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arXiv 2024年

作者： Gillon, Michaël Pedersen, Peter P. Rackham, Benjamin V. Dransfield, Georgina Ducrot, Elsa Barkaoui, Khalid Burdanov, Artem Y. Schroffenegger, Urs Chew, Yilen Gómez Maqueo Lederer, Susan M. Alonso, Roi Burgasser, Adam J. Howell, Steve B. Narita, Norio de Wit, Julien Demory, Brice-Olivier Queloz, Didier Triaud, Amaury H.M.J. Delrez, Laetitia Jehin, Emmanuël Hooton, Matthew J. Garcia, Lionel J. Muñoz, Clàudia Jano Murray, Catriona A. Pozuelos, Francisco J. Sebastian, Daniel Timmermans, Mathilde Thompson, Samantha J. Zúñiga-Fernández, Sebastián Aceituno, Jesús Aganze, Christian Amado, Pedro J. Baycroft, Thomas Benkhaldoun, Zouhair Berardo, David Bolmont, Emeline Clark, Catherine A. Davis, Yasmin T. Davoudi, Fatemeh de Beurs, Zoë L. de Leon, Jerome P. Ikoma, Masahiro Ikuta, Kai Isogai, Keisuke Fukuda, Izuru Fukui, Akihiko Gerasimov, Roman Ghachoui, Mourad Günther, Maximilian N. Hasler, Samantha Hayashi, Yuya Heng, Kevin Hu, Renyu Kagetani, Taiki Kawai, Yugo Kawauchi, Kiyoe Kitzmann, Daniel Koll, Daniel D.B. Lendl, Monika Livingston, John H. Lyu, Xintong Meier Valdés, Erik A. Mori, Mayuko McCormac, James J. Murgas, Felipe Niraula, Prajwal Pallé, Enric Plauchu-Frayn, Ilse Rebolo, Rafael Sabin, Laurence Schackey, Yannick Schanche, Nicole Selsis, Franck Sota, Alfredo Stalport, Manu Standing, Matthew R. Stassun, Keivan G. Tamura, Motohide Theissen, Christopher A. Turbet, Martin Van Grootel, Valérie Varas, Roberto Watanabe, Noriharu Lang, Francis Zong Astrobiology Research Unit Université de Liège Allée du 6 août 19 Liège4000 Belgium Cavendish Laboratory JJ Thomson Avenue CambridgeCB3 0HE United Kingdom Department of Physics ETH Zurich Wolfgang-Pauli-Strasse 2 ZurichCH-8093 Switzerland Department of Earth Atmospheric and Planetary Science Massachusetts Institute of Technology 77 Massachusetts Avenue CambridgeMA02139 United States Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA United States School of Physics & Astronomy University of Birmingham Edgbaston BirminghamB15 2TT United Kingdom LESIA Observatoire de Paris CNRS Université Paris Diderot Université Pierre et Marie Curie 5 place Jules Janssen Meudon92190 France Calle Vía Láctea s/n Tenerife La Laguna38200 Spain Center for Space and Habitability University of Bern Gesellschaftsstrasse 6 BernCH-3012 Switzerland Instituto de Astronomía Universidad Nacional Autónoma de México Ciudad Universitaria Ciudad de México04510 Mexico NASA Johnson Space Center 2101 NASA Parkway HoustonTX77058 United States Departamento de Astrofísica Universidad de La Laguna Astrofísico Francisco Sánchez s/n Tenerife La Laguna38206 Spain Department of Astronomy & Astrophysics University of California San Diego La Jolla San DiegoCA92093 United States NASA Ames Research Center Moffett FieldCA94035 United States Komaba Institute for Science The University of Tokyo 3-8-1 Komaba Meguro Tokyo153-8902 Japan Astrobiology Center 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Institute Université de Liège Allée du 6 Août 19C LiègeB-4000 Belgium Institute of Astronomy KU Leuven Celestijnenlaan 200D Leuven3001 Belgium Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States Department of Astrophysical and Planetary Sciences University of Colorado Boulder BoulderCO80309 United States Glorieta de la Astronomía s/n GranadaE-18008 Spain Centro Astro

Located at the bottom of the main-sequence, ultracool dwarf stars are widespread in the solar neighborhood. Nevertheless, their extremely low luminosity has left their planetary population largely unexplored, and only one of them, TRAPPIST-1, has so far been found to host a transiting planetary system. In this context, we present the SPECULOOS project’s detection of an Earth-sized planet in a 17-hour orbit around an ultracool dwarf of M6.5 spectral type located 16.8 parsecs away. The planet’s high irradiation (16 times that of Earth) combined with the infrared luminosity and Jupiter-like size of its host star make it one of the most promising rocky exoplanets for detailed emission spectroscopy characterization with JWST. Indeed, our sensitivity study shows that just 10 secondary eclipse observations with the Mid-InfraRed Instrument Low-Resolution Spectrometer on board JWST should bring strong constraints on its atmospheric composition and/or surface mineralogy. © 2024, CC BY.

关键词： Emission spectroscopy

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SpectAcLE: AN IMPROVED METHOD FOR MODELING LIGHT ECHO SPECTRA

arXiv

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arXiv 2023年

作者： Partoush, Roee Rest, Armin Jencson, Jacob E. Poznanski, Dovi Foley, Ryan J. Kilpatrick, Charles D. Andrews, Jennifer E. Angulo, Rodrigo Badenes, Carles Bianco, Federica B. Filippenko, Alexei V. Ridden-Harper, Ryan Li, Xiaolong Margheim, Steve Matheson, Thomas Olsen, Knut A.G. Siebert, Matthew R. Smith, Nathan Welch, Douglas L. Zenteno, A. Department of Physics and Astronomy The Johns Hopkins University BaltimoreMD21218 United States School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Space Telescope Science Institute BaltimoreMD21218 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Cahill Center for Astrophysics California Institute of Technology PasadenaCA91125 United States Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Gemini Observatory NSF’s NOIRLab 670 N. A’ohoku Place HiloHI96720 United States Department of Physics and Astronomy University of Pittsburgh United States University of Pittsburgh PittsburghPA15260 United States University of Delaware Department of Physics and Astronomy 217 Sharp Lab NewarkDE19716 United States University of Delaware Joseph R. Biden Jr. School of Public Policy and Administration 184 Academy Street NewarkDE19716 United States University of Delaware Data Science Institute NewarkDE19716 United States Vera C. Rubin Observatory TucsonAZ85719 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States School of Physical and Chemical Sciences — Te Kura Mātu University of Canterbury Private Bag 4800 Christchurch Aotearoa8140 New Zealand Vera. C. Rubin Observatory/NSF’s NOIRLab Casilla 603 La Serena Chile NSF’s National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States NOIRLab 950 N. Cherry Ave. TucsonAZ85719 United States Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States Department of Physics and Astronomy McMaster University 1280 Main Street West HamiltonONL8S 4M1 Canada Cerro Tololo Inter-American Observatory NSF’s NOIRLab Casilla 603 La Serena Chile

Light echoes give us a unique perspective on the nature of supernovae and non-terminal stellar explosions. Spectroscopy of light echoes can reveal details on the kinematics of the ejecta, probe asymmetry, and reveal details on its interaction with circumstellar matter, thus expanding our understanding of these transient events. However, the spectral features arise from a complex interplay between the source photons, the reflecting dust geometry, and the instrumental setup and observing conditions. In this work we present an improved method for modeling these effects in light echo spectra, one that relaxes the simplifying assumption of a light curve weighted sum, and instead estimates the true relative contribution of each phase. We discuss our logic, the gains we obtain over light echo analysis method(s) used in the past, and prospects for further improvements. Lastly, we show how the new method improves our analysis of echoes from Tycho’s supernova (SN 1572) as an example. © 2023, CC BY.

关键词： Supernovae

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Measurement of Differential Branching Fractions of Inclusive B→Xuℓ+νℓ Decays

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physical Review Letters 2021年第26期127卷 261801-261801页

作者： L. Cao W. Sutcliffe R. Van Tonder F. U. Bernlochner I. Adachi H. Aihara D. M. Asner T. Aushev R. Ayad V. Babu S. Bahinipati P. Behera K. Belous J. Bennett M. Bessner T. Bilka J. Biswal A. Bobrov M. Bračko P. Branchini T. E. Browder A. Budano M. Campajola D. Červenkov M.-C. Chang P. Chang B. G. Cheon K. Chilikin H. E. Cho K. Cho S.-J. Cho Y. Choi S. Choudhury D. Cinabro S. Cunliffe T. Czank N. Dash G. De Pietro R. Dhamija F. Di Capua J. Dingfelder Z. Doležal T. V. Dong S. Dubey D. Epifanov T. Ferber D. Ferlewicz A. Frey B. G. Fulsom R. Garg V. Gaur N. Gabyshev A. Garmash A. Giri P. Goldenzweig T. Gu K. Gudkova S. Halder T. Hara O. Hartbrich K. Hayasaka M. Hernandez Villanueva W.-S. Hou C.-L. Hsu K. Inami A. Ishikawa R. Itoh M. Iwasaki W. W. Jacobs E.-J. Jang S. Jia Y. Jin K. K. Joo J. Kahn K. H. Kang H. Kichimi C. Kiesling C. H. Kim D. Y. Kim S. H. Kim Y.-K. Kim T. D. Kimmel K. Kinoshita P. Kodyš T. Konno A. Korobov S. Korpar E. Kovalenko P. Križan R. Kroeger P. Krokovny T. Kuhr R. Kulasiri M. Kumar R. Kumar K. Kumara A. Kuzmin Y.-J. Kwon S. C. Lee C. H. Li J. Li L. K. Li Y. B. Li L. Li Gioi J. Libby K. Lieret D. Liventsev C. MacQueen M. Masuda M. Merola F. Metzner K. Miyabayashi R. Mizuk G. B. Mohanty S. Mohanty M. Mrvar M. Nakao A. Natochii L. Nayak M. Niiyama N. K. Nisar S. Nishida K. Nishimura S. Ogawa H. Ono Y. Onuki P. Oskin G. Pakhlova S. Pardi H. Park S.-H. Park A. Passeri S. Patra S. Paul T. K. Pedlar L. E. Piilonen T. Podobnik V. Popov E. Prencipe M. T. Prim M. Röhrken A. Rostomyan N. Rout M. Rozanska G. Russo D. Sahoo S. Sandilya A. Sangal L. Santelj T. Sanuki V. Savinov G. Schnell J. Schueler C. Schwanda A. J. Schwartz Y. Seino K. Senyo M. E. Sevior M. Shapkin C. Sharma C. P. Shen J.-G. Shiu B. Shwartz F. Simon A. Sokolov E. Solovieva M. Starič J. F. Strube M. Sumihama T. Sumiyoshi M. Takizawa U. Tamponi K. Tanida Y. Tao F. Tenchini K. Trabelsi M. Uchida T. Uglov S. Uno P. Urquijo S. E. Vahsen G. Varner K. E. Varvell E. Waheed C. H. Wang E. Wang M.-Z. Wang P. Wang X. L. Wang M. Watanabe S. Watanuki O. University of Bonn 53115 Bonn Deutsches Elektronen–Synchrotron 22607 Hamburg High Energy Accelerator Research Organization (KEK) Tsukuba 305-0801 SOKENDAI (The Graduate University for Advanced Studies) Hayama 240-0193 Department of Physics University of Tokyo Tokyo 113-0033 Brookhaven National Laboratory Upton New York 11973 National Research University Higher School of Economics Moscow 101000 Department of Physics Faculty of Science University of Tabuk Tabuk 71451 Indian Institute of Technology Bhubaneswar Satya Nagar 751007 Indian Institute of Technology Madras Chennai 600036 Institute for High Energy Physics Protvino 142281 University of Mississippi University Mississippi 38677 University of Hawaii Honolulu Hawaii 96822 Faculty of Mathematics and Physics Charles University 121 16 Prague J. Stefan Institute 1000 Ljubljana Budker Institute of Nuclear Physics SB RAS Novosibirsk 630090 Novosibirsk State University Novosibirsk 630090 Faculty of Chemistry and Chemical Engineering University of Maribor 2000 Maribor INFN–Sezione di Roma Tre I-00146 Roma INFN–Sezione di Napoli I-80126 Napoli Università di Napoli Federico II I-80126 Napoli Department of Physics Fu Jen Catholic University Taipei 24205 Department of Physics National Taiwan University Taipei 10617 Department of Physics and Institute of Natural Sciences Hanyang University Seoul 04763 P.N. Lebedev Physical Institute of the Russian Academy of Sciences Moscow 119991 Korea Institute of Science and Technology Information Daejeon 34141 Yonsei University Seoul 03722 Sungkyunkwan University Suwon 16419 Indian Institute of Technology Hyderabad Telangana 502285 Wayne State University Detroit Michigan 48202 Kavli Institute for the Physics and Mathematics of the Universe (WPI) University of Tokyo Kashiwa 277-8583 Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) and Institute of Modern Physics Fudan University Shanghai 200443 School of Physics University of Melbourne Victoria 3010 II. Physikalisches Institu

The first measurements of differential branching fractions of inclusive semileptonic B→Xuℓ+νℓ decays are performed using the full Belle data set of 711 fb−1 of integrated luminosity at the ϒ(4S) resonance and for ℓ=e, μ. With the availability of these measurements, new avenues for future shape-function model-independent determinations of the Cabibbo-Kobayashi-Maskawa matrix element |Vub| can be pursued to gain new insights in the existing tension with respect to exclusive determinations. The differential branching fractions are reported as a function of the lepton energy, the four-momentum-transfer squared, light-cone momenta, the hadronic mass, and the hadronic mass squared. They are obtained by subtracting the backgrounds from semileptonic B→Xcℓ+νℓ decays and other processes, and corrected for resolution and acceptance effects.

关键词： Electroweak interaction Leptonic, semileptonic & radiative decays Particle decays Particle interactions Quark mixing Bottom mesons Bottom quark Form factors Lepton colliders Monte Carlo methods Particle data analysis Particle detectors

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The scintillating-fiber tracker (FIT) of the HERD space mission from design to performance 38

The scintillating-fiber tracker (FIT) of the HERD space miss...

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38th International Cosmic Ray Conference, ICRC 2023

作者： Adriani, O. Alemanno, F. Altomare, C. Ambrosi, G. Antonelli, M. Bai, X.H. Bai, Y.L. Bao, T.W. Barbanera, M. Barbato, F.C.T. Bernard, F. Bernardini, P. Berti, E. Bertucci, B. Betti, P. Bi, X.J. Bigongiari, G. Blanch, O. Boix, J. Bongi, M. Bonvicini, V. Bottai, S. Brogi, P. Brugnoni, C. Cadoux, F. Cagnoli, I. Cai, H.Y. Campana, D. Cao, W.W. Cardiel-Sas, L. Casaus, J. Casilli, E. Catala, R. Catanzani, E. Cattaneo, P.W. Cerasole, D. Chang, L. Chen, H. Chen, K. Chen, L. Chen, M.L. Chen, P.D. Chen, R. Cheng, Y.D. Cianetti, F. Comerma, A. Cong, X.Q. Coppin, P. Cui, X.Z. D'Alessandro, R. D'Urso, D. Díaz, C. Dai, C. De Mitri, I. de Palma, F. De Vecchi, C. Di Felice, V. Di Giovanni, A. Di Santo, M. Di Venere, L. Dong, Y.W. Donvito, G. Du, Y.J. Duranti, M. Espinya, A. Fang, K. Fariña, L. Favre, Y. Feng, H.B. Fernandez Alonso, M. Finetti, N. Fontanella, G. Formato, V. Frieden, J.M. Fu, Y. Fusco, P. Gao, J.R. Gargano, F. Gascón, D. Gasparrini, D. Ghose, E. Giovacchini, F. Gómez, S. Gong, K. Gu, M.H. Guberman, D. Guerrisi, C. Guida, R. Guo, D.Y. Guo, J.H. He, H.L. Hu, H. Hu, H.J. Hu, Y.M. Hu, Z.X. Huang, G.S. Huang, W.H. Huang, X.T. Huang, Y.G. Ionica, M. Jia, F. Jia, J.S. Jiang, F. Jiang, X.W. Jiang, Y. Jiao, P. Kotenko, A. Kyratzis, D. La Marra, D. Lathika, K.R. Li, L. Li, M.J. Li, M.X. Li, Q.Y. Li, Q.Y. Li, R. Li, S.L. Li, T. Li, T. Li, X.Q. Li, X.Q. Li, Y.Y. Li, Z.H. Liang, M.J. Liang, X.Z. Liao, C.L. Licciulli, F. Lin, Y.J. Liu, B.H. Liu, D. Liu, H. Liu, H.B. Liu, H.W. Liu, X. Liu, X.J. Liu, X.W. Liu, Y.Q. Loparco, F. Loporchio, S. Lorusso, L. Lu, B. Lu, R.S. Lu, Y.P. Lucchetta, G. Lv, J.G. Lv, L.W. Maestro, P. Mancini, E. Manera, R. Marin, J. Marrocchesi, P.S. Marsella, G. Martinez, G. Martinez, M. Mauricio, J. Mazziotta, M.N. Morettini, G. Mori, N. Mussolin, L. Nicotri, S. Niu, Y. Oliva, A. Orlandi, D. Orta, M. Department of Physics University of Florence Via Sansone 1 Sesto Fiorentino FirenzeI-50019 Italy Istituto Nazionale di Fisica Nucleare Sezione di Firenze Sesto Fiorentino Via Sansone 1 FirenzeI-50019 Italy Viale Crispi 7 L'AquilaI-67100 Italy Istituto Nazionale di Fisica Nucleare Laboratori Nazionali del Gran Sasso Via Acitelli 22 Assergi L'AquilaI-67100 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari via Orabona 4 BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Perugia Via Alessandro Pascoli 23c PerugiaI-06123 Italy Istituto Nazionale di Fisica Nucleare Sezione di Trieste via A. Valerio 2 TriesteI-34127 Italy Université de Genève 24 quai Ernest-Ansermet 4 GenèveCH-1211 Switzerland Xi'an Institute of Optics and Precision Mechanics CAS No.17 Xinxi Road New Industrial Park Xi'an Hi-Tech Industrial Development Zone Xi'an710019 China Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Shijingshan District Beijing100049 China Bâtiment PH Station 3 LausanneCH-1015 Switzerland Dipartimento di Matematica e Fisica 'E. De Giorgi' Università del Salento LecceI-73100 Italy Istituto Nazionale di Fisica Nucleare Sezione di Lecce Via per Arnesano LecceI-73100 Italy Università degli Studi di Perugia Piazza Università 1 PerugiaI-06123 Italy University of Chinese Academy of Sciences No.1 Yanqihu East Rd Huairou District Beijing101408 China Department of Physical Sciences Earth and Environment University of Siena via Roma 56 SienaI-53100 Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa Largo B. Pontecorvo 3 PisaI-56127 Italy Bellaterra BarcelonaE-08193 Spain Istituto Nazionale di Fisica Nucleare Sezione di Napoli Via Cintia NapoliI-80126 Italy MadridE-28040 Spain BarcelonaE-08028 Spain Istituto Nazionale di Fisica Nucleare Sezione di Pavia Via Bassi 6 PaviaI-27100 Italy Dipartimento di Fisica 'M. Merlin' dell'Università e del Politecnico di Bari via

The High Energy cosmic-Radiation Detection facility (HERD) will be a calorimetric experiment on board the China Space Station. Starting from 2027, HERD will perform the first direct measurement of cosmic rays in the PeV region and the gamma-ray full-sky survey from 100 MeV. The detector will be equipped with a scintillating-fiber tracker (FIT) read out with silicon photomultipliers. A miniature of a FIT sector, called MiniFIT, was designed, built and tested with particle beams at CERN. The FIT design, together with the design and physics performance of MiniFIT will be presented in this contribution. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Cosmology

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Solvation Effect-Determined Mechanisms of Cation Exchange Reactions for Efficient Multicomponent Nanocatalysts

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Angewandte Chemie 2024年第6期137卷

作者： Shangheng Liu Xiaocan Wang Dr. Wei-Hsiang Huang Prof. Qiugen Zhang Dr. Jiajia Han Yingtian Zhang Dr. Chih-Wen Pao Prof. Zhiwei Hu Prof. Yong Xu Prof. Xiaoqing Huang State Key Laboratory of Physical Chemistry of Solid Surfaces College of Chemistry and Chemical Engineering Xiamen University 422 Siming South Road Xiamen 361005 China i-lab Suzhou Institute of Nano-Tech and Nano-Bionics (SINANO) Chinese Academy of Sciences (CAS) Suzhou 215123 China National Synchrotron Radiation Research Center 101 Hsin-Ann Road Hsinchu 30076 Taiwan Department of Materials Science and Engineering College of Materials Xiamen University 422 Siming South Road Xiamen 361005 China School of Chemical Engineering & Technology Tianjin University Tianjin 300072 China Max Planck Institute for Chemical Physics of Solids Nothnitzer Strasse 40 Dresden 01187 Germany Innovation Laboratory for Sciences and Technologies of Energy Materials of Fujian Province (IKKEM) Xiamen 361005 China

Cation exchange (CE) reaction is a classical synthesis method for creating complex structures. A lock of study on intrinsic mechanism limits its understanding and practical application. Using X-ray absorption spectroscopy, we observed that the evolution from Ru−Cl to Ru−O/OH occurs during the CE between K 2 RuCl 6 and CoSn(OH) 6 in aqueous solution, while CE between K 2 PtCl 6 and CoSn(OH) 6 is inhibited due to the failure of structural evolution from Pt−Cl to Pt−O/OH. Theoretical simulations imply that the interaction between Ru−O and CoSn(OH) 6 with Co vacancy (CoV Co Sn(OH) 6 ) endows the electron transfer, as a result of strengthened adsorption on CoV Co Sn(OH) 6 . Moreover, this mechanism is validated for CE between K 2 RuCl 6 and ASn(OH) 6 (A=Mg, Ca, Mn, Co, Cu, Zn), and CE between K 2 PdCl 6 /Na 3 RhCl 6 /K 2 IrCl 6 and CoSn(OH) 6 . Impressively, the Pt-free CoRuSn(OH) x produced via CE displays a mass activity and a power density of 15.0 A mg Ru −1 and 11.6 W mg Ru −1 , respectively, for anion exchange membrane fuel cell (AEMFC) exceeding the values of commercial PtRu/C (11.8 A mg Ru+Pt −1 and 9.0 W mg Ru+Pt −1 ). This work, for the first time, reveals the intrinsic mechanism of CE as structural evolution of target ion breaking through the traditional classic etch-adsorption mechanism and will promote fundamental research and practical application in various fields.

关键词： solvation effect-determined mechanisms cation exchange reactions multicomponent nanocatalysts anion exchange membrane fuel cell

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Alkynyl-Protected Chiral Bimetallic Ag22Cu7Superatom with Multiple Chirality Origins

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Angewandte Chemie 2022年第12期135卷

作者： Dr. Guocheng Deng Kangjae Lee Hongwen Deng Dr. Sami Malola Dr. Megalamane S. Bootharaju Prof. Hannu Häkkinen Prof. Nanfeng Zheng Prof. Taeghwan Hyeon Center for Nanoparticle Research Institute for Basic Science (IBS) School of Chemical and Biological Engineering and Institute of Chemical Processes Seoul National University Seoul 08826 Republic of Korea Collaborative Innovation Center of Chemistry for Energy Materials State Key Laboratory for Physical Chemistry of Solid Surfaces and National & Local Joint Engineering Research Center of Preparation Technology of Nanomaterials College of Chemistry and Chemical Engineering Xiamen University Xiamen 361005 China Departments of Physics and Chemistry Nanoscience Center University of Jyväskylä 40014 Jyväskylä Finland

Understanding the origin of chirality in the nanostructured materials is essential for chiroptical and catalytic applications. Here we report a chiral AgCu superatomic cluster, [Ag 22 Cu 7 (C≡CR) 16 (PPh 3 ) 5 Cl 6 ](PPh 4 ), Ag 22 Cu 7 , protected by an achiral alkynyl ligand (HC≡CR: 3,5-bis(trifluoromethyl)phenylacetylene). Its crystal structure comprises a rare interpenetrating biicosahedral Ag 17 Cu 2 core, which is stabilized by four different types of motifs: one Cu(C≡CR) 2 , four −C≡CR, two chlorides and one helical Ag 5 Cu 4 (C≡CR) 10 (PPh 3 ) 5 Cl 4 . Structural analysis reveals that Ag 22 Cu 7 exhibits multiple chirality origins, including the metal core, the metal-ligand interface and the ligand layer. Furthermore, the circular dichroism spectra of R/S-Ag 22 Cu 7 are obtained by employing appropriate chiral molecules as optical enrichment agents. DFT calculations show that Ag 22 Cu 7 is an eight-electron superatom, confirm that the cluster is chirally active, and help to analyze the origins of the circular dichroism.

关键词： Alkynyl Ligand Bimetallic Cluster Chirality Chirality Origins Superatom

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GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run

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physical Review X 2023年第4期13卷 041039-041039页

作者： R. Abbott T. D. Abbott F. Acernese K. Ackley C. Adams N. Adhikari R. X. Adhikari V. B. Adya C. Affeldt D. Agarwal M. Agathos K. Agatsuma N. Aggarwal O. D. Aguiar L. Aiello A. Ain P. Ajith S. Akcay T. Akutsu S. Albanesi A. Allocca P. A. Altin A. Amato C. Anand S. Anand A. Ananyeva S. B. Anderson W. G. Anderson M. Ando T. Andrade N. Andres T. Andrić S. V. Angelova S. Ansoldi J. M. Antelis S. Antier S. Appert Koji Arai Koya Arai Y. Arai S. Araki A. Araya M. C. Araya J. S. Areeda M. Arène N. Aritomi N. Arnaud M. Arogeti S. M. Aronson K. G. Arun H. Asada Y. Asali G. Ashton Y. Aso M. Assiduo S. M. Aston P. Astone F. Aubin C. Austin S. Babak F. Badaracco M. K. M. Bader C. Badger S. Bae Y. Bae A. M. Baer S. Bagnasco Y. Bai L. Baiotti J. Baird R. Bajpai M. Ball G. Ballardin S. W. Ballmer A. Balsamo G. Baltus S. Banagiri D. Bankar J. C. Barayoga C. Barbieri B. C. Barish D. Barker P. Barneo F. Barone B. Barr L. Barsotti M. Barsuglia D. Barta J. Bartlett M. A. Barton I. Bartos R. Bassiri A. Basti M. Bawaj J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale M. Bejger I. Belahcene V. Benedetto D. Beniwal T. F. Bennett J. D. Bentley M. BenYaala F. Bergamin B. K. Berger S. Bernuzzi C. P. L. Berry D. Bersanetti A. Bertolini J. Betzwieser D. Beveridge R. Bhandare U. Bhardwaj D. Bhattacharjee S. Bhaumik I. A. Bilenko G. Billingsley S. Bini R. Birney O. Birnholtz S. Biscans M. Bischi S. Biscoveanu A. Bisht B. Biswas M. Bitossi M.-A. Bizouard J. K. Blackburn C. D. Blair D. G. Blair R. M. Blair F. Bobba N. Bode M. Boer G. Bogaert M. Boldrini L. D. Bonavena F. Bondu E. Bonilla R. Bonnand P. Booker B. A. Boom R. Bork V. Boschi N. Bose S. Bose V. Bossilkov V. Boudart Y. Bouffanais A. Bozzi C. Bradaschia P. R. Brady A. Bramley A. Branch M. Branchesi J. Brandt J. E. Brau M. Breschi T. Briant J. H. Briggs A. Brillet M. Brinkmann P. Brockill A. F. Brooks J. Brooks D. D. Brown S. Brunett G. Bruno R. Bruntz J. Bryant T. Bulik H. J. Bulten A. Buonanno R. Buscicchio D. Buskulic C. Buy R. L. Byer G. S. Cabourn Davies L. Cadonati G. Cagn LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Louisiana State University Baton Rouge Louisiana 70803 USA Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy OzGrav School of Physics & Astronomy Monash University Clayton 3800 Victoria Australia LIGO Livingston Observatory Livingston Louisiana 70754 USA University of Wisconsin-Milwaukee Milwaukee Wisconsin 53201 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany University of Birmingham Birmingham B15 2TT United Kingdom Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) Northwestern University Evanston Illinois 60208 USA Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Gravity Exploration Institute Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa I-56127 Pisa Italy International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India University College Dublin Dublin 4 Ireland Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan INFN Sezione di Torino I-10125 Torino Italy Università di Napoli “Federico II” Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy Université de Lyon Université Claude Bernard Lyon 1 CNRS Institut L

The third Gravitational-Wave Transient Catalog (GWTC-3) describes signals detected with Advanced LIGO and Advanced Virgo up to the end of their third observing run. Updating the previous GWTC-2.1, we present candidate gravitational waves from compact binary coalescences during the second half of the third observing run (O3b) between 1 November 2019, 15∶00 Coordinated Universal Time (UTC) and 27 March 2020, 17∶00 UTC. There are 35 compact binary coalescence candidates identified by at least one of our search algorithms with a probability of astrophysical origin pastro>0.5. Of these, 18 were previously reported as low-latency public alerts, and 17 are reported here for the first time. Based upon estimates for the component masses, our O3b candidates with pastro>0.5 are consistent with gravitational-wave signals from binary black holes or neutron-star–black-hole binaries, and we identify none from binary neutron stars. However, from the gravitational-wave data alone, we are not able to measure matter effects that distinguish whether the binary components are neutron stars or black holes. The range of inferred component masses is similar to that found with previous catalogs, but the O3b candidates include the first confident observations of neutron-star–black-hole binaries. Including the 35 candidates from O3b in addition to those from GWTC-2.1, GWTC-3 contains 90 candidates found by our analysis with pastro>0.5 across the first three observing runs. These observations of compact binary coalescences present an unprecedented view of the properties of black holes and neutron stars.

关键词： Gravitational waves

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Anatase TiO₂(001)-(1 × 4) Surface Is Intrinsically More Photocatalytically Active than the Rutile TiO₂(110)-(1 × 1) Surface

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Journal of physical Chemistry C 2019年第40期123卷 24558-24565页

作者： Xiong, Feng Yin, Li-Li Li, Fei Wu, Zongfang Wang, Zhengming Sun, Guanghui Xu, Hong Chai, Peng Gong, Xue-Qing Huang, Weixin Hefei National Laboratory for Physical Sciences at Microscale Key Lab. of Surf. and Interface Chemistry and Energy Catalysis of Anhui Higher Education Institutes CAS Key Laboratory of Materials for Energy Conversion Department of Chemical Physics University of Science and Technology of China Jinzhai Road 96 Hefei 230026 China Key Laboratory for Advanced Materials Centre for Computational Chemistry Research Institute of Industrial Catalysis School of Chemistry and Molecular Engineering East China University of Science and Technology Meilong Road 130 Shanghai 200237 China Sinopec Shanghai Research Institute of Petrochemical Technology (SRIPT) Shanghai 201208 China

Aligning the intrinsic photocatalytic activities of various types of TiO2 facets is of great importance and interest in TiO2 photocatalysis. Herein, we report a comparative study of the intrinsic photocatalytic activi... 详细信息

Aligning the intrinsic photocatalytic activities of various types of TiO₂ facets is of great importance and interest in TiO₂ photocatalysis. Herein, we report a comparative study of the intrinsic photocatalytic activities of anatase TiO₂(001)-(1 × 4) and rutile TiO₂(110)-(1 × 1) surfaces probed by photostimulated desorption of O₂ with combined thermal desorption spectroscopy, photostimulated desorption spectroscopy, and density functional theory calculations. Photostimulated desorption behavior of O₂ depends on both TiO₂ surface structures and O₂ adsorption configurations. O₂ species adsorbed on the anatase TiO₂(001)-(1 × 4) surface exhibit a higher intrinsic photostimulated desorption reactivity than those on the rutile TiO₂(110)-(1 × 1) surface, which can be associated with their electronic structures and subsequent hole transfer processes from TiO₂. These results provide, for the first time, direct and unambiguous experimental evidence for the higher intrinsic photocatalytic activity of the anatase TiO₂(001) facet than those of other TiO₂ facets and highlight the key role of structures of both TiO₂ surfaces and adsorbed species in TiO₂ photocatalysis. Copyright © 2019 American chemical Society.

关键词： Desorption Oxides Electromagnetic radiation Adsorption Minerals

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Exploring Observational Heliophysics Across All Scales: Reflections and Insights From the 2023 NASA Heliophysics Summer School

Perspectives of Earth and Space Scientists

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Perspectives of Earth and Space Scientists 2024年第1期5卷

作者： S. R. Shaver A. R. Smith S. S. Babu Y. Baruah M. Bauer V. Chaturmutha H. Chen B. Dalal G. B. Dias da Silva T. Eddy G. González S. Gu E. Gülay A. P. Hoffmann O. R. Idolor R. Khan Y. Liou N. Liu X. Lyu A. Maharana D. K. V. Radhakrishnan O. M. Romeo P. O. C. Silva H. M. Salah C. Thibeault A. Weiss Laboratory for Atmospheric and Space Physics University of Colorado Boulder CO USA Geophysical Institute University of Alaska Fairbanks AK USA Department of Physics University of Alberta Edmonton AB Canada Department of Physical Sciences Indian Institute of Science Education and Research Kolkata Mohanpur West Bengal India Center of Excellence in Space Sciences India Indian Institute of Science Education and Research Kolkata Mohanpur West Bengal India Austrian Space Weather Office GeoSphere Austria Graz Austria Department of Physics & Astronomy Georgia State University Atlanta GA USA Department of Electrical and Computer Engineering University of Illinois Urbana-Champaign Urbana IL USA Space and Atmospheric Sciences Physical Research Laboratory Ahmedabad Gujarat India National Institute for Space Research (INPE) São Paulo Brazil Department of Climate and Space Sciences and Engineering University of Michigan Ann Arbor MI USA Space Sciences Laboratory University of California Berkeley Berkeley CA USA Department of Physics University of Texas at Dallas Richardson TX USA Istanbul Technical University Istanbul Turkiye Department of Physics Faculty of Science University of Lagos Lagos Nigeria Indian Institute of Astrophysics Bangalore Karnataka India Department of Engineering Physics Embry-Riddle Aeronautical University Daytona Beach FL USA New Jersey Institute of Technology Newark NJ USA West Virginia University Morgantown WV USA Katholieke Universiteit Leuven Leuven Belgium University of Texas at San Antonio San Antonio TX USA Southwest Research Institute San Antonio TX USA Physics Department Faculty of Science Space Weather Monitoring Center Helwan University Cairo Egypt Université de Montréal Montréal QC Canada NASA Postdoctoral Program Fellowship NASA Goddard Space Flight Center Greenbelt MD USA

The field of heliophysics encompasses a diverse range of research areas and rich plasma environments, from the solar dynamo and solar wind turbulence, to the complex terrestrial thermosphere-ionosphere-magnetosphere (TIM) system, to investigations of both induced and intrinsic magnetospheres across the solar system. This perspective paper delves into the experiences and outcomes of a summer school held in person in Boulder, Colorado, USA, from 7–11 August, which offered a platform for interdisciplinary learning and collaboration. The event, supported by NASA's Living with a Star program and hosted by the University Corporation for Atmospheric Research and Cooperative programs for the Advancement of Earth System science, assembled a cohort of 26 graduate students and postdoctoral researchers from around the world, all engaged in heliophysics research. The summer school included a series of lectures, interactive activities, and a culminating capstone project. The participants' diverse backgrounds enriched discussions and encouraged novel approaches to traditional problems. The capstone projects spanned an array of topics, including investigating the origins of solar wind switchbacks, dissecting the sequence of events from solar eruptions and their corresponding terrestrial consequences, investigating the energy transfer from solar coronal mass ejections to Earth's magnetosphere, and advocating for the exploration of Coulomb collisions in understanding large-scale global systems. Through this perspective, we shed light on the value of international and interdisciplinary collaboration in advancing heliophysics research. This perspective paper encapsulates the ethos of the summer school, serving as a testament to the continuing and collective pursuit of unraveling the mysteries of the heliosphere. Cooperative programs for the Advancement of Earth System science/University Corporation for Atmospheric Research held the seventeenth annual NASA Heliophysics Summer School bot

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The ALMA-QUARKS survey: – I. Survey description and data reduction

arXiv

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arXiv 2023年

作者： Liu, Xunchuan Liu, Tie Zhu, Lei Garay, Guido Liu, Hong-Li Goldsmith, Paul Evans, Neal Kim, Kee-Tae Liu, Sheng-Yuan Xu, Fengwei Lu, Xing Tej, Anandmayee Mai, Xiaofeng Bronfman, Leonardo Li, Shanghuo Mardones, Diego Stutz, Amelia Tatematsu, Kenichi Wang, Ke Zhang, Qizhou Qin, Sheng-Li Zhou, Jianwen Luo, Qiuyi Zhang, Siju Cheng, Yu He, Jinhua Gu, Qilao Li, Ziyang Zhang, Zhenying Zhang, Suinan Saha, Anindya Dewangan, Lokesh Sanhueza, Patricio Shen, Zhiqiang Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile School of Physics and Astronomy Yunnan University Kunming650091 China Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Department of Astronomy The University of Texas AustinTX78712-1205 United States Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Institute of Astronomy and Astrophysics Academia Sinica Roosevelt Road Taipei10617 Taiwan Kavli Institute for Astronomy and Astrophysics Peking University Haidian District Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Indian Institute of Space Science and Technology Kerala Thiruvananthapuram695 547 India Max Planck Institute for Astronomy Königstuhl 17 HeidelbergD-69117 Germany Departamento de Astronomía Universidad de Concepción Casilla 160-C Concepción Chile Nobeyama Radio Observatory National Astronomical Observatory of Japan National Institutes of Natural Sciences 462-2 Nobeyama Minamimaki Minamisaku Nagano384-1305 Japan Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53125 Germany School of Astronomy and Space Sciences University of Chinese Academy of Sciences Beijing100049 China National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Yunnan Observatories Chinese Academy of Sciences Yunnan Kunming650216 China Physical Research Laboratory Navrangpura Ahmedabad380 009 India GUAS Astronomical Science Program SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan

This paper presents an overview of the QUARKS survey, which stands for ‘Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures’. The QUARKS survey is observing 139 massive clumps covered by 156 pointings at ALMA Band 6 (λ ∼ 1.3 mm). In conjunction with data obtained from the ALMA-ATOMS survey at Band 3 (λ ∼ 3 mm), QUARKS aims to carry out an unbiased statistical investigation of massive star formation process within protoclusters down to a scale of 1000 au. This overview paper describes the observations and data reduction of the QUARKS survey, and gives a first look at an exemplar source, the mini-starburst Sgr B2(M). The wide-bandwidth (7.5 GHz) and high-angular-resolution (∼ 0.3′′) observations of the QUARKS survey allow to resolve much more compact cores than could be done by the ATOMS survey, and to detect previously unrevealed fainter filamentary structures. The spectral windows cover transitions of species including CO, SO, N2D+, SiO, H30α, H2CO, CH3CN and many other complex organic molecules, tracing gas components with different temperatures and spatial extents. QUARKS aims to deepen our understanding of several scientific topics of massive star formation, such as the mass transport within protoclusters by (hub-)filamentary structures, the existence of massive starless cores, the physical and chemical properties of dense cores within protoclusters, and the feedback from already formed high-mass young protostars. Copyright © 2023, The Authors. All rights reserved.

关键词： Data reduction

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