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arXiv 2024年

作者： Suess, Katherine A. Weaver, John R. Price, Sedona H. Pan, Richard Wang, Bingjie Bezanson, Rachel Brammer, Gabriel Cutler, Sam E. Labbé, Ivo Leja, Joel Williams, Christina C. Whitaker, Katherine E. Dayal, Pratika de Graaff, Anna Feldmann, Robert Franx, Marijn Fudamoto, Yoshinobu Fujimoto, Seiji Furtak, Lukas J. Goulding, Andy D. Greene, Jenny E. Khullar, Gourav Kokorev, Vasily Kriek, Mariska Lorenz, Brian Marchesini, Danilo Maseda, Michael V. Matthee, Jorryt Miller, Tim B. Mitsuhashi, Ikki Mowla, Lamiya A. Muzzin, Adam Naidu, Rohan P. Nanayakkara, Themiya Nelson, Erica J. Oesch, Pascal A. Setton, David J. Shipley, Heath Smit, Renske Spilker, Justin S. van Dokkum, Pieter Zitrin, Adi Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Department of Astronomy University of Massachusetts AmherstMA01003 United States Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Department of Physics and Astronomy Tufts University 574 Boston Ave. MedfordMA02155 United States Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Copenhagen Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen Denmark Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia NSF’s National Optical-Infrared Astronomy Research Laboratory 950 North Cherry Avenue TucsonAZ85719 United States Denmark Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Department of Astrophysics University of Zurich ZurichCH-8057 Switzerland Leiden Observatory Leiden University P.O.Box 9513 LeidenNL-2300 AA Netherlands Center for Frontier Science Chiba University 1-33 Yayoi-cho Inage-ku Chiba263-8522 Japan Department of Astronomy The University of Texas at Austin AustinTX78712 United States Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Astronomy University of California BerkeleyCA94720 United States Department of Physics & Astronomy Tufts University MA02155 United States Department of Astronomy University of W

In this paper, we describe the "Medium Bands, Mega Science" JWST Cycle 2 survey (JWST-GO-4111) and demonstrate the power of these data to reveal both the spatially-integrated and spatially-resolved properties of galaxies from the local universe to the era of cosmic dawn. Executed in November 2023, MegaScience obtained ∼ 30arcmin2 of deep multiband NIRCam imaging centered on the z ∼ 0.3 Abell 2744 cluster, including eleven medium-band filters and the two shortest-wavelength broad-band filters, F070W and F090W. Together, MegaScience and the UNCOVER Cycle 1 treasury program provide a complete set of deep (∼ 28−30magAB) images in all NIRCam medium- and broad-band filters. This unique dataset allows us to precisely constrain photometric redshifts, map stellar populations and dust attenuation for large samples of distant galaxies, and examine the connection between galaxy structures and formation histories. MegaScience also includes ∼ 17 arcmin2 of NIRISS parallel imaging in two broad-band and four medium-band filters from 0.9 − 4.8µm, expanding the footprint where robust spectral energy distribution (SED) fitting is possible. We provide example SEDs and multiband cutouts at a variety of redshifts, and use a catalog of JWST spectroscopic redshifts to show that MegaScience improves both the scatter and catastrophic outlier rate of photometric redshifts by factors of 2-3. Additionally, we demonstrate the spatially-resolved science enabled by MegaScience by presenting maps of the [OIII] line emission and continuum emission in three spectroscopically-confirmed z > 6 galaxies. We show that line emission in reionization-era galaxies can be clumpy, extended, and spatially offset from continuum emission, implying that galaxy assembly histories are complex even at these early epochs. We publicly release fully reduced mosaics and photometric catalogs for both the NIRCam primary and NIRISS parallel fields (***/megascience). Copyright © 2024, The Authors. All right

关键词： Galaxies

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The TESS-Keck Survey XXI: 13 New Planets and Homogeneous Properties for 21 Subgiant Systems

arXiv

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arXiv 2024年

作者： Chontos, Ashley Huber, Daniel Grunblatt, Samuel K. Saunders, Nicholas Winn, Joshua N. McCormack, Mason Knudstrup, Emil Albrecht, Simon H. Crossfield, Ian J.M. Rodriguez, Joseph E. Ciardi, David R. Collins, Karen A. Jenkins, Jon M. Bieryla, Allyson Batalha, Natalie M. Beard, Corey Dai, Fei Dalba, Paul A. Fetherolf, Tara Giacalone, Steven Hill, Michelle L. Howard, Andrew W. Isaacson, Howard Kane, Stephen R. Lubin, Jack Macdougall, Mason G. Močnik, Teo Akana Murphy, Joseph M. Petigura, Erik A. Pidhorodetska, Daria Polanski, Alex S. Robertson, Paul Rubenzahl, Ryan A. Turtelboom, Emma V. Weiss, Lauren M. van Zandt, Judah Ricker, George R. Vanderspek, Roland Latham, David W. Seager, Sara Quinn, Samuel N. Shporer, Avi Eisner, Nora L. Goeke, Robert F. Levine, Alan M. Ting, Eric B. Howell, Steve Schlieder, Joshua E. Benni, Paul Boyle, Andrew W. Gan, Tianjun Girardin, Eric Gonzalez, Erica Gregorio, Joao Horne, Keith Livingston, John Lund, Michael B. Mann, Christopher R. Massey, Bob Matthews, Elisabeth C. McLeod, Kim K. Palle, Enric Popowicz, Adam Relles, Howard M. Schwarz, Richard P. Sefako, Ramotholo Srdoc, Gregor Tan, Thiam-Guan Wang, Gavin Ziegler, Carl Institute for Astronomy University of Hawai'i 2680 Woodlawn Drive HonoluluHI96822 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States School of Physics University of Sydney NSW2006 Australia Department of Physics and Astronomy Johns Hopkins University 3400 N Charles St BaltimoreMD21218 United States Department of Astronomy & Astrophysics University of Chicago ChicagoIL60637 United States Department of Space Earth and Environment Chalmers University of Technology Gothenburg412 93 Sweden Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Department of Physics & Astronomy University of Kansas 1251 Wescoe Hall Dr. 1082 Malott LawrenceKS66045 United States Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Caltech/IPAC-NASA Exoplanet Science Institute 770 S. Wilson Avenue PasadenaCA91106 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States NASA Ames Research Center Moffett FieldCA94035 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95060 United States Department of Physics & Astronomy University of California Irvine IrvineCA92697 United States Division of Geological and Planetary Sciences 1200 E California Blvd PasadenaCA91125 United States Department of Astronomy California Institute of Technology PasadenaCA91125 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Department of Physics California State University San MarcosCA92096 United States Department of Earth and Planetary Sciences University of California RiversideCA92521 United States Department of Astronomy University of California Berkeley BerkeleyCA94720 United States

We present a dedicated transit and radial velocity survey of planets orbiting subgiant stars observed by the TESS Mission. Using ∼16 nights on Keck/HIRES, we confirm and characterize 12 new transiting planets - TOI-329 b, HD 39688 b (TOI-480), TOI-603 b, TOI-1199 b, TOI-1294 b, TOI-1439 b, TOI-1605 b, TOI-1828 b, HD 148193 b (TOI-1836), TOI-1885 b, HD 83342 b (TOI-1898), TOI-2019 b - and provide updated properties for 9 previously confirmed TESS subgiant systems (TOI-197, TOI-954, TOI-1181, TOI-1296, TOI-1298, TOI-1601, TOI-1736, TOI-1842, TOI-2145). We also report the discovery of an outer, non-transiting planet, TOI-1294 (Equation presented) and three additional stars with long-term RV trends. We find that at least 19±8% of subgiants in our sample of 21 stars have outer companions, comparable to main-sequence stars. We perform a homogeneous analysis of the stars and planets in the sample, with median uncertainties of 3%, 8% and 15% for planet radii, masses and ages, doubling the number of known planets orbiting subgiant stars with bulk densities measured to better than 10%. We observe a dearth of giant planets around evolved stars with short orbital periods, consistent with tidal dissipation theories that predict the rapid inspiral of planets as their host stars leave the main sequence. We note the possible evidence for two distinct classes of hot Jupiter populations, indicating multiple formation channels to explain the observed distributions around evolved stars. Finally, continued RV monitoring of planets in this sample will provide a more comprehensive understanding of demographics for evolved planetary systems. © 2024, CC BY.

关键词： Planets

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An Extremely Deep Rubin Survey to Explore the Extended Kuiper Belt and Identify Objects Observable by New Horizons

arXiv

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arXiv 2025年

作者： Kavelaars, J.J. Buie, Marc W. Fraser, Wesley C. Peltier, Lowell Benecchi, Susan D. Porter, Simon B. Verbiscer, Anne J. Gerdes, David W. Napier, Kevin J. Murtagh, Joseph Ito, Takashi Singer, Kelsi N. Stern, S. Alan Terai, Tsuyoshi Yoshida, Fumi Bannister, Michele T. Bernardinelli, Pedro H. Bernstein, Gary M. Chandler, Colin Orion Gladman, Brett Jones, Lynne Petit, Jean-Marc Schwamb, Megan E. Brandt, Pontus C. Parker, Joel W. National Research Council of Canada Herzberg Astronomy and Astrophysics Research Centre 5071 W. Saanich Rd. VictoriaBCV9E 2E7 Canada Department of Physics and Astronomy University of Victoria Elliott Building 3800 Finnerty Road VictoriaBCV8P 5C2 Canada Department of Physics & Astronomy University of British Columbia 6224 Agricultural Road VancouverBCV6T 1Z1 Canada Southwest Research Institute 1301 Walnut St. Suite 400 BoulderCO80302 United States Planetary Science Institute 1700 East Fort Lowell Suite 106 TucsonAZ85719 United States Department of Astronomy University of Virginia P.O. Box 400325 CharlottesvilleVA22904-4325 United States Department of Physics University of Michigan Ann ArborMI48109 United States Department of Astronomy University of Michigan Ann ArborMI48109 United States Michigan Institute for Data Science University of Michigan Ann ArborMI48109 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast BelfastBT7 1NN United Kingdom Center for Computational Astrophysics National Astronomical Observatory of Japan Osawa 2-21-1 Mitaka Tokyo181-8588 Japan Subaru Telescope National Astronomical Observatory of Japan 650 North A‘ohoku Place HiloHI96720 United States University of Occupational and Environmental Health 1-1 Iseigaoka Yahata Kitakyushu807-8555 Japan Planetary Exploration Research Center Chiba Institute of Technology 2-17-1 Tsudanuma Narashino Chiba275-0016 Japan School of Physical and Chemical Sciences — Te Kura Matū University of Canterbury Private Bag 4800 Christchurch8140 New Zealand DiRAC Institute The Department of Astronomy University of Washington Seattle United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Astronomy and Planetary Science Northern Arizona University PO Box 6010

A proposed Vera C. Rubin Observatory Deep Drilling micro-survey of the Kuiper Belt will investigate key properties of the distant solar system. Utilizing 30 hours of Rubin time across six 5-hour visits over one year starting in summer 2026, the survey aims to discover and determine orbits for up to 730 Kuiper Belt Objects (KBOs) to an r-magnitude of 27.5. These discoveries will enable precise characterization of the KBO size distribution, which is critical for understanding planetesimal formation. By aligning the survey field with NASA’s New Horizons spacecraft trajectory, the micro-survey will facilitate discoveries for the mission operating in the Kuiper Belt. Modeling based on the Outer Solar System Origin Survey (OSSOS) predicts at least 12 distant KBOs observable with the New Horizons LOng Range Reconnaissance Imager (LORRI) and approximately three objects within 1 au of the spacecraft, allowing higher-resolution observations than Earth-based facilities. LORRI’s high solar phase angle monitoring will reveal these objects’ surface properties and shapes, potentially identifying contact binaries and orbit-class surface correlations. The survey could identify a KBO suitable for a future spacecraft flyby. The survey’s size, depth, and cadence design will deliver transformative measurements of the Kuiper Belt’s size distribution and rotational properties across distance, size, and orbital class. Additionally, the high stellar density in the survey field also offers synergies with transiting exoplanet studies. © 2025, CC BY.

关键词： NASA

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DeePMD-kit v3: A Multiple-Backend Framework for Machine Learning Potentials

arXiv

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arXiv 2025年

作者： Zeng, Jinzhe Zhang, Duo Peng, Anyang Zhang, Xiangyu He, Sensen Wang, Yan Liu, Xinzijian Bi, Hangrui Li, Yifan Cai, Chun Zhang, Chengqian Du, Yiming Zhu, Jia-Xin Mo, Pinghui Huang, Zhengtao Zeng, Qiyu Shi, Shaochen Qin, Xuejian Yu, Zhaoxi Luo, Chenxing Ding, Ye Liu, Yun-Pei Shi, Ruosong Wang, Zhenyu Bore, Sigbjørn Løland Chang, Junhan Deng, Zhe Ding, Zhaohan Han, Siyuan Jiang, Wanrun Ke, Guolin Liu, Zhaoqing Lu, Denghui Muraoka, Koki Oliaei, Hananeh Singh, Anurag Kumar Que, Haohui Xu, Weihong Xu, Zhangmancang Zhuang, Yong-Bin Dai, Jiayu Giese, Timothy J. Jia, Weile Xu, Ben York, Darrin M. Zhang, Linfeng Wang, Han School of Artificial Intelligence and Data Science Unversity of Science and Technology of China Hefei China AI for Science Institute Beijing100080 China DP Technology Beijing100080 China Academy for Advanced Interdisciplinary Studies Peking University Beijing100871 China State Key Lab of Processors Institute of Computing Technology Chinese Academy of Sciences Beijing100871 China University of Chinese Academy of Sciences Beijing China Baidu Inc. Beijing China Department of Computer Science University of Toronto TorontoON Canada Department of Chemistry Princeton University PrincetonNJ08540 United States University of Chinese Academy of Sciences Beijing100871 China State Key Laboratory of Physical Chemistry of Solid Surfaces iChEM College of Chemistry and Chemical Engineering Xiamen University Xiamen361005 China College of Integrated Circuits Hunan University Changsha410082 China State Key Laboratory of Advanced Technology for Materials Synthesis and Processing Center for Smart Materials and Device Integration School of Material Science and Engineering Wuhan University of Technology Wuhan430070 China College of Science National University of Defense Technology Changsha410073 China Hunan Key Laboratory of Extreme Matter and Applications National University of Defense Technology Changsha410073 China ByteDance Research Beijing100098 China Ningbo Institute of Materials Technology and Engineering Chinese Academy of Sciences Ningbo315201 China College of Materials Science and Opto-Electronic Technology University of Chinese Academy of Sciences Beijing100049 China Key Laboratory of Theoretical and Computational Photochemistry of Ministry of Education College of Chemistry Beijing Normal University Beijing100875 China Department of Geosciences Princeton University PrincetonNJ08544 United States Department of Applied Physics and Applied Mathematics Columbia University New YorkNY10027 United States IKKEM Fujian Xiamen361005 China Graduate

In recent years, machine learning potentials (MLPs) have become indispensable tools in physics, chemistry, and materials science, driving the development of software packages for molecular dynamics (MD) simulations and related applications. These packages, typically built on specific machine learning frameworks such as TensorFlow, PyTorch, or JAX, face integration challenges when advanced applications demand communication across different frameworks. The previous TensorFlow-based implementation of DeePMD-kit exemplified these limitations. In this work, we introduce DeePMD-kit version 3, a significant update featuring a multi-backend framework that supports TensorFlow, PyTorch, JAX, and PaddlePaddle backends, and demonstrate the versatility of this architecture through the integration of other MLPs packages and of Differentiable Molecular Force Field. This architecture allows seamless backend switching with minimal modifications, enabling users and developers to integrate DeePMD-kit with other packages using different machine learning frameworks. This innovation facilitates the development of more complex and interoperable workflows, paving the way for broader applications of MLPs in scientific research. Copyright © 2025, The Authors. All rights reserved.

关键词： Molecular dynamics

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UNCOVER NIRSpec/PRISM Spectroscopy Unveils Evidence of Early Core Formation in a Massive, Centrally Dusty Quiescent Galaxy at zspec = 3.97

arXiv

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arXiv 2024年

作者： Setton, David J. Khullar, Gourav Miller, Tim B. Bezanson, Rachel Greene, Jenny E. Suess, Katherine A. Whitaker, Katherine E. Antwi-Danso, Jacqueline Atek, Hakim Brammer, Gabriel Cutler, Sam E. Dayal, Pratika Feldmann, Robert Fujimoto, Seiji Furtak, Lukas J. Glazebrook, Karl Goulding, Andy D. Kokorev, Vasily Labbe, Ivo Leja, Joel Ma, Yilun Marchesini, Danilo Nanayakkara, Themiya Pan, Richard Price, Sedona H. Siegel, Jared C. Shipley, Heath Weaver, John R. van Dokkum, Pieter Wang, Bingjie Williams, Christina C. Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Northwestern University 1800 Sherman Ave EvanstonIL60201 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Department of Astronomy University of Massachusetts AmherstMA01003 United States Denmark David A. Dunlap Department of Astronomy & Astrophysics University of Toronto 50 St George Street TorontoONM5S 3H4 Canada Dunlap Institute for Astronomy & Astrophysics University of Toronto 50 St George Street TorontoONM5S 3H4 Canada Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Department of Astrophysics University of Zurich Winterthurerstrasse 190 Zurich8057 Switzerland Department of Astronomy The University of Texas at Austin AustinTX78712 United States Physics Department Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Physics & Astronomy Tufts University MA02155 United States NSF Graduate Research Fellow Department of Physi

We report the spectroscopic confirmation of a massive (log(M/M) = 10.34±00.0706), HST-dark (mF150W−mF444W = 3.6) quiescent galaxy at zspec = 3.97 in the UNCOVER survey. NIRSpec/PRISM spectroscopy and a non-detection in deep ALMA imaging surprisingly reveals that the galaxy is consistent with a low (−1) star formation rate despite evidence for moderate dust attenuation. The F444W image is well modeled with a two component Sérsic fit that favors a compact, re ∼ 200 pc, n ∼ 2.9 component and a more extended, re ∼ 1.6 kpc, n ∼ 1.7 component. The galaxy exhibits strong color gradients: the inner regions are significantly redder than the outskirts. Spectral energy distribution models that reproduce both the red colors and low star formation rate in the center of UNCOVER 18407 require both significant (Av ∼ 1.4 mag) dust attenuation and a stellar mass-weighted age of 900 Myr, implying 50% of the stars in the core already formed by z = 7.5. Using spatially resolved annular mass-to-light measurements enabled by the galaxy’s moderate magnification (µ = 2.12±00.0501) to reconstruct a radial mass profile from the best-fitting two-component Sérsic model, we infer a total mass-weighted reff = 0.72±00.1511 kpc and log(Σ1kpc [M/kpc2]) = 9.61±00.0810. The early formation of a dense, low star formation rate, and dusty core embedded in a less attenuated stellar envelope suggests an evolutionary link between the earliest-forming massive galaxies and their elliptical descendants. Furthermore, the disparity between the global, integrated dust properties and the spatially resolved gradients highlights the importance of accounting for radially varying stellar populations when characterizing the early growth of galaxy structure. © 2024, CC BY.

关键词： Galaxies

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Dense matter with eXTP

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Science China(physics,Mechanics & Astronomy) 2019年第2期62卷 28-44页

作者： Anna L.Watts WenFei Yu Juri Poutanen Shu Zhang Sudip Bhattacharyya Slavko Bogdanov Long Ji Alessandro Patruno Thomas E.Riley Pavel Bakala Altan Baykal Federico Bernardini Ignazio Bombaci Edward Brown Yuri Cavecchi Deepto Chakrabarty Jér?me Chenevez Nathalie Degenaar Melania Del Santo Tiziana Di Salvo Victor Doroshenko Maurizio Falanga Robert D.Ferdman Marco Feroci Angelo F.Gambino MingYu Ge Svenja K.Greif Sebastien Guillot Can Gungor Dieter H.Hartmann Kai Hebeler Alexander Heger Jeroen Homan Rosario Iaria Jean in 't Zand Oleg Kargaltsev Aleksi KurkelaTheoretical physics Department CERN XiaoYu Lai Ang Li XiangDong Li ZhaoSheng Li Manuel Linares FangJun Lu Simin Mahmoodifar Mariano Méndez M.Coleman Miller Sharon Morsink Joonas N?ttil? Andrea Possenti Chanda Prescod-Weinstein JinLu Qu Alessandro Riggio Tuomo Salmi Andrea Sanna Andrea Santangelo Hendrik Schatz Achim Schwenk LiMing Song Eva?rámková Benjamin Stappers Holger Stiele Tod Strohmayer Ingo Tews Laura Tolos Gabriel T?r?k David Tsang Martin Urbanec Andrea Vacchi RenXin Xu YuPeng Xu Silvia Zane GuoBao Zhang ShuangNan Zhang WenDa Zhang ShiJie Zheng Xia Zhou Anton Pannekoek Institute for Astronomy University of Amsterdam Shanghai Astronomical Observatory Tuorla Observatory Department of Physics and Astronomy University of Turku Nordita KTH Royal Institute of Technology and Stockholm University Institute of High Energy Physics Chinese Academy Sciences Tata Institute of Fundamental Research Columbia Astrophysics Laboratory Columbia University Institut für Astronomie und Astrophysik Tübingen Universit?t Tübingen Leiden Observatory Leiden University Research Center for Computational Physics and Data Processing Silesian University in Opava Physics Department Middle East Technical University INAF Osservatorio Astronomico di Roma New York University Abu Dhabi Dipartimento di Fisica Enrico Fermi University of Pisa INFN Italian National Institute for Nuclear Physics Department of Physics and Astronomy Michigan State University Department of Astrophysical Sciences Princeton University Mathematical Sciences and STAG Research Centre University of Southampton MIT Kavli Institute for Astrophysics and Space Research DTU Space Technical University of Denmark INAF/IASF Palermo via Ugo La Malfa 153 Universita degli Studi di Palermo Dipartimento di Fisica e Chimica International Space Science Institute (ISSI) Faculty of Science University of East Anglia INAF Istituto di Astrofisica e Planetologie Spaziali Institut für Kernphysik Technische Universit?t Darmstadt ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH Instituto de Astrof'?sica Pontificia Universidad Católica de Chile Department of Physics & Astronomy Kinard Lab of Physics Clemson University School of Physics and Astronomy Monash University SRON Netherlands Institute for Space Research Department of Physics The George Washington University Faculty of Science and Technology University of Stavanger School of Physics and Mechanical & Electrical Engineering Hubei University of Education Department of Astronomy Xiamen University (Haiyun Campus) School of Astronomy and Space

In this White Paper we present the potential of the Enhanced X-ray Timing and Polarimetry(eXTP) mission for determining the nature of dense matter; neutron star cores host an extreme density regime which cannot be replicated in a terrestrial laboratory. The tightest statistical constraints on the dense matter equation of state will come from pulse profile modelling of accretion-powered pulsars, burst oscillation sources, and rotation-powered pulsars. Additional constraints will derive from spin measurements, burst spectra, and properties of the accretion flows in the vicinity of the neutron star. Under development by an international Consortium led by the institute of High Energy physics of the Chinese Academy of Sciences, the eXTP mission is expected to be launched in the mid 2020 s.

关键词： neutron X-rays dense matter equation of state

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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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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

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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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Three-dimensional general relativistic Poynting-Robertson effect. III. Static and nonspherical quadrupolar massive source

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Physical Review D 2020年第12期101卷 124031-124031页

作者： Vittorio De Falco Pavel Bakala Maurizio Falanga M. R. Štefánik Observatory and Planetarium Sládkovičova 41 920 01 Hlohovec Slovak Republic Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 CZ-74601 Opava Czech Republic International Space Science Institute Hallerstrasse 6 3012 Bern Switzerland

We investigate the three-dimensional (3D) motion of a test particle in the gravitational field generated by a nonspherical compact object endowed with a mass quadrupole moment, described by the Erez-Rosen metric, and a radiation field, including the general relativistic Poynting-Robertson (PR) effect, coming from a rigidly rotating spherical emitting source located outside of the compact object. We derive the equations of motion for test particles influenced by such radiation field, recovering the two-dimensional (2D) description, and the weak-field approximation. This dynamical system admits the existence of a critical hypersurface, region where gravitational and radiation forces balance. Selected test particle orbits for different set of input parameters are displayed. The possible configurations on the critical hypersurfaces can be either latitudinal drift toward the equatorial ring or suspended orbits. We discuss about the existence of multiple hypersurface solutions through a simple method to perform the calculations. We graphically prove also that the critical hypersurfaces are stable configurations within the Lyapunov theory.

关键词： General relativity Gravitation Classical black holes Astrophysical electromagnetic fields Numerical simulations in gravitation & astrophysics

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A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots

arXiv

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arXiv 2025年

作者： Setton, David J. Greene, Jenny E. Spilker, Justin S. Williams, Christina C. Labbé, Ivo Ma, Yilun Wang, Bingjie Whitaker, Katherine E. Leja, Joel de Graaff, Anna Alberts, Stacey Bezanson, Rachel Boogaard, Leindert A. Brammer, Gabriel Cutler, Sam E. Cleri, Nikko J. Cooper, Olivia R. Dayal, Pratika Fujimoto, Seiji Furtak, Lukas J. Goulding, Andy D. Hirschmann, Michaela Kokorev, Vasily Maseda, Michael V. McConachie, Ian Matthee, Jorryt Miller, Tim B. Naidu, Rohan P. Oesch, Pascal A. Pan, Richard Price, Sedona H. Suess, Katherine A. Weaver, John R. Xiao, Mengyuan Zhang, Yunchong Zitrin, Adi Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Physics and Astronomy George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University 4242 TAMU College StationTX77843-4242 United States NSF’s National Optical-Infrared Astronomy Research Laboratory TucsonAZ85719 United States Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and The Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Astronomy University of Massachusetts AmherstMA01003 United States Denmark Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Leiden Observatory Leiden University PO Box 9513 LeidenNL-2300 RA Netherlands Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark The University of Texas at Austin 2515 Speedway Boulevard Stop C1400 AustinTX78712 United States Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Department of Astronomy The University of Texas at Austin AustinTX78712 United States David A. Dunlap Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada Department of Physics Ben-Gurion University of The Negev P.O. Box 653 Be’er-Sheva84105 Israel Institute of Physics GalSpec laboratory EPFL Observatory of Geneva Chemin Pegasi 51 Versoix1290

Luminous broad Hα emission and red rest-optical SEDs are the hallmark of compact Little Red Dots (LRDs), implying highly attenuated dusty starbursts and/or obscured active galactic nuclei. However, the lack of observed FIR emission has proved difficult to reconcile with the implied attenuated luminosity in these models. Here, we utilize deep new ALMA imaging, new and existing JWST/MIRI imaging, and archival Spitzer/Herschel imaging of two of the rest-optically brightest LRDs (z = 3.1 and z = 4.47) to place the strongest constraints on the IR luminosity in LRDs to date. The detections at λrest = 1 − 4 µm imply flat slopes in the rest-IR, ruling out a contribution from hot (T 500 K) dust. Similarly, FIR non-detections rule out any appreciable cold (T 75 K) dust component. Assuming energy balance, these observations are inconsistent with the typical FIR dust emission of dusty starbursts and quasar torii, which usually show a mixture of cold and hot dust. Additionally, our [CII] non-detections rule out typical dusty starbursts. We compute empirical maximum IR SEDs and find that both LRDs must have log(LIR/L☉) 12.2 at the 3σ level. These limits are in tension with the predictions of rest-optical spectrophotometric fits, be they galaxy only, AGN only, or composite. It is unlikely that LRDs are highly dust-reddened intrinsically blue sources with a dust temperature distribution that conspires to avoid current observing facilities. Rather, we favor an intrinsically redder LRD SED model that alleviates the need for strong dust attenuation. © 2025, CC BY.

关键词： Active Galactic Nuclei

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