检索结果-内蒙古大学图书馆

arXiv 2024年

作者： Ma, Yilun Greene, Jenny E. Setton, David J. Volonteri, Marta Leja, Joel Wang, Bingjie Bezanson, Rachel Brammer, Gabriel Cutler, Sam E. Dayal, Pratika van Dokkum, Pieter Furtak, Lukas J. Glazebrook, Karl Goulding, Andy D. de Graaff, Anna Kokorev, Vasily Labbe, Ivo Pan, Richard Price, Sedona H. Weaver, John R. Williams, Christina C. Whitaker, Katherine E. Zitrin, Adi Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Institut d’Astrophysique de Paris Sorbonne Université CNRS UMR 7095 98 bis bd Arago ParisF-75014 France 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 and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Astronomy University of Massachusetts AmherstMA01003 United States Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Department of Astronomy Yale University New HavenCT06511 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 Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Department of Astronomy The University of Texas at Austin AustinTX78712 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Physics and Astronomy Tufts University 574 Boston Ave MedfordMA02155 United States NSF National Optical-Infrared Astronomy Research Laboratory 950 North Cherry Avenue TucsonAZ85719 United States Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel

JWST has revealed an abundance of compact, red objects at z ≈ 5 − 8 dubbed "little red dots" (LRDs), whose SEDs display a faint blue UV continuum followed by a steep rise in the optical. Despite extensive study of their characteristic V-shaped SEDs, the nature of LRDs remains unknown. We present a new analysis of the NIRSpec/PRISM spectrum of A2744-QSO1, a triply imaged LRD at z = 7.04 from the UNCOVER survey. The spectrum shows a strong Balmer break and broad Balmer emission lines, both of which are difficult to explain with models invoking exclusively AGN or stellar contributions. Our fiducial model decomposes the spectrum into a post-starburst galaxy dominating the UV-optical continuum and a reddened AGN being sub-dominant at all wavelength and contributing at ∼ 20% level. However, this model infers a stellar mass of M✶ ≈ 4 × 109 M☉ within a radius of re © 2024, CC BY.

关键词： Stars

来源：评论

学校读者我要写书评

暂无评论

Cosmogenic background simulations for the DARWIN observatory at different underground locations

arXiv

引用

arXiv 2023年

作者： Adrover, M. Althueser, L. Andrieu, B. Angelino, E. Angevaare, J.R. Antunovic, B. Aprile, E. Babicz, M. Bajpai, D. Barberio, E. Baudis, L. Bazyk, M. Bell, N. Bellagamba, L. Biondi, R. Biondi, Y. Bismark, A. Boehm, C. Breskin, A. Brookes, E.J. Brown, A. Bruno, G. Budnik, R. Capelli, C. Cardoso, J.M.R. Chauvin, A. Cimental Chavez, A.P. Colijn, A.P. Conrad, J. Jose. Cuenca-García, J. Andrea, V.D. Decowski, M.P. Deisting, A. Di Gangi, P. Diglio, S. Doerenkamp, M. Drexlin, G. Eitel, K. Elykov, A. Engel, R. Farrell, S. Ferella, A.D. Ferrari, C. Fischer, H. Flierman, M. Fulgione, W. Gaemers, P. Gaior, R. Galloway, M. Garroum, N. Ghosh, S. Girard, F. Glade-Beucke, R. Glück, F. Grandi, L. Grigat, J. Größle, R. Guan, H. Guida, M. Hammann, R. Hannen, V. Hansmann-Menzemer, S. Hargittai, N. Hasegawa, T. Hils, C. Higuera, A. Hiraoka, K. Hoetzsch, L. Iacovacci, M. Itow, Y. Jakob, J. Jörg, F. Kara, M. Kavrigin, P. Kazama, S. Keller, M. Kilminster, B. Kleifges, M. Kobayashi, M. Kopec, A. von Krosigk, B. Kuger, F. Landsman, H. Lang, R.F. Li, I. Li, S. Liang, S. Lindemann, S. Lindner, M. Lombardi, F. Loizeau, J. Luce, T. Ma, Y. Macolino, C. Mahlstedt, J. Mancuso, A. Marrodán Undagoitia, T. Lopes, J.A.M. Marignetti, F. Martens, K. Masbou, J. Mastroianni, S. Milutinovic, S. Miuchi, K. Miyata, R. Molinario, A. Monteiro, C.M.B. Morå, K. Morteau, E. Mosbacher, Y. Müller, J. Murra, M. Newstead, J.L. Ni, K. Oberlack, U.G. Ostrovskiy, I. Paetsch, B. Pandurovic, M. Pellegrini, Q. Peres, R. Pienaar, J. Pierre, M. Piotter, M. Plante, G. Pollmann, T.R. Principe, L. Qi, J. Qin, J. Rajado Silva, M. Ramírez García, D. Razeto, A. Sakamoto, S. Sanchez, L. Sanchez-Lucas, P. dos Santos, J.M.F. Sartorelli, G. Scaffidi, A. Schulte, P. Schultz-Coulon, H.-C. Schulze Eißing, H. Schumann, M. Scotto Lavina, L. Selvi, M. Semeria, F. Shagin, P. Sharma, S. Shen, W. Silva, M. Simgen, H. Singh, R. Solmaz, M. Stanley, O. Steidl, M. Tan, P.-L. Terliuk, A. Physik-Institut University of Zürich Zürich8057 Switzerland Institut für Kernphysik Westfälische Wilhelms-Universität Münster Münster48149 Germany LPNHE Sorbonne Université CNRS IN2P3 Paris75005 France INAF-Astrophysical Observatory of Torino Department of Physics University of Torino INFN-Torino Torino10125 Italy Nikhef The University of Amsterdam Science Park Amsterdam1098XG Netherlands Vinca Institute of Nuclear Science University of Belgrade Mihajla Petrovica Alasa 12-14 Belgrade Serbia Physics Department Columbia University New YorkNY10027 United States New York University Abu Dhabi Center for Astro Particle and Planetary Physics Abu Dhabi United Arab Emirates Department of Physics and Astronomy University of Alabama TuscaloosaAL35487 United States Institute for Data Processing and Electronics Karlsruhe Institute of Technology Karlsruhe76021 Germany ARC Centre of Excellence for Dark Matter Particle Physics School of Physics The University of Melbourne VIC3010 Australia SUBATECH IMT Atlantique CNRS IN2P3 Université de Nantes Nantes44307 France Department of Physics and Astronomy University of Bologna INFN-Bologna Bologna40126 Italy Max-Planck-Institut für Kernphysik Heidelberg69117 Germany Institute for Astroparticle Physics Karlsruhe Institute of Technology Karlsruhe76021 Germany School of Physics The University of Sydney NSW 2006 Camperdown Sydney Australia Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot7610001 Israel Physikalisches Institut Universität Freiburg Freiburg79104 Germany LIBPhys Department of Physics University of Coimbra Coimbra3004-516 Portugal Physikalisches Institut Universität Heidelberg Heidelberg Germany Oskar Klein Centre Department of Physics Stockholm University AlbaNova StockholmSE-10691 Sweden INFN-Laboratori Nazionali del Gran Sasso Gran Sasso Science Institute L’Aquila67100 Italy Institut für Physik & Exzellenzcluster PRISMA+ Johannes Gutenber

Xenon dual-phase time projections chambers (TPCs) have proven to be a successful technology in studying physical phenomena that require low-background conditions. With 40t of liquid xenon (LXe) in the TPC baseline design, DARWIN will have a high sensitivity for the detection of particle dark matter, neutrinoless double beta decay (0νββ), and axion-like particles (ALPs). Although cosmic muons are a source of background that cannot be entirely eliminated, they may be greatly diminished by placing the detector deep underground. In this study, we used Monte Carlo simulations to model the cosmogenic background expected for the DARWIN observatory at four underground laboratories: Laboratori Nazionali del Gran Sasso (LNGS), Sanford Underground research Facility (SURF), Laboratoire Souterrain de Modane (LSM) and SNOLAB. We determine the production rates of unstable xenon isotopes and tritium due to muon-included neutron fluxes and muon-induced spallation. These are expected to represent the dominant contributions to cosmogenic backgrounds and thus the most relevant for site selection. Copyright © 2023, The Authors. All rights reserved.

关键词： Observatories

来源：评论

学校读者我要写书评

暂无评论

TOI-2005b: An Eccentric Warm Jupiter in Spin-Orbit Alignment

arXiv

引用

arXiv 2025年

作者： Bieryla, Allyson Dong, Jiayin Zhou, George Eastman, Jason D. Mayorga, L.C. Latham, David W. Carter, Brad Huang, Chelsea X. Quinn, Samuel N. Collins, Karen A. Abe, Lyu Beletsky, Yuri Brahm, Rafael Colón, Knicole D. Essack, Zahra Guillot, Tristan Henning, Thomas Hobson, Melissa J. Horne, Keith Jenkins, Jon M. Jones, Matías I. Jordán, Andrés Osip, David Ricker, George R. Rodriguez, Joseph E. Schulte, Jack Schwarz, Richard P. Seager, Sara Shporer, Avi Suarez, Olga Tan, Thiam-Guan Ting, Eric B. Triaud, Amaury Vanderburg, Andrew Villaseñor, Jesus Noel Vowell, Noah Watkins, Cristilyn N. Winn, Joshua N. Ziegler, Carl Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States University of Southern Queensland Centre for Astrophysics West Street ToowoombaQLD4350 Australia Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States Department of Astronomy University of Illinois at Urbana-Champaign UrbanaIL61801 United States The Johns Hopkins University Applied Physics Laboratory 11100 Johns Hopkins Rd LaurelMD20723 United States Observatoire de la Côte d’Azur UniCA Laboratoire Lagrange CNRS UMR 7293 CS 34229 06304 Nice cedex 4 France Las Campanas Observatory Carnegie Institution for Science Colina El Pino Casilla La Serena601 Chile Facultad de Ingeniería y Ciencias Universidad Adolfo Ibáñez Av. Diagonal las Torres 2640 Santiago Peñalolén Chile Millennium Institute for Astrophysics Chile Data Observatory Foundation Chile GreenbeltMD20771 United States Department of Physics and Astronomy The University of New Mexico 210 Yale Blvd NE AlbuquerqueNM87106 United States Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany SUPA Physics and Astronomy University of St. Andrews Fife ScotlandKY16 9SS United Kingdom NASA Ames Research Center Moffett FieldCA94035 United States European Southern Observatory Alonso de Córdova 3107 Vitacura Casilla Santiago19001 Chile Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Earth Atmospheric and Planetary Sciences Massachusetts Institute of Technology CambridgeMA02139 United States Department of Aeronautics and Astronautics MIT 77 Massachusetts Avenue CambridgeMA02139 United States Observatoire de la Côte d’Azur UniCA CNRS CS 34229 Nice06304 cedex 4

We report the discovery and characterization of TOI-2005 b, a warm Jupiter on an eccentric (e ∼ 0.59), 17.3-day orbit around a Vmag = 9.867 rapidly rotating F-star. The object was detected as a candidate by TESS and the planetary nature of TOI-2005 b was then confirmed via a series of ground-based photometric, spectroscopic, and diffraction-limited imaging observations. The planet was found to reside in a low sky-projected stellar obliquity orbit (λ =4.8+2−235 degrees) via a transit spectroscopic observation using the Magellan MIKE spectrograph. TOI-2005 b is one of a few planets known to have a low-obliquity, high-eccentricity orbit, which may be the result of high-eccentricity coplanar migration. The planet has a periastron equilibrium temperature of ∼ 2100 K, similar to some highly irradiated hot Jupiters where atomic metal species have been detected in transmission spectroscopy, and varies by almost 1000 K during its orbit. Future observations of the atmosphere of TOI-2005b can inform us about its radiative timescales thanks to the rapid heating and cooling of the planet. © 2025, CC BY.

关键词： Photometry

来源：评论

学校读者我要写书评

暂无评论

Quantifying the Effects of Known Unknowns on Inferred High-redshift Galaxy Properties: Burstiness, the IMF, and Nebular physics

arXiv

引用

arXiv 2023年

作者： Wang, Bingjie Leja, Joel Atek, Hakim Labbé, Ivo Li, Yijia Bezanson, Rachel Brammer, Gabriel Cutler, Sam E. Dayal, Pratika Furtak, Lukas J. Greene, Jenny E. Kokorev, Vasily Pan, Richard Price, Sedona H. Suess, Katherine A. Weaver, John R. Whitaker, Katherine E. Williams, Christina C. 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 Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Physics & Astronomy and PITT PACC University of Pittsburgh PittsburghPA15260 United States Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Astronomy University of Massachusetts AmherstMA01003 United States Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Department of Physics & Astronomy Tufts University MA02155 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States NSF’s National Optical-Infrared Astronomy Research Laboratory TucsonAZ85719 United States Steward Observatory University of Arizona TucsonAZ85721 United States

The era of the James Webb Space Telescope ushers stellar population models into uncharted territories, particularly at the high-redshift frontier. In a companion paper, we apply the Prospector Bayesian framework to jointly infer galaxy redshifts and stellar population properties from broad-band photometry as part of the UNCOVER survey. Here we present a comprehensive error budget in spectral energy distribution (SED) modeling. Using a sample selected to have photometric redshifts higher than 9, we quantify the systematic shifts stemming from various model choices in inferred stellar mass, star formation rate (SFR), and age. These choices encompass different timescales for changes in the star formation history (SFH), non-universal stellar initial mass functions (IMF), and the inclusion of variable nebular abundances, gas density and ionizing photon budget. We find that the IMF exerts the strongest influence on the inferred properties: the systematic uncertainties can be as much as 1 dex, 2–5 times larger than the formal reported uncertainties in mass and SFR;and importantly, exceed the scatter seen when using different SED fitting codes. Although the assumptions on the lower end of the IMF induce degeneracy, our findings suggest that a common practice in the literature of assessing uncertainties in SED-fitting processes by comparing multiple codes is substantively underestimating the true systematic uncertainty. Highly stochastic SFHs change the inferred SFH by much larger than the formal uncertainties, and introduce ∼ 0.8 dex systematics in SFR averaged over short time scale and ∼ 0.3 dex systematics in average age. Finally, employing a flexible nebular emission model causes ∼ 0.2 dex systematic increase in mass and SFR, comparable to the formal uncertainty. This paper constitutes an initial step toward a complete uncertainty estimate in SED modeling. Copyright © 2023, The Authors. All rights reserved.

关键词： Stochastic systems

来源：评论

学校读者我要写书评

暂无评论

New measurement of double-β decays of Mo100 to excited states of Ru100 with the CUPID-Mo experiment

引用

Physical Review C 2023年第2期107卷 025503-025503页

作者： C. Augier A. S. Barabash F. Bellini G. Benato M. Beretta L. Bergé J. Billard Yu. A. Borovlev L. Cardani N. Casali A. Cazes M. Chapellier D. Chiesa I. Dafinei F. A. Danevich M. De Jesus T. Dixon L. Dumoulin K. Eitel F. Ferri B. K. Fujikawa J. Gascon L. Gironi A. Giuliani V. D. Grigorieva M. Gros D. L. Helis H. Z. Huang R. Huang L. Imbert J. Johnston A. Juillard H. Khalife M. Kleifges V. V. Kobychev Yu. G. Kolomensky S. I. Konovalov J. Kotila P. Loaiza L. Ma E. P. Makarov P. de Marcillac R. Mariam L. Marini S. Marnieros X.-F. Navick C. Nones E. B. Norman E. Olivieri J. L. Ouellet L. Pagnanini L. Pattavina B. Paul M. Pavan H. Peng G. Pessina S. Pirro D. V. Poda O. G. Polischuk S. Pozzi E. Previtali Th. Redon A. Rojas S. Rozov V. Sanglard J. A. Scarpaci B. Schmidt Y. Shen V. N. Shlegel V. Singh C. Tomei V. I. Tretyak V. I. Umatov L. Vagneron M. Velázquez B. Welliver L. Winslow M. Xue E. Yakushev M. Zarytskyy A. S. Zolotarova Univ. Lyon Université Lyon 1 CNRS/IN2P3 IP2I-Lyon F-69622 Villeurbanne France National Research Centre Kurchatov Institute Institute of Theoretical and Experimental Physics 117218 Moscow Russia Dipartimento di Fisica Sapienza Università di Roma P.le Aldo Moro 2 I-00185 Rome Italy INFN Sezione di Roma P.le Aldo Moro 2 I-00185 Rome Italy INFN Laboratori Nazionali del Gran Sasso I-67100 Assergi (AQ) Italy University of California Berkeley California 94720 USA Université Paris-Saclay CNRS/IN2P3 IJCLab 91405 Orsay France Nikolaev Institute of Inorganic Chemistry 630090 Novosibirsk Russia Dipartimento di Fisica Università di Milano-Bicocca I-20126 Milano Italy INFN Sezione di Milano-Bicocca I-20126 Milano Italy Institute for Nuclear Research of NASU 03028 Kyiv Ukraine IRFU CEA Université Paris-Saclay F-91191 Gif-sur-Yvette France Karlsruhe Institute of Technology Institute for Astroparticle Physics 76021 Karlsruhe Germany Lawrence Berkeley National Laboratory Berkeley California 94720 USA Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) Fudan University Shanghai 200433 P.R. China Massachusetts Institute of Technology Cambridge Massachusetts 02139 USA Karlsruhe Institute of Technology Institute for Data Processing and Electronics 76021 Karlsruhe Germany Department of Physics University of Jyväskylä P.O. Box 35 FI-40014 Jyväskylä Finland Finnish Institute for Educational Research University of Jyväskylä P.O. Box 35 FI-40014. Jyväskylä Finland Center for Theoretical Physics Sloane Physics Laboratory Yale University New Haven Connecticut 06520-8120 USA INFN Gran Sasso Science Institute I-67100 L'Aquila Italy Physik Department Technische Universität München Garching D-85748 Germany Department of Modern Physics University of Science and Technology of China Hefei 230027 P.R. China LSM Laboratoire Souterrain de Modane 73500 Modane France Laboratory of Nuclear Problems JINR 141980 Dubna Moscow region Russia Université Grenobl

The CUPID-Mo experiment, located at the Laboratoire Souterrain de Modane (France), was a demonstrator experiment for CUPID. It consisted of an array of 20Li2Mo100O4 (LMO) calorimeters, each equipped with a Ge light detector for particle identification. In this work, we present the result of a search for two-neutrino and neutrinoless double-β decays of Mo100 to the first 0+ and 2+ excited states of Ru100 using the full CUPID-Mo exposure (2.71kgyr of LMO). We measure the half-life of 2νββ decay to the 01+ state as T1/22ν→01+=(7.5±0.8(stat.)−0.3+0.4(syst.))×1020yr. The bolometric technique enables measurement of the electron energies as well as the γ rays from nuclear deexcitation and this allows us to set new limits on the two-neutrino decay to the 21+ state of T1/22ν→21+>4.4×1021yr(90% c.i.) and on the neutrinoless modes of T1/20ν→21+>2.1×1023yr(90% c.i.), T1/20ν→01+>1.2×1023yr(90% c.i.). Information on the electrons' spectral shape is obtained, which allows us to make the first comparison of the single and higher state dominance 2νββ decay models for the 01+ excited state of Ru100.

关键词： Double beta decay Neutrinoless double beta decay Nuclear structure & decays Majorana neutrinos Neutrinos 90 ≤ A ≤ 149

来源：评论

学校读者我要写书评

暂无评论

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

arXiv

引用

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

来源：评论

学校读者我要写书评

暂无评论

DeePMD-kit v2: A software package for Deep Potential models

arXiv

引用

arXiv 2023年

作者： Zeng, Jinzhe Zhang, Duo Lu, Denghui Mo, Pinghui Li, Zeyu Chen, Yixiao Rynik, Marián Huang, Li'ang Li, Ziyao Shi, Shaochen Wang, Yingze Ye, Haotian Tuo, Ping Yang, Jiabin Ding, Ye Li, Yifan Tisi, Davide Zeng, Qiyu Bao, Han Xia, Yu Huang, Jiameng Muraoka, Koki Wang, Yibo Chang, Junhan Yuan, Fengbo Bore, Sigbjørn Løland Cai, Chun Lin, Yinnian Wang, Bo Xu, Jiayan Zhu, Jia-Xin Luo, Chenxing Zhang, Yuzhi Goodall, Rhys E.A. Liang, Wenshuo Singh, Anurag Kumar Yao, Sikai Zhang, Jingchao Wentzcovitch, Renata Han, Jiequn Liu, Jie Jia, Weile York, Darrin M. Weinan, E. Car, Roberto Zhang, Linfeng Wang, Han Laboratory for Biomolecular Simulation Research Institute for Quantitative Biomedicine Department of Chemistry and Chemical Biology Rutgers University PiscatawayNJ08854 United States AI for Science Institute Beijing100080 China DP Technology Beijing100080 China Academy for Advanced Interdisciplinary Studies Peking University Beijing100871 China HEDPS CAPT College of Engineering Peking University Beijing100871 China College of Electrical and Information Engineering Hunan University Changsha China Yuanpei College Peking University Beijing100871 China Program in Applied and Computational Mathematics Princeton University PrincetonNJ08540 United States Department of Experimental Physics Comenius University Mlynská Dolina F2 Bratislava842 48 Slovakia Center for Quantum Information Institute for Interdisciplinary Information Sciences Tsinghua University Beijing100084 China Center for Data Science Peking University Beijing100871 China ByteDance Research Zhonghang Plaza No. 43 North 3rd Ring West Road Haidian District Beijing China College of Chemistry and Molecular Engineering Peking University Beijing100871 China Baidu Inc. Beijing China Key Laboratory of Structural Biology of Zhejiang Province School of Life Sciences Westlake University Zhejiang Hangzhou China Westlake AI Therapeutics Lab Westlake Laboratory of Life Sciences and Biomedicine Zhejiang Hangzhou China Department of Chemistry Princeton University PrincetonNJ08544 United States SISSA Scuola Internazionale Superiore di Studi Avanzati Trieste34136 Italy Laboratory of Computational Science and Modeling Institute of Materials École Polytechnique Fédérale de Lausanne Lausanne1015 Switzerland Department of Physics National University of Defense Technology Hunan Changsha410073 China State Key Lab of Processors Institute of Computing Technology Chinese Academy of Sciences Beijing China University of Chinese Academy of Sciences Beijing China School of Electronics Engineerin

DeePMD-kit is a powerful open-source software package that facilitates molecular dynamics simulations using machine learning potentials (MLP) known as Deep Potential (DP) models. This package, which was released in 2017, has been widely used in the fields of physics, chemistry, biology, and material science for studying atomistic systems. The current version of DeePMD-kit offers numerous advanced features such as DeepPot-SE, attention-based and hybrid descriptors, the ability to fit tensile properties, type embedding, model deviation, Deep Potential - Range Correction (DPRc), Deep Potential Long Range (DPLR), GPU support for customized operators, model compression, non-von Neumann molecular dynamics (NVNMD), and improved usability, including documentation, compiled binary packages, graphical user interfaces (GUI), and application programming interfaces (API). This article presents an overview of the current major version of the DeePMD-kit package, highlighting its features and technical details. Additionally, the article benchmarks the accuracy and efficiency of different models and discusses ongoing developments. © 2023, CC BY-NC-ND.

关键词： Molecular dynamics

来源：评论

学校读者我要写书评

暂无评论

Comparison and Evaluation of Methods for a Predict+Optimize Problem in Renewable Energy

arXiv

引用

arXiv 2022年

作者： Bergmeir, Christoph de Nijs, Frits Sriramulu, Abishek Abolghasemi, Mahdi Bean, Richard Betts, John Bui, Quang Dinh, Nam Trong Einecke, Nils Esmaeilbeigi, Rasul Ferraro, Scott Galketiya, Priya Genov, Evgenii Glasgow, Robert Godahewa, Rakshitha Kang, Yanfei Limmer, Steffen Magdalena, Luis Montero-Manso, Pablo Peralta, Daniel Kumar, Yogesh Pipada Sunil Rosales-Pérez, Alejandro Ruddick, Julian Stratigakos, Akylas Stuckey, Peter Tack, Guido Triguero, Isaac Yuan, Rui Department of Data Science and Artificial Intelligence Monash University Melbourne Australia School of Mathematics and Physics University of Queensland Brisbane Australia Centre for Energy Data Innovation School of Information Technology and Electrical Engineering University of Queensland Brisbane Australia School of Electrical and Electronics Engineering University of Adelaide Adelaide Australia Honda Research Institute Europe GmbH Offenbach am Main63073 Germany School of Information Technology Deakin University Melbourne Australia Building and Property Division Monash University Melbourne Australia EVERGi MOBI Vrije Universiteit Brussel Brussels Belgium School of Economics and Management Beihang University Beijing China E.T.S. Ingenieros Informáticos Universidad Politécnica de Madrid Madrid28660 Spain Disciple of Business Analytics University of Sydney Australia IDLab Department of Information Technology Ghent University - imec Belgium Department of Computer Science Centro de Investigación en Matem áticas Monterrey66629 Mexico Mines Paris PSL University Sophia Antipolis06904 France DaSCI Andalusian Institute in Data Science and Computational Intelligence Granada Spain Department of Computer Science and Artificial Intelligence University of Granada Granada Spain

Algorithms that involve both forecasting and optimization are at the core of solutions to many difficult real-world problems, such as in supply chains (inventory optimization), traffic, and in the transition towards carbon-free energy generation in battery/load/production scheduling in sustainable energy systems. Typically, in these scenarios we want to solve an optimization problem that depends on unknown future values, which therefore need to be forecast. As both forecasting and optimization are difficult problems in their own right, relatively few research has been done in this area. This paper presents the findings of the "IEEE-CIS Technical Challenge on Predict+Optimize for Renewable Energy Scheduling," held in 2021. We present a comparison and evaluation of the seven highest-ranked solutions in the competition, to provide researchers with a benchmark problem and to establish the state of the art for this benchmark, with the aim to foster and facilitate research in this area. The competition used data from the Monash Microgrid, as well as weather data and energy market data. It then focused on two main challenges: forecasting renewable energy production and demand, and obtaining an optimal schedule for the activities (lectures) and on-site batteries that lead to the lowest cost of energy. The most accurate forecasts were obtained by gradient-boosted tree and random forest models, and optimization was mostly performed using mixed integer linear and quadratic programming. The winning method predicted different scenarios and optimized over all scenarios jointly using a sample average approximation method. Copyright © 2022, The Authors. All rights reserved.

关键词： Forecasting

来源：评论

学校读者我要写书评

暂无评论

Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy

arXiv

引用

arXiv 2024年

作者： Park, Minjung Belli, Sirio Conroy, Charlie Johnson, Benjamin D. Davies, Rebecca L. Leja, Joel Tacchella, Sandro Mendel, J. Trevor Benton, Chloë Bugiani, Letizia Emami, Razieh Khoram, Amir H. Li, Yijia Maheson, Gabriel Mathews, Elijah P. Naidu, Rohan P. Nelson, Erica J. Terrazas, Bryan A. Weinberger, Rainer Center for Astrophysics Harvard & Smithsonian CambridgeMA02138 United States Dipartimento di Fisica e Astronomia Università di Bologna Bologna40129 Italy Centre for Astrophysics and Supercomputing Swinburne University of Technology HawthornVIC3122 Australia Australia Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Kavli Institute for Cosmology University of Cambridge CambridgeCB3 0EZ United Kingdom Cavendish Laboratory University of Cambridge CambridgeCB3 0EZ United Kingdom Research School of Astronomy and Astrophysics Australian National University CanberraACT2611 Australia De artment for Astro h sical and Planetar Science Universit of Colorado BoulderCO80305 United States MIT Kavli Institute for Astro h sics and S ace Research CambridgeMA02139 United States Department of Physics & Astronomy Oberlin College OberlinOH44074 United States Leibniz Institute for Astrophysics An der Starnwarte 16 Potsdam14482 Germany

Massive quiescent galaxies in the young Universe are expected to be quenched rapidly, but it is unclear whether they all experience starbursts before quenching and what physical mechanism drives rapid quenching. We study 14 massive quiescent galaxies (log(M M) > 10) at z ∼ 2 selected from a representative sample of the Blue Jay survey. We reconstruct their star formation histories (SFHs) by fitting spectral energy distribution models to the JWST/NIRSpec R ∼ 1000 spectra. We find that massive quiescent galaxies can be split into three categories with roughly equal numbers of galaxies according to their SFHs: (1) relatively old galaxies quenched at early epochs;(2) galaxies that are rapidly and recently quenched after a flat or bursty formation history (depending on the assumed prior);and (3) galaxies that are rapidly and recently quenched after a major starburst. Most recently quenched galaxies show neutral gas outflows, probed by blueshifted Na I D absorption, and ionized gas emission, with line ratios consistent with active galactic nucleus (AGN) diagnostics. This suggests that AGN activity drives multiphase gas outflows, leading to rapid quenching. By tracing back the SFHs of the entire sample, we predict the number density of massive quiescent galaxies at z = 4–6: n = (1.5–6.0) × 10−5 Mpc−3. The two old massive quiescent galaxies in our sample appear to have extremely early formation and quenching (z 6) and are possibly descendants of early post-starbursts at z > 3. These galaxies still show neutral gas reservoirs and weak Hα emission, perhaps because the ejective AGN feedback that caused rapid quenching has weakened over time. Copyright © 2024, The Authors. All rights reserved.

关键词： Rapid quenching

来源：评论

学校读者我要写书评

暂无评论

Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b

arXiv

引用

arXiv 2023年

作者： Fitzmaurice, Evan Stefánsson, Guðmundur Kavanagh, Robert D. Mahadevan, Suvrath Cañas, Caleb I. Winn, Joshua N. Robertson, Paul Ninan, Joe P. Albrecht, Simon Callingham, J.R. Cochran, William D. Delamer, Megan Kanodia, Shubham Lin, Andrea S.J. Marcussen, Marcus L. Pope, Benjamin J.S. Ramsey, Lawrence W. Roy, Arpita Vedantham, Harish Wright, Jason T. Department of Astronomy & Astrophysics Pennsylvania State University University ParkPA16802 United States Center for Exoplanets and Habitable Worlds Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences Scholar NASA Sagan Fellow United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08540 United States ASTRON Netherlands Institute for Radio Astronomy Oude Hoogeveensedijk 4 Dwingeloo7991 PD Netherlands NASA Postdoctoral Fellow United States NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Department of Physics & Astronomy The University of California Irvine IrvineCA92697 United States Department of Astronomy and Astrophysics Tata Institute of Fundamental Research Homi Bhabha Road Colaba Mumbai400005 India Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus C8000 Denmark Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands McDonald Observatory Department of Astronomy The University of Texas at Austin 2515 Speedway AustinTX78712 United States Center for Planetary Systems Habitability The University of Texas at Austin 2515 Speedway AustinTX78712 United States Earth and Planets Laboratory Carnegie Institution for Science 5241 Broad Branch Road NW WashingtonDC20015 United States School of Mathematics & Physics University of Queensland St LuciaQLD4072 Australia Centre for Astrophysics University of Southern Queensland West Street ToowoombaQLD4350 Australia Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics and Astronomy Johns Hopkins University 3400 N Charles St BaltimoreMD21218 United States Kapteyn Astronomical Institute University of Groningen

We characterize the LHS 1610 system, a nearby (d = 9.7 pc) M5 dwarf hosting a brown dwarf in a 10.6 day, eccentric (e ∼ 0.37) orbit. A joint fit of the available Gaia two-body solution, discovery radial velocities (RVs) from TRES, and new RVs obtained with the Habitable-zone Planet Finder, yields an orbital inclination of 117.2 ±0.9◦ and a mass constraint of 50.9 ±0.9 MJ. This gives LHS 1610 b the second most precise mass of brown dwarfs orbiting M stars within 25pc. We highlight a discrepancy between the Gaia two-body solution eccentricity (e = 0.52±0.03) and that from the RVs (e = 0.3702± 0.0003), which requires the astrometric time-series release (Gaia DR4) for further diagnostics. With a flare rate of 0.28 ±0.07 flares/day from TESS photometry, and a rotation period of 84 ±8 days, LHS 1610 joins other mid M stars—including Proxima Centauri and YZ Ceti—as nearby mid M dwarfs with flare rates on the higher end for their long rotation periods. These stars are promising candidates for searching for sub-Alfvénic star-companion interactions, raising the question whether LHS 1610 b could be driving the flares on its host star. However, the available TESS photometry is insufficient to confirm or rule out any orbital phase-dependence of the flares. We show that the LHS 1610 system, as a nearby mid M star with a large, short-period companion, is a promising target to look for evidence of star-companion interactions or aural emission from the brown dwarf at radio wavelengths. Copyright © 2023, The Authors. All rights reserved.

关键词： Stars

来源：评论

学校读者我要写书评

暂无评论

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案：

请选择收藏分类：

通借通还

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：