (KIT) Wolfgang-Gaede-Str. 1 76131 Karlsruhe Germany Institute for Technical Physics (ITEP) Karlsruhe Institute of Technology (KIT) Hermann-von-Helmholtz-Platz 1 76344 Eggenstein-Leopoldshafen Germany Technische Universität München James-Franck-Str. 1 85748 Garching Germany Max-Planck-Institut für Physik Föhringer Ring 6 80805 München Germany Department of Physics and Astronomy University of North Carolina Chapel Hill North Carolina 27599 USA Triangle Universities Nuclear Laboratory Durham North Carolina 27708 USA Institute for Nuclear and Particle Astrophysics and Nuclear Science Division Lawrence Berkeley National Laboratory Berkeley California 94720 USA Department of Physics Faculty of Mathematics and Natural Sciences University of Wuppertal Gaußtraße 20 42119 Wuppertal Germany Departamento de Química Física Aplicada Universidad Autonoma de Madrid Campus de Cantoblanco 28049 Madrid Spain Center for Experimental Nuclear Physics and Astrophysics and Department of Physics University of Washington Seattle Washington 98195 USA Nuclear Physics Institute Czech Academy of Sciences 25068 Řež Czech Republic Laboratory for Nuclear Science Massachusetts Institute of Technology 77 Massachusetts Ave Cambridge Massachusetts 02139 USA Department of Physics Carnegie Mellon University Pittsburgh Pennsylvania 15213 USA IRFU (DPhP & APC) CEA Université Paris-Saclay

Some extensions of the Standard Model of particle physics allow for Lorentz invariance and charge-parity-time invariance violations. In the neutrino sector strong constraints have been set by neutrino-oscillation and time-of-flight experiments. However, some Lorentz-invariance-violating parameters are not accessible via these probes. In this work, we focus on the parameters (aof(3))00, (aof(3))10, and (aof(3))11 which would manifest themselves in a nonisotropic β-decaying source as a sidereal oscillation and an overall shift of the spectral endpoint. Based on the data of the first scientific run of the KATRIN experiment, we set the first 90% confidence-level limit on |(aof(3))11| of <0.9×10−6 GeV to 3.7×10−6 GeV, depending on the phase. Moreover, we derive new constraints on (aof(3))00 and (aof(3))10.

关键词： Particle astrophysics Neutrinos Lorentz symmetry Particle properties Spectroscopy

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ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -XXI. A Large-sample Observational Study of Ethanol and Dimethyl Ether in Hot Cores

arXiv

引用

arXiv 2025年

作者： Kou, Zhiping Li, Xiaohu Qin, Sheng-Li Liu, Tie Mannfors, E. Tang, Xindi Gorai, Prasanta Garay, Guido Das, Swagat R. García, Pablo Bronfman, Leonardo Juvela, M. Chen, Li Liu, Xunchuan Sanhueza, Patricio Peng, Yaping Chen, Long-Fei Zou, Jiahang Yang, Dongting Tóth, L. Viktor Dewangan, Lokesh Liu, Hong-Li Chibueze, James O. Li, Ziyang Xinjiang Astronomical Observatory Chinese Academy of Sciences 150 Science 1-Stree Urumqi Xinjiang830011 China University of Chinese Academy of Sciences Beijing100049 China School of Physics and Astronomy Yunnan University Kunming650091 China Xinjiang Key Laboratory of Radio Astrophysics 150 Science 1-Street Urumqi Xinjiang830011 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Department of Physics University of Helsinki PO Box 64 Helsinki00014 Finland Rosseland Centre for Solar Physics University of Oslo PO Box 1029 Blindern Oslo0315 Norway Institute of Theoretical Astrophysics University of Oslo PO Box 1029 Blindern Oslo0315 Norway Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Department of Earth and Planetary Sciences Institute of Science Tokyo Meguro Tokyo152-8551 Japan National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Astronomical Science SOKENDAI The Graduate University for Advanced Studies 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Physics Faculty of Science Kunming University of Science and Technology Kunming650500 China School of Physics and Electronic Science Guizhou Normal University Guiyang550025 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guiyang550025 China Department of Astronomy Eötvös Loránd University Pázmány Péter sétány 1/A BudapestH-1117 Hungary University of Debrecen Faculty of Science and Technology Egyetemtér 1 DebrecenH-4032 Hungary Physical Research Laboratory Navrangpura Ahmedabad380 009 India Department of Mathematical Sciences University of South Africa Cnr Christian de Wet Rd and Pioneer Avenue Florida Park Roodepoort1709 South Africa Centre for Sp

Hot cores, as a stage of massive star formation, exhibit abundant line emissions of COMs. We present a deep line survey of two isomers of C2H6O: ethanol (C2H5OH;EA), and dimethyl ether (CH3OCH3;DE) as well as their possible precursor CH3OH towards 60 hot cores by using the ALMA 3 mm line observations. EA is detected in 40 hot cores and DE is detected in 59 hot cores. Of these, EA and DE are simultaneously detected in 39 hot cores. We calculate rotation temperatures and column densities of EA and DE by using the XCLASS software. The average rotation temperature of EA is higher than that of DE, whereas the average column density of EA is lower than that of DE. Combined with previous studies of hot cores and hot corinos, we find strong column density correlations among EA and DE (ρ = 0.92), EA and CH3OH (ρ = 0.82), as well as DE and CH3OH (ρ = 0.80). The column density ratios of EA/DE versus the column densities of CH3OH remain nearly constant with values within ~1 order of magnitude. These strong correlations and the stable ratios, suggest that EA, DE, and CH3OH could be chemically linked, with CH3OH potentially serving as a precursor for EA and DE. Compared with chemical models, the three different warm-up timescale models result in the systematic overproduction of EA and the systematic underproduction of DE. Therefore, our large sample observations can provide crucial constraints on chemical models. Copyright © 2025, The Authors. All rights reserved.

关键词： Giant stars

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