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Electric and magnetic dipole strength in Sn112,114,116,118,120,124

Physical Review C 2020年第3期102卷 034327-034327页

作者： S. Bassauer P. von Neumann-Cosel P.-G. Reinhard A. Tamii S. Adachi C. A. Bertulani P. Y. Chan A. D'Alessio H. Fujioka H. Fujita Y. Fujita G. Gey M. Hilcker T. H. Hoang A. Inoue J. Isaak C. Iwamoto T. Klaus N. Kobayashi Y. Maeda M. Matsuda N. Nakatsuka S. Noji H. J. Ong I. Ou N. Pietralla V. Yu. Ponomarev M. S. Reen A. Richter M. Singer G. Steinhilber T. Sudo Y. Togano M. Tsumura Y. Watanabe V. Werner Institut für Kernphysik Technische Universität Darmstadt D-64289 Darmstadt Germany Institut für Theoretische Physik II Universität Erlangen D-91058 Erlangen Germany Research Center for Nuclear Physics Osaka University Ibaraki Osaka 567-0047 Japan Department of Physics and Astronomy Texas A&M University–Commerce Commerce Texas 75429 USA Department of Physics Tokyo Institute of Technology Tokyo 152-8551 Japan RIKEN Nishina Center for Accelerator-Based Science 2-1 Hirosawa Wako 351-0198 Saitama Japan Department of Applied Physics Miyazaki University Miyazaki 889-2192 Japan Department of Communications Engineering Graduate School of Engineering Tohoku University Aramaki Aza Aoba Aoba-ku Sendai 980-8579 Japan National Superconducting Cyclotron Laboratory Michigan State University East Lansing Michigan 48824 USA Institute of Modern Physics Chinese Academy of Sciences Lanzhou 730000 China Department of Physics Okayama University Okayama 700-8530 Japan Department of Physics Akal University Talwandi Sabo Bathinda Punjab-151 302 India Department of Physics Rikkyo University Tokyo 171-8501 Japan Department of Physics Kyoto University Kyoto 606-8502 Japan Department of Physics University of Tokyo Tokyo 113-8654 Japan

Background: There is renewed interest in electric dipole strength distributions for a variety of reasons including the extraction of the dipole polarizability related to properties of the symmetry energy and a measure for the neutron skin thickness, understanding the structure of low-energy E1 strength in nuclei with neutron excess, and establishing the systematics of the isovector giant dipole resonance (IVGDR). Inelastic proton scattering at energies of a few hundred MeV and very forward angles including 0∘ has been established as a tool for the study of electric and magnetic dipole strength distributions in nuclei.

关键词： Collective levels Electromagnetic transitions H & He induced nuclear reactions Nuclear density functional theory Nuclear structure & decays Photonuclear reactions

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ALMA-IMF XIII: N2H+ kinematic analysis on the intermediate protocluster G353.41

arXiv

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arXiv 2024年

作者： Álvarez-Gutiérrez, R.H. Stutz, A.M. Sandoval-Garrido, N. Louvet, F. Motte, F. Galván-Madrid, R. Cunningham, N. Sanhueza, P. Bonfand, M. Bontemps, S. Gusdorf, A. Ginsburg, A. Csengeri, T. Reyes, S.D. Salinas, J. Baug, T. Bronfman, L. Busquet, G. Díaz-González, D.J. Fernandez-Lopez, M. Guzmán, A. Koley, A. Liu, H.-L. Olguin, F.A. Valeille-Manet, M. Wyrowski, F. Departamento de Astronomía Universidad de Concepción Casilla 160-C Concepción Chile Univ. Grenoble Alpes CNRS IPAG Grenoble38000 France Instituto de Radioastronomía y Astrofísica Universidad Nacional Autónoma de México Michoacán Morelia58089 Mexico SKA Observatory Jodrell Bank Lower Withington MacclesfieldSK11 9FT United Kingdom National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Departments of Astronomy University of Virginia CharlottesvilleVA22904 United States Laboratoire d'astrophysique de Bordeaux Univ. Bordeaux CNRS B18N allée Geoffroy Saint-Hilaire PessacF-33615 France Laboratoire de Physique de l'École Normale Supérieure ENS Université PSL CNRS Sorbonne Université Université Paris Cité ParisF-75005 France Observatoire de Paris PSL University Sorbonne Université LERMA Paris75014 France Department of Astronomy University of Florida P.O. Box 112055 GainesvilleFL32611 United States Max Planck Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany S. N. Bose National Centre for Basic Sciences Sector-III Salt Lake Kolkata700106 India Astronomy Department Universidad de Chile Camino El Observatorio 1515 Las Condes Santiago Chile Martí i Franquès 1 Catalonia Barcelona08028 Spain Universitat de Barcelona Martí i Franquès 1 Catalonia Barcelona08028 Spain Gran Capità 2-4 Catalonia Barcelona08034 Spain C.C. No. 5 Villa Elisa Buenos Aires1894 Argentina Alonso de Córdova 3107 Vitacura Santiago Chile School of Physics and Astronomy Yunnan University Kunming650091 China Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu30013 Taiwan Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany

The ALMA-IMF Large program provides multi-tracer observations of 15 Galactic massive protoclusters at matched sensitivity and spatial resolution. We focus on the dense gas kinematics of the G353.41 protocluster traced by N2H+ (1−0), with an spatial resolution ∼ 0.02 pc. G353.41, at a distance of ∼ 2 kpc, is embedded in a larger scale (∼ 8 pc) filament and has a mass of ∼ 2.5 × 103 M☉ within 1.3 × 1.3 pc2. We extract the N2H+ (1−0) isolated line component and we decompose it by fitting up to 3 Gaussian velocity components. This allows us to identify velocity structures that are either muddled or impossible to identify in the traditional position-velocity diagram. We identify multiple velocity gradients on large (∼ 1 pc) and small scales (∼0.2 pc). We find good agreement between the N2H+ velocities and the previously reported DCN core velocities, suggesting that cores are kinematically coupled to the dense gas in which they form. We measure 9 converging "V-shaped" velocity gradients (VGs) (∼ 20 km s−1 pc−1) that are well-resolved (sizes ∼ 0.1 pc), located in filaments, which are sometimes associated with cores near their point of convergence. We interpret these V-shapes as inflowing gas feeding the regions near cores (the immediate sites of star formation). We estimate the timescales associated with V-shapes as VG−1, and we interpret them as inflow timescales. The average inflow timescale is ∼ 67 kyr, or about twice the free-fall time of cores in the same area (∼ 33 kyr) but substantially shorter than protostar lifetime estimates (∼ 0.5 Myr). We derive mass accretion rates in the range of (0.35 − 8.77) × 10−4 M☉ yr−1. This feeding might lead to further filament collapse and formation of new cores. We suggest that the protocluster is collapsing on large scales, but the velocity signature of collapse is slow compared to pure free-fall. Thus these data are consistent with a comparatively slow global protocluster contraction under gravity, and faster core formation within

关键词： Kinematics

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Non-reciprocal interactions induced by water in confinement

arXiv

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arXiv 2020年

作者： Jiménez-Ángeles, Felipe Harmon, Katherine Nguyen, Trung Dac Fenter, Paul de la Cruz, Monica Olvera Department of Materials Science and Engineering Northwestern University EvanstonIL60208 United States Applied Physics Graduate Program Northwestern University EvanstonIL60208 United States Department of Chemical and Biological Engineering Northwestern University EvanstonIL60208 United States Chemical Sciences and Engineering Division Argonne National Laboratory LemontIL60439 United States Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Department of Chemistry Northwestern University EvanstonIL60208 United States

Water mediates electrostatic interactions via the orientation of its dipoles around ions, molecules, and interfaces. This induced water polarization consequently influences multiple phenomena. In particular, water polarization modulated by nanoconfinement affects ion adsorption and transport, biomolecular self-assembly, and surface chemical reactions. Therefore, it is of paramount importance to understand how water-mediated interactions change at the nanoscale. Here we show that near the graphene surface anion-cation interactions do not obey the translational and isotropic symmetries of Coulomb’s law. We identify a new property, referred to as non-reciprocity, which describes the non-equivalent and directional interaction between two oppositely charged ions near the confining surface when their positions with respect to the interface are exchanged. Specifically, upon exchange of the two ions’ positions along the surface normal direction the interaction energy changes by about 5kBT. In both cases, confinement enhances the attraction between two oppositely charged ions near the graphene surface, while intercalation of one ion into the graphene layers shifts the interaction to repulsive. While the water permittivity in confinement is different from that in bulk, the effects observed here via molecular dynamics simulations and X-ray reflectivity experiments cannot be accounted for by current permittivity models. Our work shows that the water structure is not enough to infer electrostatic interactions near interfaces. Copyright © 2020, The Authors. All rights reserved.

关键词： Ions

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Experimental observation of topological exciton-polaritons in transition metal dichalcogenide monolayers

arXiv

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arXiv 2020年

作者： Li, Mengyao Sinev, Ivan Benimetskiy, Fedor Ivanova, Tatyana Khestanova, Ekaterina Kiriushechkina, Svetlana Vakulenko, Anton Guddala, Sriram Skolnick, Maurice Menon, Vinod Krizhanovskii, Dmitry Alù, Andrea Samusev, Anton Khanikaev, Alexander B. Department of Electrical Engineering City College of New York New YorkNY United States Physics Department City College of New York New YorkNY United States Physics Program Graduate Center of the City University of New York New YorkNY United States Department of Physics and Engineering ITMO University Saint Petersburg Russia Department of Physics and Astronomy University of Sheffield SheffieldS3 7RH United Kingdom Photonics Initiative Advanced Science Research Center City University of New York New YorkNY United States

The rise of quantum science and technologies motivates photonics research to seek new platforms with strong light-matter interactions to facilitate quantum behaviors at moderate light intensities.1–3 One promising platform to reach such strong light-matter interacting regimes is offered by polaritonic metasurfaces, which represent ultrathin artificial media structured on nano-scale and designed to support polaritons – half-light half-matter quasiparticles. Topological polaritons, or "topolaritons", offer an ideal platform in this context, with unique properties stemming from topological phases of light strongly coupled with matter. Here we explore polaritonic metasurfaces based on 2D transition metal dichalcogenides (TMDs) supporting in-plane polarized exciton resonances as a promising platform for topological polaritonics. We enable a spin-Hall4,5 topolaritonic phase by strongly coupling valley polarized in-plane excitons in a TMD monolayer with a suitably engineered all-dielectric topological photonic metasurface. We first show that the strong coupling between topological photonic bands supported by the metasurface and excitonic bands in MoSe2 yields an effective phase winding and transition to a topolaritonic spin-Hall state. We then experimentally realize such phenomena and confirm the presence of one-way spin-polarized edge topolaritons. Combined with the valley polarization in a MoSe2 monolayer, the proposed system enables a new approach to engage the photonic angular momentum and valley degree of freedom in TMDs, offering a promising platform for photonic/solid-state interfaces for valleytronics and spintronics. Copyright © 2020, The Authors. All rights reserved.

关键词： Monolayers

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Fluorine abundances in CEMP stars at the lowest metallicity: Hints on the nature of the first stars

arXiv

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arXiv 2025年

作者： Mura-Guzmán, Aldo Yong, David Kobayashi, Chiaki Tominaga, Nozomu McKenzie, Madeleine Salinas, Ricardo Mace, Gregory Kim, Hwihyun Zucker, Daniel B. Faculty of Science and Engineering School of Mathematical and Physical Sciences Macquarie University SydneyNSW2109 Australia Research School of Astronomy and Astrophysics Australian National University Mount Stromlo Observatory Cotter Road Weston CreekACT2611 Australia Astrophysics and Space Technologies Research Centre Macquarie University SydneyNSW2109 Australia Australia Centre for Astrophysics Research University of Hertfordshire College Lane HatfieldAL10 9AB United Kingdom National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Tokyo Mitaka181-8588 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Tokyo Mitaka181-8588 Japan Department of Physics Faculty of Science and Engineering Konan University 8-9-1 Okamoto Hyogo Kobe658-8501 Japan Carnegie Science Observatories 813 Santa Barbara St. PasadenaCA91101 United States Nicolaus Copernicus Astronomical Center Polish Academy of Sciences Bartycka 18 Warszawa00-716 Poland Department of Astronomy McDonald Observatory University of Texas at Austin 2515 Speedway Stop C1400 AustinTX78712-1205 United States Gemini Observatory NSF NOIRLab 950 N Cherry Avenue TucsonAZ85719 United States

In the last decade, the available measurements of fluorine abundance have increased significantly, providing additional information on the chemical evolution of our Galaxy and details on complex stellar nucleosynthesis processes. However, the observational challenges to obtain stellar F abundances favor samples with higher metallicities, resulting in a scarcity of measurements at low-metallicity ([Fe/H] Copyright © 2025, The Authors. All rights reserved.

关键词： Infrared spectrometers

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Discovery of two infrared objects with strong ice absorption in the AKARI slit-less spectroscopic survey of the Galactic Plane

arXiv

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arXiv 2021年

作者： Onaka, Takashi Kimura, Tomoyuki Sakon, Itsuki Shimonishi, Takashi Department of Physics Faculty of Science and Engineering Meisei University 2-1-1 Hodokubo Hino Tokyo191-8506 Japan Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Center for Transdisciplinary Research Niigata University Ikarashi-nihoncho 8050 Nishi-ku Niigata950-2181 Japan Environmental Science Program Department of Science Faculty of Science Niigata University Ikarashi-nihoncho 8050 Nishi-ku Niigata950-2181 Japan

We discover two infrared objects that show deep absorption features of H2O, CO2, and CO ices in the AKARI/Infrared Camera (IRC) slit-less spectroscopic survey of the Galactic plane in 2.5-13 µm. Both objects are located neither in known star-forming regions nor in known dense clouds. For one of the objects, Object 1, we successfully extract a spectrum from 2.5 to 13 µm, which also shows several absorption features in 5-13 µm, including deep silicate absorption at 10 µm. For the other object, Object 2, only a spectrum from 3.1 to 5 µm is reliably extracted due to the presence of nearby overlapping objects and faint nebulosity. Both objects show warm (> 100 K) CO gas absorption in addition to the ice absorption features, suggesting that they are embedded young stellar objects (YSOs). On the other hand, both objects have spectral energy distributions (SEDs) that peak at around 5 µm and decrease towards longer wavelengths. These characteristics of the SEDs and the presence of deep absorption features cannot easily be accounted for by standard YSO models. They may be explained as background stars behind dense clouds. We discuss possible nature of the objects and implications of the present discovery. © 2021, CC BY-NC-ND.

关键词： Ice

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Simultaneous multicolour transit photometry of hot Jupiters HAT-P-19b, HAT-P-51b, HAT-P-55b, and HAT-P-65b

arXiv

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arXiv 2024年

作者： Kang, Huiyi Chen, Guo Pallé, Enric Murgas, Felipe García, Nestor Abreu de Leon, Jerome Enoc, Gareb Esparza-Borges, Emma Fukuda, Izuru Fukui, Akihiko Galán, Daniel Hayashi, Yuya Isogai, Keisuke Kagetani, Taiki Kawauchi, Kiyoe Korth, Judith Livingston, John H. Luque, Rafael Ma, Yuehua Madrigal-Aguado, Alberto Meni, Pedro Rodriguez, Pilar Montañes Mori, Mori Torres, Sara Muñoz Narita, Norio Orell-Miquel, Jaume Parviainen, Hannu Peláez-Torres, Alberto Stangret, Monika Tamura, Motohide Watanabe, Noriharu CAS Key Laboratory of planetary sciences Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China CAS Center for Excellence in Comparative Planetology Hefei230026 China Instituto de Astrofísica de Canarias Vía Láctea s/n Tenerife La Laguna38205 Spain Departamento de Astrofísica Universidad de La Laguna C/Padre Herrera Tenerife La Laguna38206 Spain Department of Multi-Disciplinary Sciences Graduate School of Arts and Sciences The University of Tokyo 3-8-1 Komaba Meguro Tokyo153-8902 Japan Komaba Institute for Science The University of Tokyo 3-8-1 Komaba Meguro Tokyo153-8902 Japan Okayama Observatory Kyoto University 3037-5 Honjo Kamogatacho Okayama Asakuchi719-0232 Japan Department of Physical Sciences Ritsumeikan University Shiga Kusatsu525-8577 Japan Lund Observatory Division of Astrophysics Department of Physics Lund University Box 43 Lund22100 Sweden Astrobiology Center 2-21-1 Osawa Mitaka Tokyo181-8588 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Astronomy & Astrophysics University of Chicago ChicagoIL60637 United States School of Architecture Universidad Europea de Canarias C/Inocencio Garcia 1 Tenerife La Orotava38300 Spain INAF - Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 Padova35122 Italy Department of Astronomy University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan

Accurate physical parameters of exoplanet systems are essential for further exploration of planetary internal structure, atmospheres, and formation history. We aim to use simultaneous multicolour transit photometry to improve the estimation of transit parameters, to search for transit timing variations (TTVs), and to establish which of our targets should be prioritised for follow-up transmission spectroscopy. We performed time series photometric observations of 12 transits for the hot Jupiters HAT-P-19b, HAT-P-51b, HAT-P-55b, and HAT-P-65b using the simultaneous four-colour camera MuSCAT2 on the Telescopio Carlos Sánchez. We collected 56 additional transit light curves from TESS photometry. To derive transit parameters, we modelled the MuSCAT2 light curves with Gaussian processes to account for correlated noise. To derive physical parameters, we performed EXOFASTv2 global fits to the available transit and radial velocity data sets, together with the Gaia DR3 parallax, isochrones, and spectral energy distributions. To assess the potential for atmospheric characterisation, we compared the multicolour transit depths with a flat line and a clear atmosphere model. We consistently refined the transit and physical parameters. We improved the orbital period and ephemeris estimates, and found no evidence for TTVs or orbital decay. The MuSCAT2 broadband transmission spectra of HAT-P-19b and HAT-P-65b are consistent with previously published low-resolution transmission spectra. We also found that, except for HAT-P-65b, the assumption of a planetary atmosphere can improve the fit to the MuSCAT2 data. In particular, we identified HAT-P-55b as a priority target among these four planets for further atmospheric studies using transmission spectroscopy. Copyright © 2024, The Authors. All rights reserved.

关键词： Photometry

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Measurement of f₁(1285) production in pp collisions at s = 13 TeV

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physics Letters, Section B: Nuclear, Elementary Particle and High-Energy physics 2025年 866卷

作者： Acharya, S. Agarwal, A. Aglieri Rinella, G. Aglietta, L. Agnello, M. Agrawal, N. Ahammed, Z. Ahmad, S. Ahn, S.U. Ahuja, I. Akindinov, A. Akishina, V. Al-Turany, M. Aleksandrov, D. Alessandro, B. Alfanda, H.M. Alfaro Molina, R. Ali, B. Alici, A. Alizadehvandchali, N. Alkin, A. Alme, J. Alocco, G. Alt, T. Altamura, A.R. Altsybeev, I. Alvarado, J.R. Alvarez, C.O.R. Anaam, M.N. Andrei, C. Andreou, N. Andronic, A. Andronov, E. Anguelov, V. Antinori, F. Antonioli, P. Apadula, N. Aphecetche, L. Appelshäuser, H. Arata, C. Arcelli, S. Arnaldi, R. Arneiro, J.G.M.C.A. Arsene, I.C. Arslandok, M. Augustinus, A. Averbeck, R. Averyanov, D. Azmi, M.D. Baba, H. Badalà, A. Bae, J. Baek, Y.W. Bai, X. Bailhache, R. Bailung, Y. Bala, R. Balbino, A. Baldisseri, A. Balis, B. Banoo, Z. Barbasova, V. Barile, F. Barioglio, L. Barlou, M. Barman, B. Barnaföldi, G.G. Barnby, L.S. Barreau, E. Barret, V. Barreto, L. Bartels, C. Barth, K. Bartsch, E. Bastid, N. Basu, S. Batigne, G. Battistini, D. Batyunya, B. Bauri, D. Bazo Alba, J.L. Bearden, I.G. Beattie, C. Becht, P. Behera, D. Belikov, I. Bell Hechavarria, A.D.C. Bellini, F. Bellwied, R. Belokurova, S. Beltran, L.G.E. Beltran, Y.A.V. Bencedi, G. Bensaoula, A. Beole, S. Berdnikov, Y. Berdnikova, A. Bergmann, L. Besoiu, M.G. Betev, L. Bhaduri, P.P. Bhasin, A. Bhattacharjee, B. Bianchi, L. Bielčík, J. Bielčíková, J. Bigot, A.P. Bilandzic, A. Biro, G. Biswas, S. Bize, N. Blair, J.T. Blau, D. Blidaru, M.B. Bluhme, N. Blume, C. Boca, G. Bock, F. Bodova, T. Bok, J. Boldizsár, L. Bombara, M. Bond, P.M. Bonomi, G. Borel, H. Borissov, A. Borquez Carcamo, A.G. Botta, E. Bouziani, Y.E.M. Bratrud, L. Braun-Munzinger, P. Bregant, M. Broz, M. Bruno, G.E. Buchakchiev, V.D. Buckland, M.D. Budnikov, D. Buesching, H. Bufalino, S. Buhler, P. Burmasov, N. Buthelezi, Z. Bylinkin, A. Bysiak, S.A. Cabanillas Noris, J.C. Cabrera, M.F.T. Cai, M. Caines, H. Caliva, A. Calvo Villar, E. Camacho, J.M.M. Camerini, P. Canedo, F.D.M. Cantway, S.L. Carabas, M. Carballo, A.A. Carnesecchi, F. Caron, R. Carvalho, L.A.D. Castil A.I. Alikhanyan National Science Laboratory (Yerevan Physics Institute) Foundation Yerevan Armenia AGH University of Krakow Cracow Poland Bogolyubov Institute for Theoretical Physics National Academy of Sciences of Ukraine Kiev Ukraine Bose Institute Department of Physics Centre for Astroparticle Physics and Space Science (CAPSS) Kolkata India California Polytechnic State University San Luis Obispo CA United States Central China Normal University Wuhan China Centro de Aplicaciones Tecnológicas y Desarrollo Nuclear (CEADEN) Havana Cuba Centro de Investigación y de Estudios Avanzados (CINVESTAV) Mexico City and Mérida Mexico Chicago State University Chicago IL United States China Institute of Atomic Energy Beijing China China University of Geosciences Wuhan China Chungbuk National University Cheongju South Korea Comenius University Bratislava Faculty of Mathematics Physics and Informatics Bratislava Slovakia Creighton University Omaha NE United States Department of Physics Aligarh Muslim University Aligarh India Department of Physics Pusan National University Pusan South Korea Department of Physics Sejong University Seoul South Korea Department of Physics University of California Berkeley CA United States Department of Physics University of Oslo Oslo Norway Department of Physics and Technology University of Bergen Bergen Norway Dipartimento di Fisica Università di Pavia Pavia Italy Dipartimento di Fisica dell'Università Sezione INFN Cagliari Italy Dipartimento di Fisica dell'Università Sezione INFN Trieste Italy Dipartimento di Fisica dell'Università Sezione INFN Turin Italy Dipartimento di Fisica e Astronomia dell'Università Sezione INFN Bologna Italy Dipartimento di Fisica e Astronomia dell'Università Sezione INFN Catania Italy Dipartimento di Fisica e Astronomia dell'Università Sezione INFN Padova Italy Dipartimento di Fisica ‘E.R. Caianiello’ dell'Università Gruppo Collegato INFN Salerno Italy Dipartimento DISAT del Politecnico Sezi

This study presents the first measurement of the f1(1285) resonance using the ALICE detector in inelastic proton–proton collisions at a center-of-mass energy of 13 TeV. The resonance is reconstructed at midrapidity (...

This study presents the first measurement of the f₁(1285) resonance using the ALICE detector in inelastic proton–proton collisions at a center-of-mass energy of 13 TeV. The resonance is reconstructed at midrapidity (|y|< 0.5) through the hadronic decay channel f₁(1285)→K_S⁰K^±π^∓. Key measurements include the determination of its mass, transverse-momentum integrated yield, and average transverse momentum. Additionally, the ratio of the transverse-momentum integrated yield of f₁(1285) to pion is compared with calculations from the canonical statistical hadronization model. The model calculation, assuming a zero total strangeness content for f₁(1285), reproduces the data within 1σ deviation, shedding light on the quark composition of f₁(1285). © 2025 CERN for the benefit of the ALICE Collaboration

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First polarisation measurement of coherently photoproduced J/ψ in ultra-peripheral Pb–Pb collisions at s_NN=5.02 TeV

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physics Letters, Section B: Nuclear, Elementary Particle and High-Energy physics 2025年 865卷

作者： Acharya, S. Adamová, D. Adler, A. Aglieri Rinella, G. Agnello, M. Agrawal, N. Ahammed, Z. Ahmad, S. Ahn, S.U. Ahuja, I. Akindinov, A. Al-Turany, M. Aleksandrov, D. Alessandro, B. Alfanda, H.M. Alfaro Molina, R. Ali, B. Alici, A. Alizadehvandchali, N. Alkin, A. Alme, J. Alocco, G. Alt, T. Altsybeev, I. Alvarado, J.R. Anaam, M.N. Andrei, C. Andronic, A. Anguelov, V. Antinori, F. Antonioli, P. Apadula, N. Aphecetche, L. Appelshäuser, H. Arata, C. Arcelli, S. Aresti, M. Arnaldi, R. Arneiro, J.G.M.C.A. Arsene, I.C. Arslandok, M. Augustinus, A. Averbeck, R. Azmi, M.D. Badalà, A. Bae, J. Baek, Y.W. Bai, X. Bailhache, R. Bailung, Y. Balbino, A. Baldisseri, A. Balis, B. Banerjee, D. Banoo, Z. Barbera, R. Barile, F. Barioglio, L. Barlou, M. Barnaföldi, G.G. Barnby, L.S. Barret, V. Barreto, L. Bartels, C. Barth, K. Bartsch, E. Bastid, N. Basu, S. Batigne, G. Battistini, D. Batyunya, B. Bauri, D. Bazo Alba, J.L. Bearden, I.G. Beattie, C. Becht, P. Behera, D. Belikov, I. Bell Hechavarria, A.D.C. Bellini, F. Bellwied, R. Belokurova, S. Belyaev, V. Bencedi, G. Beole, S. Bercuci, A. Berdnikov, Y. Berdnikova, A. Bergmann, L. Besoiu, M.G. Betev, L. Bhaduri, P.P. Bhasin, A. Bhat, M.A. Bhattacharjee, B. Bianchi, L. Bianchi, N. Bielčík, J. Bielčíková, J. Biernat, J. Bigot, A.P. Bilandzic, A. Biro, G. Biswas, S. Bize, N. Blair, J.T. Blau, D. Blidaru, M.B. Bluhme, N. Blume, C. Boca, G. Bock, F. Bodova, T. Bogdanov, A. Boi, S. Bok, J. Boldizsár, L. Bombara, M. Bond, P.M. Bonomi, G. Borel, H. Borissov, A. Borquez Carcamo, A.G. Bossi, H. Botta, E. Bouziani, Y.E.M. Bratrud, L. Braun-Munzinger, P. Bregant, M. Broz, M. Bruno, G.E. Buckland, M.D. Budnikov, D. Buesching, H. Bufalino, S. Buhler, P. Buthelezi, Z. Bylinkin, A. Bysiak, S.A. Cai, M. Caines, H. Caliva, A. Calvo Villar, E. Camacho, J.M.M. Camerini, P. Canedo, F.D.M. Cantway, S.L. Carabas, M. Carballo, A.A. Carnesecchi, F. Caron, R. Carvalho, L.A.D. Castillo Castellanos, J. Catalano, F. Ceballos Sanchez, C. Chakaberia, I. Chakraborty, P. Chandra, S. Chapeland, S. Chartier, M. Chattopa A.I. Alikhanyan National Science Laboratory (Yerevan Physics Institute) Foundation Yerevan Armenia AGH University of Krakow Cracow Poland Bogolyubov Institute for Theoretical Physics National Academy of Sciences of Ukraine Kiev Ukraine Bose Institute Department of Physics Centre for Astroparticle Physics and Space Science (CAPSS) Kolkata India California Polytechnic State University San Luis Obispo CA United States Central China Normal University Wuhan China Centro de Aplicaciones Tecnológicas y Desarrollo Nuclear (CEADEN) Havana Cuba Centro de Investigación y de Estudios Avanzados (CINVESTAV) Mexico City and Mérida Mexico Chicago State University Chicago IL United States China Institute of Atomic Energy Beijing China Chungbuk National University Cheongju South Korea Comenius University Bratislava Faculty of Mathematics Physics and Informatics Bratislava Slovakia COMSATS University Islamabad Islamabad Pakistan Creighton University Omaha NE United States Department of Physics Aligarh Muslim University Aligarh India Department of Physics Pusan National University Pusan South Korea Department of Physics Sejong University Seoul South Korea Department of Physics University of California Berkeley CA United States Department of Physics University of Oslo Oslo Norway Department of Physics and Technology University of Bergen Bergen Norway Dipartimento di Fisica Università di Pavia Pavia Italy Dipartimento di Fisica dell'Università Sezione INFN Cagliari Italy Dipartimento di Fisica dell'Università Sezione INFN Trieste Italy Dipartimento di Fisica dell'Università Sezione INFN Turin Italy Dipartimento di Fisica e Astronomia dell'Università Sezione INFN Bologna Italy Dipartimento di Fisica e Astronomia dell'Università Sezione INFN Catania Italy Dipartimento di Fisica e Astronomia dell'Università Sezione INFN Padova Italy Dipartimento di Fisica ‘E.R. Caianiello’ dell'Università Gruppo Collegato INFN Salerno Italy Dipartimento DISAT del Politecnico

The first measurement of the polarisation of coherently photoproduced J/ψ mesons in ultra-peripheral Pb–Pb collisions, using data at sNN=5.02 TeV, is presented. The J/ψ meson is measured via its dimuon decay channe...

The first measurement of the polarisation of coherently photoproduced J/ψ mesons in ultra-peripheral Pb–Pb collisions, using data at s_NN=5.02 TeV, is presented. The J/ψ meson is measured via its dimuon decay channel in the forward rapidity interval −4.0−1 ± 5% (syst) is analysed. Hadronic activity is highly suppressed since the interaction is mediated by a photon. The polar and azimuthal angle distributions of the decay muons are measured, and the polarisation parameters λ_θ, λ_φ, λ_θφ are extracted. The analysis is carried out in the helicity frame. The results are found to be consistent with a transversely polarised J/ψ. These values are compared with previous measurements by the H1 and ZEUS experiments. The polarisation parameters of coherent J/ψ photoproduction in Pb–Pb collisions are found to be consistent with the s-channel helicity conservation hypothesis. © 2025 CERN for the benefit of the ALICE Collaboration

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Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy

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Astrophysical Journal Letters 2024年第2期967卷 L21-L21页

作者： Kuzuhara, Masayuki Fukui, Akihiko Livingston, John H. Caballero, José A. de Leon, Jerome P. Hirano, Teruyuki Kasagi, Yui Murgas, Felipe Narita, Norio Omiya, Masashi Orell-Miquel, Jaume Palle, Enric Changeat, Quentin Esparza-Borges, Emma Harakawa, Hiroki Hellier, Coel Hori, Yasunori Ikuta, Kai Ishikawa, Hiroyuki Tako Kodama, Takanori Kotani, Takayuki Kudo, Tomoyuki Morales, Juan C. Mori, Mayuko Nagel, Evangelos Parviainen, Hannu Perdelwitz, Volker Reiners, Ansgar Ribas, Ignasi Sanz-Forcada, Jorge Sato, Bun’ei Schweitzer, Andreas Tabernero, Hugo M. Takarada, Takuya Uyama, Taichi Watanabe, Noriharu Zechmeister, Mathias García, Néstor Abreu Aoki, Wako Beichman, Charles Béjar, Víctor J. S. Brandt, Timothy D. Calatayud-Borras, Yéssica Carleo, Ilaria Charbonneau, David Collins, Karen A. Currie, Thayne Doty, John P. Dreizler, Stefan Fernández-Rodríguez, Gareb Fukuda, Izuru Galán, Daniel Geraldía-González, Samuel González-Garcia, Josafat Hayashi, Yuya Hedges, Christina Henning, Thomas Hodapp, Klaus Ikoma, Masahiro Isogai, Keisuke Jacobson, Shane Janson, Markus Jenkins, Jon M. Kagetani, Taiki Kambe, Eiji Kawai, Yugo Kawauchi, Kiyoe Kokubo, Eiichiro Konishi, Mihoko Korth, Judith Krishnamurthy, Vigneshwaran Kurokawa, Takashi Kusakabe, Nobuhiko Kwon, Jungmi Laza-Ramos, Andrés Libotte, Florence Luque, Rafael Madrigal-Aguado, Alberto Matsumoto, Yuji Mawet, Dimitri McElwain, Michael W. Gallardo, Pedro Pablo Meni Morello, Giuseppe Torres, Sara Muñoz Nishikawa, Jun Nugroho, Stevanus K. Ogihara, Masahiro Peláez-Torres, Alberto Rapetti, David Sánchez-Benavente, Manuel Schlecker, Martin Seager, Sara Serabyn, Eugene Serizawa, Takuma Stangret, Monika Takahashi, Aoi Teng, Huan-Yu Tamura, Motohide Terada, Yuka Ueda, Akitoshi Usuda, Tomonori Vanderspek, Roland Vievard, Sébastien Watanabe, David Winn, Joshua N. Zapatero Osorio, Maria Rosa Astrobiology Center NINS 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan National Astronomical Observatory of Japan NINS 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Komaba Institute for Science The University of Tokyo 3-8-1 Komaba Meguro Tokyo 153-8902 Japan Instituto de Astrofísica de Canarias (IAC) La Laguna Tenerife E-38200 Spain Astronomical Science Program Graduate University for Advanced Studies (SOKENDAI) 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Centro de Astrobiología CSIC-INTA Camino Bajo del Castillo s/n Villanueva de la Cañada Madrid E-28692 Spain Department of Multi-Disciplinary Sciences Graduate School of Arts and Sciences The University of Tokyo 3-8-1 Komaba Meguro Tokyo 153-8902 Japan Departamento de Astrofísica Universidad de La Laguna (ULL) La Laguna Tenerife E-38206 Spain European Space Agency (ESA) ESA Office Space Telescope Science Institute (STScI) Baltimore 21218 MD United States Department of Physics and Astronomy University College London Gower Street London WC1E 6BT United Kingdom National Astronomical Observatory of Japan 650 North A‘ohōkū Place Hilo 96720 HI United States Astrophysics Group Keele University Staffordshire ST5 5BG United Kingdom Department of Physics and Astronomy The University of Western Ontario 1151 Richmond Street London N6A 3K7 ON Canada Earth-Life Science Institute (ELSI) Tokyo Institute of Technology 2-12-1-I7E-315 Ookayama Meguro-ku Tokyo 152-8550 Japan Institut de Ciències de l’Espai (ICE CSIC) Campus UAB Can Magrans s/n Bellaterra Barcelona 08193 Spain Institut d’Estudis Espacials de Catalunya (IEEC) c/ Gran Capità 2-4 Barcelona 08034 Spain Institut für Astrophysik und Geophysik Georg-August-Universität Friedrich-Hund-Platz 1 Göttingen 37077 Germany Department of Physics Ariel University Ariel 40700 Israel Department of Earth and Planetary Sciences School of Science Tokyo Institute of Technology 2-12-1 Ookayama Meguro-ku Tokyo 152-8551 Japan Hamburger Sternwarte Goje

Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (P _orb) of 12.76 days. The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous P _orb from TESS data. We confirmed the transit signal and P _orb using ground-based photometry with MuSCAT2 and MuSCAT3, and validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host star is inactive, with an X-ray-to-bolometric luminosity ratio of log L X / L bol ≈ − 5.7 . Joint analysis of the light curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R _⊕, a 3σ mass upper limit of 3.9 M _⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric (TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST. © 2024. The Author(s). Published by the American Astronomical Society.

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