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arXiv 2022年

作者： Abe, S. Asami, S. Eizuka, M. Futagi, S. Gando, A. Gando, Y. Gima, T. Goto, A. Hachiya, T. Hata, K. Hosokawa, K. Ichimura, K. Ieki, S. Ikeda, H. Inoue, K. Ishidoshiro, K. Kamei, Y. Kawada, N. Kishimoto, Y. Kinoshita, T. Koga, M. Kurasawa, M. Maemura, N. Mitsui, T. Miyake, H. Nakahata, T. Nakamura, K. Nakamura, K. Nakamura, R. Ozaki, H. Sakai, T. Sambonsugi, H. Shimizu, I. Shirai, J. Shiraishi, K. Suzuki, A. Suzuki, Y. Takeuchi, A. Tamae, K. Watanabe, H. Yoshida, Y. Obara, S. Ichikawa, A.K. Yoshida, S. Umehara, S. Fushimi, K. Kotera, K. Urano, Y. Berger, B.E. Fujikawa, B.K. Learned, J.G. Maricic, J. Axani, Spencer N. Smolsky, J. Lertprasertpong, J. Winslow, L.A. Fu, Z. Ouellet, J. Efremenko, Y. Karwowski, H.J. Markoff, D.M. Tornow, W. Li, A. Detwiler, J.A. Enomoto, S. Decowski, M.P. Grant, C. Song, H. O'Donnell, T. Dell'Oro, S. Research Center for Neutrino Science Tohoku University Sendai980-8578 Japan Frontier Research Institute for Interdisciplinary Sciences Tohoku University Sendai980-8578 Japan Graduate Program on Physics for the Universe Tohoku University Sendai980-8578 Japan Department of Physics Tohoku University Sendai980-8578 Japan Institute for the Physics and Mathematics of the Universe The University of Tokyo Kashiwa277-8568 Japan Graduate School of Science Osaka University Toyonaka560-0043 Japan Osaka University Osaka Ibaraki567-0047 Japan Graduate School of Advanced Technology and Science Tokushima University Tokushima770-8506 Japan Nuclear Science Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics and Astronomy University of Hawaii at Manoa HonoluluHI96822 United States Massachusetts Institute of Technology CambridgeMA02139 United States Boston University BostonMA02215 United States Department of Physics and Astronomy University of Tennessee KnoxvilleTN37996 United States Triangle Universities Nuclear Laboratory DurhamNC27708 United States The University of North Carolina at Chapel Hill Chapel HillNC27599 United States North Carolina Central University DurhamNC27701 United States Physics Department Duke University DurhamNC27705 United States Center for Experimental Nuclear Physics and Astrophysics University of Washington SeattleWA98195 United States Nikhef The University of Amsterdam Science Park Amsterdam Netherlands Center for Neutrino Physics Virginia Polytechnic Institute State University BlacksburgVA24061 United States

We report the results of a search for MeV-scale astrophysical neutrinos in KamLAND presented as an excess in the number of coincident neutrino interactions associated with the publicly available high-energy neutrino datasets from the IceCube Neutrino Observatory. We find no statistically significant excess in the number of observed low-energy electron antineutrinos in KamLAND, given a coincidence time window of ±500 s, ±1,000 s, ±3,600 s, and ±10,000 s around each of the IceCube neutrinos. We use this observation to present limits from 1.8 MeV to 100 MeV on the electron antineutrino fluence, assuming a mono-energetic flux. We then compare the results to several astrophysical measurements performed by IceCube and place a limit at the 90% confidence level on the electron antineutrino isotropic thermal luminosity from the TXS 0506+056 blazar. Copyright © 2022, The Authors. All rights reserved.

关键词： Electrons

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Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck. I. Construction of CMB lensing maps and modeling choices

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Physical Review D 2023年第2期107卷 023529-023529页

作者： Y. Omori E. J. Baxter C. Chang O. Friedrich A. Alarcon O. Alves A. Amon F. Andrade-Oliveira K. Bechtol M. R. Becker G. M. Bernstein J. Blazek L. E. Bleem H. Camacho A. Campos A. Carnero Rosell M. Carrasco Kind R. Cawthon R. Chen A. Choi J. Cordero T. M. Crawford M. Crocce C. Davis J. DeRose S. Dodelson C. Doux A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole S. Everett X. Fang A. Ferté P. Fosalba M. Gatti G. Giannini D. Gruen R. A. Gruendl I. Harrison K. Herner H. Huang E. M. Huff D. Huterer M. Jarvis E. Krause N. Kuropatkin P.-F. Leget P. Lemos A. R. Liddle N. MacCrann J. McCullough J. Muir J. Myles A. Navarro-Alsina S. Pandey Y. Park A. Porredon J. Prat M. Raveri R. P. Rollins A. Roodman R. Rosenfeld A. J. Ross E. S. Rykoff C. Sánchez J. Sanchez L. F. Secco I. Sevilla-Noarbe E. Sheldon T. Shin M. A. Troxel I. Tutusaus T. N. Varga N. Weaverdyck R. H. Wechsler W. L. K. Wu B. Yanny B. Yin Y. Zhang J. Zuntz T. M. C. Abbott M. Aguena S. Allam J. Annis D. Bacon B. A. Benson E. Bertin S. Bocquet D. Brooks D. L. Burke J. E. Carlstrom J. Carretero C. L. Chang R. Chown M. Costanzi L. N. da Costa A. T. Crites M. E. S. Pereira T. de Haan J. De Vicente S. Desai H. T. Diehl M. A. Dobbs P. Doel W. Everett I. Ferrero B. Flaugher D. Friedel J. Frieman J. García-Bellido E. Gaztanaga E. M. George T. Giannantonio N. W. Halverson S. R. Hinton G. P. Holder D. L. Hollowood W. L. Holzapfel K. Honscheid J. D. Hrubes D. J. James L. Knox K. Kuehn O. Lahav A. T. Lee M. Lima D. Luong-Van M. March J. J. McMahon P. Melchior F. Menanteau S. S. Meyer R. Miquel L. Mocanu J. J. Mohr R. Morgan T. Natoli S. Padin A. Palmese F. Paz-Chinchón A. Pieres A. A. Plazas Malagón C. Pryke C. L. Reichardt A. K. Romer J. E. Ruhl E. Sanchez K. K. Schaffer M. Schubnell S. Serrano E. Shirokoff M. Smith Z. Staniszewski A. A. Stark E. Suchyta G. Tarle D. Thomas C. To J. D. Vieira J. Weller R. Williamson Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA Kavli Institute for Particle Astrophysics and Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ 20921-400 Brazil Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Department of Physics Northeastern University Boston Massachusetts 02115 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue. Argonne Illinois 60439 USA Instituto de Física Teórica Universidade Estadual Paulista São Paulo 01140-070 Brazil Department of Physics Carnegie Mellon University Pittsburgh Pennsylvania 15312 USA Instituto de Astrofisica de Canarias E-38205 La Laguna Tenerife Spain Universidad de La Laguna Departamento Astrofísica E-38206 La Laguna Tenerife Spain Center for Astrophysical Surveys National Center for Supercomputing Applications 1205 West Clark Street Urbana Illinois 61801 USA Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street Urbana Illinois 61801 USA Physic

Joint analyses of cross-correlations between measurements of galaxy positions, galaxy lensing, and lensing of the cosmic microwave background (CMB) offer powerful constraints on the large-scale structure of the Universe. In a forthcoming analysis, we will present cosmological constraints from the analysis of such cross-correlations measured using Year 3 data from the Dark Energy Survey (DES), and CMB data from the South Pole Telescope (SPT) and Planck. Here we present two key ingredients of this analysis: (1) an improved CMB lensing map in the SPT-SZ survey footprint and (2) the analysis methodology that will be used to extract cosmological information from the cross-correlation measurements. Relative to previous lensing maps made from the same CMB observations, we have implemented techniques to remove contamination from the thermal Sunyaev Zel’dovich effect, enabling the extraction of cosmological information from smaller angular scales of the cross-correlation measurements than in previous analyses with DES Year 1 data. We describe our model for the cross-correlations between these maps and DES data, and validate our modeling choices to demonstrate the robustness of our analysis. We then forecast the expected cosmological constraints from the galaxy survey-CMB lensing auto and cross-correlations. We find that the galaxy-CMB lensing and galaxy shear-CMB lensing correlations will on their own provide a constraint on S8=σ8Ωm/0.3 at the few percent level, providing a powerful consistency check for the DES-only constraints. We explore scenarios where external priors on shear calibration are removed, finding that the joint analysis of CMB lensing cross-correlations can provide constraints on the shear calibration amplitude at the 5% to 10% level.

关键词： Cosmic microwave background Cosmological parameters Dark matter Evolution of the Universe Gravitational lenses Large scale structure of the Universe

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Horizons: Nuclear Astrophysics in the 2020s and Beyond

arXiv

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arXiv 2022年

作者： Schatz, Hendrik Becerril Reyes, A.D. Best, A. Brown, E.F. Chatziioannou, K. Chipps, K.A. Deibel, C.M. Ezzeddine, R. Galloway, D.K. Hansen, C.J. Herwig, F. Ji, A.P. Lugaro, M. Meisel, Z. Norman, D. Read, J.S. Roberts, L.F. Spyrou, A. Tews, I. Timmes, F.X. Travaglio, C. Vassh, N. Abia, C. Adsley, P. Agarwal, S. Aliotta, M. Aoki, W. Arcones, A. Aryan, A. Bandyopadhyay, A. Banu, A. Bardayan, D.W. Barnes, J. Bauswein, A. Beers, T.C. Bishop, J. Boztepe, T. Côté, B. Caplan, M.E. Champagne, A.E. Clark, J.A. Couder, M. Couture, A. de Mink, S.E. Debnath, S. deBoer, R.J. den Hartogh, J. Denissenkov, P. Dexheimer, V. Dillmann, I. Escher, J.E. Famiano, M.A. Farmer, R. Fisher, R. Fröhlich, C. Frebel, A. Fryer, C. Fuller, G. Ganguly, A.K. Ghosh, S. Gibson, B.K. Gorda, T. Gourgouliatos, K.N. Graber, V. Gupta, M. Haxton, W. Heger, A. Hix, W.R. Ho, W.C.G. Holmbeck, E.M. Hood, A.A. Huth, S. Imbriani, G. Izzard, R.G. Jain, R. Jayatissa, H. Johnston, Z. Kajino, T. Kankainen, A. Kiss, G.G. Kwiatkowski, A. La Cognata, M. Laird, A.M. Lamia, L. Landry, P. Laplace, E. Launey, K.D. Leahy, D. Leckenby, G. Lennarz, A. Longfellow, B. Lovell, A.E. Lynch, W.G. Lyons, S.M. Maeda, K. Masha, E. Matei, C. Merc, J. Messer, B. Montes, F. Mukherjee, A. Mumpower, M. Neto, D. Nevins, B. Newton, W.G. Nguyen, L.Q. Nishikawa, K. Nishimura, N. Nunes, F.M. O’Connor, E. O’Shea, B.W. Ong, W.-J. Pain, S.D. Pajkos, M.A. Pignatari, M. Pizzone, R.G. Placco, V.M. Plewa, T. Pritychenko, B. Psaltis, A. Puentes, D. Qian, Y.-Z. Radice, D. Rapagnani, D. Rebeiro, B.M. Reifarth, R. Richard, A.L. Rijal, N. Roederer, I.U. Rojo, J.S. Sk, J. Saito, Y. Schwenk, A. Sergi, M.L. Sidhu, R.S. Simon, A. Sivarani, T. Skúladóttir, Á. Smith, M.S. Spiridon, A. Sprouse, T.M. Starrfield, S. Steiner, A.W. Strieder, F. Sultana, I. Surman, R. Szücs, T. Tawfik, A. Thielemann, F. Trache, L. Trappitsch, R. Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Facility for Rare Isotope Beams Michigan State University East LansingMI48824 United States United States Department of Physics University of Naples"Federico II" Napoli80126 Italy INFN - Sezione di Napoli Napoli80126 Italy Department of Computational Mathematics Science and Engineering MichiganState University East LansingMI48824 United States Department of Physics California Institute of Technology PasadenaCA91125 United States LIGO Laboratory California Institute of Technology PasadenaCA91125 United States Physics Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Department of Physics and Astronomy University of Tennessee Knoxville KnoxvilleTN37996 United States Department of Physics and Astronomy Louisiana State University Baton RougeLA70803 United States Department of Astronomy University of Florida GainesvilleFL32601 United States School of Physics and Astronomy Monash University VIC3800 Australia OzGRav-Monash School of Physics & Astronomy Monash University VIC3800 Australia Goethe University Frankfurt Institute for Applied Physics Max-von-Laue-Str. 12 Frankfurt am Main60438 Germany Technical University of Darmstadt Institute for Nuclear Physics Germany Max Planck Institute for Astronomy Heidelberg Germany Department of Physics and Astronomy University of Victoria VictoriaBCV8P 5C2 Canada Department of Astronomy & Astrophysics University of Chicago 5640 S Ellis Avenue ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Excellence Centre of the Hungarian Academy of Sciences Konkoly-Thege Miklós út 15-17 BudapestH-1121 Hungary ELTE Eötvös Loránd University Institute of Physics Pázmány Péter sétány 1/A Budapest1117 Hungary Institute of Nuclear & Particle Physics Department of Physics & Astronomy Ohio University AthensOH45701

Nuclear Astrophysics is a field at the intersection of nuclear physics and astrophysics, which seeks to understand the nuclear engines of astronomical objects and the origin of the chemical elements. This white paper summarizes progress and status of the field, the new open questions that have emerged, and the tremendous scientific opportunities that have opened up with major advances in capabilities across an ever growing number of disciplines and subfields that need to be integrated. We take a holistic view of the field discussing the unique challenges and opportunities in nuclear astrophysics in regards to science, diversity, education, and the interdisciplinarity and breadth of the field. Clearly nuclear astrophysics is a dynamic field with a bright future that is entering a new era of discovery opportunities. © 2022, CC BY-NC-SA.

关键词： Astrophysics

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Intensity interferometry with the MAGIC telescopes 37

Intensity interferometry with the MAGIC telescopes

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37th International Cosmic Ray Conference, ICRC 2021

作者： Delgado Mendez, Carlos Acciari, V.A. Colombo, E. Cortina, J. Diaz, C. Fink, D. Fiori, M. Hassan, T. Jiménez-Martínez, I. Lyard, E. Mangano, S. Mirzoyan, R. Naleto, G. Njoh Ekoume, T. Polo, M. Produit, N. Rodriguez, J.J. Schweizer, T. Walter, R. Wunderlich, C. Zampieri, L. Ansoldi, S. Antonelli, L.A. Arbet Engels, A. Artero, M. Asano, K. Baack, D. Babić, A. Baquero, A. Barres de Almeida, U. Barrio, J.A. Batković, I. Becerra González, J. Bednarek, W. Bellizzi, L. Bernardini, E. Bernardos, M. Berti, A. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Biland, A. Blanch, O. Bökenkamp, H. Bonnoli, G. Bošnjak, Ž. Busetto, G. Carosi, R. Ceribella, G. Cerruti, M. Chai, Y. Chilingarian, A. Cikota, S. Colak, S.M. Contreras, J.L. Covino, S. D'Amico, G. D'Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. Delfino, M. Delgado, J. Depaoli, D. Di Pierro, F. Di Venere, L. Do Souto Espiñeira, E. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsaesser, D. Fallah Ramazani, V. Fattorini, A. Fonseca, M.V. Font, L. Fruck, C. Fukami, S. Fukazawa, Y. García López, R.J. Garczarczyk, M. Gasparyan, S. Gaug, M. Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Green, J.G. Green, D. Hadasch, D. Hahn, A. Heckmann, L. Herrera, J. Hoang, J. Hrupec, D. Hütten, M. Inada, T. Ishio, K. Iwamura, Y. Jiménez Martínez, I. Jormanainen, J. Jouvin, L. Karjalainen, M. Kerszberg, D. Kobayashi, Y. Kubo, H. Kushida, J. Lamastra, A. Lelas, D. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, A. Loporchio, S. Machado de Oliveira Fraga, B. Maggio, C. Majumdar, P. Makariev, M. Mallamaci, M. Maneva, G. Manganaro, M. Mannheim, K. Maraschi, L. Mariotti, M. Martínez, M. Mazin, D. Menchiari, S. Mender, S. Mićanović, S. Miceli, D. Miener, T. Miranda, J.M. Molina, E. Moralejo, A. Morcuende, D. Moreno, V. Moretti, E. Nakamori, T. Nava, L. Neustroev, V. Nigro, C. Nilsson, K. Nishijima, K. Noda, K. Nozaki, S. Ohtani, Y. University of Geneva Department of Astronomy Geneva Switzerland INFN-Padova Padova University Department of Physics and Astronomy Padova Italy INAF - Astronomical Observatory of Padova Padova Italy Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain Università di Udine INFN Trieste UdineI-33100 Italy RomeI-00136 Italy ETH Zürich ZürichCH-8093 Switzerland Bellaterra BarcelonaE-08193 Spain The University of Tokyo Chiba Kashiwa277-8582 Japan Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil Università di Padova INFN PadovaI-35131 Italy University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Università di Siena INFN Pisa SienaI-53100 Italy ZeuthenD-15738 Germany Max-Planck-Institut für Physik MünchenD-80805 Germany Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía s/n Granada18008 Spain Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Armenian MAGIC Group A. Alikhanyan National Science Laboratory Yerevan0036 Armenia Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica Università e del Politecnico di Bari BariI-70125 Italy Croatian MAGIC Group University of Rijeka Department of Physics Rijeka51000 Croatia Universität Würzburg WürzburgD-97074 Germany Finnish MAGIC Group Finnish Centre for Astronomy with ESO University of Turku TurkuFI-20014 Finland Departament de Física CERES IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Japanese MAGIC G

Due to their large mirror size, fast response to single photons, sensitivity and telescope baselines in the order of 100 m, Imaging Atmospheric Cherenkov Telescopes are ideally suited to perform intensity interferometry observations. In 2019 a test readout setup was installed in the two 17-m diameter MAGIC telescopes to allow performing interferometry measurements with them. The first on-sky measurements were able to detect correlated intensity fluctuations consistent with the stellar diameters of three different stars: Adhara (∊ CMa), Benetnasch (η UMa) and Mirzam (β CMa). After the upgrade of the setup in 2021, MAGIC is now equipped with a high-duty-cycle intensity interferometer, already in operation. A technical description of the interferometer and first performance results obtained by measuring several known stellar diameter are presented. © 2022 Sissa Medialab Srl. All rights reserved.

关键词： Interferometry

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Bridging between type IIb and Ib supernovae: SN IIb 2022crv with a very thin Hydrogen envelope

arXiv

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arXiv 2023年

作者： Gangopadhyay, Anjasha Maeda, Keiichi Singh, Avinash Nayana, A.J. Nakaoka, Tatsuya Kawabata, Koji S. Taguchi, Kenta Singh, Mridweeka Chandra, Poonam Ryder, Stuart D. Dastidar, Raya Yamanaka, Masayuki Kawabata, Miho Alsaberi, Rami Z.E. Dukiya, Naveen Teja, Rishabh Singh Ailawadhi, Bhavya Dutta, Anirban Sahu, D.K. Moriya, Takashi J. Misra, Kuntal Tanaka, Masaomi Chevalier, Roger Tominaga, Nozomu Uno, Kohki Imazawa, Ryo Hamada, Taisei Hori, Tomoya Isogai, Keisuke Hiroshima Astrophysical Science Centre Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan Indian Institute of Astrophysics Koramangala 2nd Block Bangalore560034 India Department of Physics Graduate School of Advanced Science and Engineering Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States School of Mathematical and Physical Sciences Macquarie University NSW2109 Australia Astrophysics and Space Technologies Research Centre Macquarie University SydneyNSW2109 Australia Instituto de Astrofísica Universidad Andres Bello Fernandez Concha 700 Las Condes RM Santiago Chile Millennium Institute of Astrophysics Nuncio Monsenor Sótero Sanz 100 Providencia Santiago8320000 Chile Graduate School of Science and Engineering Kagoshima University 1-21-35 Korimoto Kagoshima Kagoshima890-0065 Japan Nishi-Harima Astronomical Observatory Center for Astronomy University of Hyogo 407-2 Nishigaichi Sayo-cho Hyogo Sayo679-5313 Japan Western Sydney University Locked Bag 1797 PenrithNSW2751 Australia Aryabhatta Research Institute of observational sciencES Manora Peak Nainital263 002 India Department of Applied Physics Mahatma Jyotiba Phule Rohilkhand University Bareilly243006 India Pondicherry University Chinna Kalapet Puducherry Kalapet605014 India Department of Physics Deen Dayal Upadhyaya Gorakhpur University Gorakhpur273009 India National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan School of Physics and Astronomy Faculty of Science Monash University ClaytonVIC3800 Australia Astronomical Institute Tohoku University Aoba Sendai980-8578 Japan University Of Virginia Astronomy Building 530 McCormick Road CharlottesvilleVA2290

We present optical, near-infrared, and radio observations of supernova (SN) SN IIb 2022crv. We show that it retained a very thin H envelope and transitioned from a SN IIb to a SN Ib;prominent Hα seen in the pre-maximum phase diminishes toward the post-maximum phase, while He i lines show increasing strength. SYNAPPS modeling of the early spectra of SN 2022crv suggests that the absorption feature at 6200 Å is explained by a substantial contribution of Hα together with Si ii, as is also supported by the velocity evolution of Hα. The light-curve evolution is consistent with the canonical stripped-envelope supernova subclass but among the slowest. The light curve lacks the initial cooling phase and shows a bright main peak (peak MV =−17.82±0.17 mag), mostly driven by radioactive decay of 56Ni. The light-curve analysis suggests a thin outer H envelope (Menv ∼0.05 M☉) and a compact progenitor (Renv ∼3 R☉). An interaction-powered synchrotron self-absorption (SSA) model can reproduce the radio light curves with a mean shock velocity of 0.1c. The mass-loss rate is estimated to be in the range of (1.9−2.8) × 10−5 M☉ yr−1 for an assumed wind velocity of 1000 km s−1, which is on the high end in comparison with other compact SNe IIb/Ib. SN 2022crv fills a previously unoccupied parameter space of a very compact progenitor, representing a beautiful continuity between the compact and extended progenitor scenario of SNe IIb/Ib. Copyright © 2023, The Authors. All rights reserved.

关键词： Supernovae

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Cubic ferromagnet and emergent U(1) symmetry on its phase boundary

arXiv

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arXiv 2022年

作者： Tu, Wei-Lin Lyu, Xinliang Ghazanfari, S.R. Wu, Huan-Kuang Lee, Hyun-Yong Kawashima, Naoki Division of Display and Semiconductor Physics Korea University Sejong30019 Korea Republic of Faculty of Science and Technology Keio University 3-14-1 Hiyoshi Kohoku-ku Yokohama223-8522 Japan Institute for Solid State Physics University of Tokyo Chiba Kashiwa277-8581 Japan Department of Physics Condensed Matter Theory Center Joint Quantum Institute University of Maryland College ParkMD20742 United States Department of Applied Physics Graduate School Korea University Sejong30019 Korea Republic of Interdisciplinary Program in E·ICT-Culture-Sports Convergence Korea University Sejong30019 Korea Republic of Trans-scale Quantum Science Institute The University of Tokyo Bunkyo Tokyo113-0033 Japan

We study the simplest quantum lattice spin model for the two-dimensional (2D) cubic ferromagnet by means of mean-field analysis and tensor network calculation. While both methods give rise to similar results in detecting related phases, the 2D infinite projected entangled-pair state (iPEPS) calculation provides more accurate values of transition points. Near the phase boundary, moreover, our iPEPS results indicate that it is more difficult to pin down the orientation of magnetic easy axes, and we interpret it as the easy-axis softening. This phenomenon implies an emergence of continuous U(1) symmetry, which is indicated by the low-energy effective model and has been analytically shown by the field theory. Our model and study provide a concrete example for utilizing iPEPS near the critical region, showing that the emergent phenomenon living on the critical points can already be captured by iPEPS with a rather small bond dimension. © 2022, CC BY.

关键词： Quantum entanglement

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Precise and extensive characterization of an optical resonator for cavity-based quantum networks

arXiv

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arXiv 2021年

作者： Lee, Dowon Kim, Myunghun Hong, Jungsoo Ha, Taegyu Kim, Junwoo Kang, Sungsam Choi, Youngwoon An, Kyungwon Lee, Moonjoo Pohang37673 Korea Republic of 145 Anam-ro Seongbuk-gu Seoul02841 Korea Republic of Department of Physics Korea University 145 Anam-ro Seongbuk-gu Seoul02841 Korea Republic of Department of Bioengineering Korea University Seoul02841 Korea Republic of Interdisciplinary Program in Precision Public Health Korea University Seoul02841 Korea Republic of Department of Physics and Astronomy Institute of Applied Physics Seoul National University Seoul08826 Korea Republic of

Cavity-based quantum node is a competitive platform for distributed quantum networks. Here, we characterize a high-finesse Fabry-Pérot optical resonator for coupling single or few atomic quantum registers. Our cavity consists of two mirrors with different reflectivities: One has minimal optical loss, and the other high transmission loss where more than 90% of the intracavity photons would be emitted. Cavity finesse, birefringent effects, and mechanical resonances are measured using the lasers at 780, 782, and 795 nm. In order to obtain cavity geometric parameters, we drive the adjacent longitudinal or transverse modes with two lasers simultaneously, and measure those frequencies using a precision wavelength meter (WLM). A major novelty of this method is that the parameters' uncertainties are solely determined by the resolution of the WLM, eliminating all of the temporal environment fluctuations. Our scheme makes it possible to quantify the atom-cavity coupling constant up to four significant figures, the most precise and accurate estimation so far, which would become a key ingredient for benchmarking a cavity-based quantum node. Furthermore, the distortion of polarized photonic qubits would be minimized owing to the small birefringent splitting, below 4.9% of the cavity linewidth. Our system should operate in the intermediate atom-cavity coupling regime that would allow us to implement various quantum network protocols. © 2021, CC BY.

关键词： Birefringence

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In Situ Electric-Field Control of THz Nonreciprocal Directional Dichroism in the Multiferroic Ba2CoGe2O7

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Physical Review Letters 2021年第15期127卷 157201-157201页

作者： J. Vít J. Viirok L. Peedu T. Rõõm U. Nagel V. Kocsis Y. Tokunaga Y. Taguchi Y. Tokura I. Kézsmárki P. Balla K. Penc J. Romhányi S. Bordács Department of Physics Budapest University of Technology and Economics 1111 Budapest Hungary Institute of Physics ASCR Na Slovance 2 182 21 Prague 8 Czech Republic Faculty of Nuclear Science and Physical Engineering Czech Technical University Břehová 7 115 19 Prague 1 Czech Republic National Institute of Chemical Physics and Biophysics Akadeemia tee 23 12618 Tallinn Estonia RIKEN Center for Emergent Matter Science (CEMS) Wako 351-0198 Japan Department of Advanced Materials Science University of Tokyo Kashiwa 277-8561 Japan Department of Applied Physics and Tokyo College University of Tokyo Tokyo 113-8656 Japan Experimental Physics V Center for Electronic Correlations and Magnetism University of Augsburg 86135 Augsburg Germany Institute for Solid State Physics and Optics Wigner Research Centre for Physics P.O. Box. 49 H-1525 Budapest Hungary Department of Physics and Astronomy University of California Irvine 4129 Frederick Reines Hall Irvine California 92697 USA Hungarian Academy of Sciences Premium Postdoctor Program 1051 Budapest Hungary

Nonreciprocal directional dichroism, also called the optical-diode effect, is an appealing functional property inherent to the large class of noncentrosymmetric magnets. However, the in situ electric control of this phenomenon is challenging as it requires a set of conditions to be fulfilled: Special symmetries of the magnetic ground state, spin excitations with comparable magnetic- and electric-dipole activity, and switchable electric polarization. We demonstrate the isothermal electric switch between domains of Ba2CoGe2O7 possessing opposite magnetoelectric susceptibilities. Combining THz spectroscopy and multiboson spin-wave analysis, we show that unbalancing the population of antiferromagnetic domains generates the nonreciprocal light absorption of spin excitations.

关键词： Magnetoelectric effect Magnons Optical & microwave phenomena Antiferromagnets Multiferroics

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The 300 pc resolution imaging of a z = 8.31 galaxy: Turbulent ionized gas and potential stellar feedback 600 million years after the Big Bang

arXiv

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arXiv 2023年

作者： Tamura, Yoichi Bakx, Tom J.L.C. Inoue, Akio K. Hashimoto, Takuya Tokuoka, Tsuyoshi Imamura, Chihiro Hatsukade, Bunyo Lee, Minju M. Moriwaki, Kana Okamoto, Takashi Ota, Kazuaki Umehata, Hideki Yoshida, Naoki Zackrisson, Erik Hagimoto, Masato Matsuo, Hiroshi Shimizu, Ikkoh Sugahara, Yuma Takeuchi, Tsutomu T. Department of Physics Graduate School of Science Nagoya University Furo Chikusa Aichi Nagoya464-8602 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Pure and Applied Physics Graduate School of Advanced Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Faculty of Pure and Applied Sciences University of Tsukuba Ibaraki Tsukuba305-8571 Japan Institute of Astronomy Graduate School of Science The University of Tokyo 2-21-1 Osawa Mitaka Tokyo181-0015 Japan Jagtvej 128 Copenhagen NDK-2200 Denmark DTU-Space Technical University of Denmark Elektrovej 327 Kgs. LyngbyDK-2800 Denmark Giessenbachstr. 1 GarchingD-85748 Germany Research Center for the Early Universe Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan Department of Physics Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan Department of Cosmosciences Graduate School of Science Hokkaido University N10W8 Kitaku Sapporo060-0810 Japan Frontier Science and Social Co-creation Initiative Kanazawa University Kakuma-machi Ishikawa Kanazawa920-1192 Japan Institute for Advanced Research Nagoya University Furo Chikusa Aichi Nagoya464-8601 Japan Observational Astrophysics Department of Physics and Astronomy Uppsala University Box 516 UppsalaSE-751 20 Sweden Department of Literature Shikoku Gakuin University 3-2-1 Bunkyocho Zentsuji Kagawa765-8505 Japan The Research Center for Statistical Machine Learning The Institute of Statistical Mathematics 10-3 Midori-cho Tachikawa Tokyo190—8562 Japan

We present the results of 300 pc resolution ALMA imaging of the [O III] 88 µm line and dust continuum emission from a z = 8.312 Lyman break galaxy MACS0416 Y1. The velocity-integrated [O III] emission has three peaks which are likely associated with three young stellar clumps of MACS0416 Y1, while the channel map shows a complicated velocity structure with little indication of a global velocity gradient unlike what was found in [C II] 158 µm at a larger scale, suggesting random bulk motion of ionized gas clouds inside the galaxy. In contrast, dust emission appears as two individual clumps apparently separating or bridging the [O III]/stellar clumps. The cross correlation coefficient between dust and ultraviolet-related emission (i.e., [O III] and ultraviolet continuum) is unity on a galactic scale, while it drops at © 2023, CC BY.

关键词： Dust

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The SRG/eROSITA All-Sky Survey Subaru/HSC-SSP weak-lensing mass measurements for the eRASS1 Galaxy Clusters

arXiv

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arXiv 2025年

作者： Okabe, Nobuhiro Reiprich, Thomas Grandis, Sebastian Chiu, I-Non Oguri, Masamune Umetsu, Keiichi Bulbul, Esra Bahar, Emre Balzer, Fabian Clerc, Nicolas Comparat, Johan Ghirardini, Vittorio Kleinebreil, Florian Kluge, Matthias Liu, Ang Lin, Yen-Ting Monteiro-Oliveira, Rogério Pacaud, Florian Ceja, Miriam Ramos Sanders, Jeremy Schrabback, Tim Seppi, Riccardo Sommer, Martin Zhang, Xiaoyuan Physics Program Graduate School of Advanced Science and Engineering Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Core Research for Energetic Universe Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Universität Bonn Auf dem Hügel 71 Bonn53121 Germany Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstr. 25/8 Innsbruck6020 Austria Center for Frontier Science Chiba University 1-33 Yayoicho Inage-ku Chiba263-8522 Japan Department of Physics Graduate School of Science Chiba University 1-33 Yayoi-Cho Inage-Ku Chiba263-8522 Japan Institute of Astronomy and Astrophysics Academia Sinica P.O. Box 23-141 Taipei10617 Taiwan Max Planck Institute for Extraterrestrial Physics Giessenbachstrasse 1 Garching85748 Germany IRAP Université de Toulouse CNRS UPS CNES Toulouse France Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China

We perform individual weak-lensing (WL) mass measurements for 78 eROSITA’s first All-Sky Survey (eRASS1) clusters in the footprint of Hyper Suprime-Cam Subaru Strategic program (HSC-SSP) S19A, without any priors of the eRASS1 X-ray quantities or assumption of the mass and concentration relation. In the sample, we find 3 clusters are mis-associated with optical counterparts and 12 clusters are poorly fitted with an NFW profile. The average mass for the 12 poor-fit clusters changes from ∼ 1014h−701 M☉ to ∼ 2 × 1013h−701 M☉ when lensing contamination from surrounding mass structures is taken into account. The scaling relations between the true mass and cluster richness and X-ray count-rate agree well with the results of the eRASS1 Western Galactic Hemisphere region based on count-rate-inferred masses, which are calibrated with the HSC-SSP, DES, and KiDS surveys. We develop a Bayesian framework for inferring the mass-concentration relation of the cluster sample, explicitly incorporating the effects of weak-lensing mass calibration in the mass-concentration parameter space. The redshift-dependent mass and concentration relation is in excellent agreement with predictions of dark-matter-only numerical simulations and previous studies using X-ray-selected clusters. Based on the two-dimensional (2D) WL analysis, the offsets between the WL-determined centers and the X-ray centroids for 36 eRASS1 clusters with high WL S/N are described by two Gaussian components. We find that the mis-centering effect with X-ray centroids is smaller than that with peaks in the galaxy maps. Stacked mass maps support a small mis-centering effect even for clusters with low WL S/N. The projected halo ellipticity is 〈Ε〉 = 0.45 at M200 ∼ 4 × 1014h−701 M☉, in agreement with results of numerical simulations and previous studies of clusters more than twice our mass. Copyright © 2025, The Authors. All rights reserved.

关键词： Dark Matter

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