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37th International Cosmic Ray Conference, ICRC 2021

作者： Rongen, Martin Chirkin, dmitry Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, d. Bernardini, E. Besson, d.Z. Binder, G. Bindig, d. Blaufuss, E. Blot, S. Boddenberg, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Chen, C. Chirkin, d. Choi, K. Clark, B.A. Clark, K. Classen, l. Coleman, A. Collin, G.H. Conrad, J.M. Coppin, P. Correa, P. Cowen, d.F. Cross, R. dappen, C. dave, P. de Clercq, C. delaunay, J.J. dembinski, H. deoskar, K. de Ridder, S. desai, A. desiati, P. de Vries, K.d. de Wasseige, G. de With, M. deYoung, T. dharani, S. diaz, A. díaz-Vélez, J.C. dittmer, M. dujmovic, H. dunkman, M. duVernois, M.A. dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.l. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, l. Fox, d. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gerhardt, l. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, d. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Halve, l. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haungs, A. Hauser, S. Hebecker, d. Helbing, K. Henningsen, F. Hettinger, E.C. Hickford, S. Hignight, J. Hill, C. Hill, G.C. Hoffman, K.d. Hoffmann, R. Hoinka, T. Hokanson-Fasig, B. Hoshina, K. Huang, F. Huber, M. Huber, T. Hultqvist, K. Hünnefeld, M. Hussain, R. In, S. Institute of Physics University of Mainz MainzD-55099 Germany Dept. of Physics and WIPAC University of Wisconsin MadisonWI53706 United States III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics Institute for Global Prominent Research Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United States Dept. of Physics Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Niels Bohr Institute Univers

The IceCube Neutrino Observatory instruments about 1 km3 of deep, glacial ice at the geographic South Pole using 5160 photomultipliers to detect Cherenkov light of charged relativistic particles. Most of IceCube’s science goals rely heavily on an ever more precise understanding of the optical properties of the instrumented ice. A curious light propagation effect observed by the experiment is an anisotropic attenuation, which is aligned with the local flow of the ice. Having recently identified curved photon trajectories resulting from asymmetric light diffusion in the birefringent polycrystalline microstructure of the ice as the most likely underlying cause of this effect, work is now ongoing to optimize the model parameters (effectively deducing the average crystal size and shape in the detector). We present the parametrization of the birefringence effect in our photon propagation simulation, the fitting procedures and results as well as the impact of the new ice model on data-MC agreement. © Copyright owned by the author(s).

关键词： Anisotropy

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Uncertainty quantification of SiP based integrated voltage regulator 22

Uncertainty quantification of SiP based integrated voltage r...

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22nd IEEE Workshop on Signal and Power Integrity, SPI 2018

作者： Barbi, M. Torun, H.M. Swaminathan, M. Stievano, I.S. Canavero, F.G. Besnier, P. School of Electrical and Computer Engineering Georgia Institute of Technology AtlantaGA30332 United States Dipartimento di Elettronica Politecnico di Torino Torino10129 Italy IETR UMR CNRS 6164 Institut d'Electronique et de Télécommunications de Rennes INSA de Rennes Rennes35708 France

ISBN: (纸本)9781538622995

This paper deals with the uncertainty quantification applied to the analysis of Integrated Voltage Regulator (IVR) efficiency. It presents a meta-model based on a sparse polynomial chaos technique, aiming at estimating statistical quantities of a response with a relative low computational cost compared to Monte Carlo (MC) simulation. Results obtained are validated against MC simulation. © 2018 IEEE.

关键词： Voltage regulators

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The FASER detector

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JOURNAl OF INSTRUMENTATION 2024年第5期19卷 P05066页

作者： [Anonymous] Department of Physics and Astronomy Technion — Israel Institute of Technology Haifa 32000 Israel Département de Physique Nucléaire et Corpusculaire University of Geneva CH-1211 Geneva 4 Switzerland Albert Einstein Center for Fundamental Physics Laboratory for High Energy Physics University of Bern Sidlerstrasse 5 CH-3012 Bern Switzerland Department of Physics Chiba University 1-33 Yayoi-cho Inage-ku Chiba 263-8522 Japan Kyushu University Nishi-ku 819-0395 Fukuoka Japan Universität Bonn Regina-Pacis-Weg 3 D-53113 Bonn Germany CERN CH-1211 Geneva 23 Switzerland Nikhef National institute for subatomic physics Science Park 105 1098 XG Amsterdam Netherlands Department of Physics and Astronomy University of California Irvine CA 92697-4575 U.S.A. University of Liverpool Liverpool L69 3BX U.K. Department of Physics Tsinghua University Beijing China INFN Sezione di Genova Via Dodecaneso 33–16146 Genova Italy Affiliated with an international laboratory covered by a cooperation agreement with CERN Institut de Physique des 2 Infinis de Lyon (IP2I) 4 Rue Enrico Fermi 69100 Villeurbanne France Faculté de Physique et Ingénierie University of Strasbourg 3–5 rue de l'Université Strasbourg France 67000 University of Oregon Eugene OR 97403 U.S.A. Turner & Townsend Calverley Ln Low Hall Rd Horsforth Leeds LS18 4GH U.K. Royal Holloway University of London Egham TW20 0EX U.K. Department of Physics Chiba University 1-33 Yayoi-cho Inage-ku Chiba 263-8522 Japan Department of Physics University of Washington PO Box 351560 Seattle WA 98195-1460 U.S.A. Deutsches Elektronen-Synchrotron DESY Notkestr. 85 22607 Hamburg Germany National Institute of Standards and Technology Boulder Colorado 80305 U.S.A. University of Colorado Boulder Colorado 80309-0440 U.S.A. Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot 76100 Israel Department of Physics & Astronomy University of Sussex Sussex House Falmer Brighton BN1 9RH U.K. Nago

FASER, the ForwArd Search ExpeRiment, is an experiment dedicated to searching for light, extremely weakly-interacting particles at CERN's large Hadron Collider (lHC). Such particles may be produced in the very forward direction of the lHC's high-energy collisions and then decay to visible particles inside the FASER detector, which is placed 480m downstream of the ATlAS interaction point, aligned with the beam collisions axis. FASER also includes a sub-detector, FASER.., designed to detect neutrinos produced in the lHC collisions and to study their properties. In this paper, each component of the FASER detector is described in detail, as well as the installation of the experiment system and its commissioning using cosmic-rays collected in September 2021 and during the lHC pilot beam test carried out in October 2021. FASER has successfully started taking lHC collision data in 2022, and will run throughout lHC Run 3.

关键词： Calorimeters Gamma detectors (scintillators, CZT, HPGe, HgI etc) Particle tracking detectors (Solid-state detectors) Spectrometers

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Physical Review d 2022年第5期105卷 052002-052002页

作者： M. Agostini K. Altenmüller S. Appel V. Atroshchenko Z. Bagdasarian d. Basilico G. Bellini J. Benziger R. Biondi d. Bravo B. Caccianiga F. Calaprice A. Caminata P. Cavalcante A. Chepurnov d. d’Angelo S. davini A. derbin A. di Giacinto V. di Marcello X. F. ding A. di ludovico l. di Noto I. drachnev A. Formozov d. Franco C. Galbiati C. Ghiano M. Giammarchi A. Goretti A. S. Göttel M. Gromov d. Guffanti Aldo Ianni Andrea Ianni A. Jany d. Jeschke V. Kobychev G. Korga S. Kumaran M. laubenstein E. litvinovich P. lombardi I. lomskaya l. ludhova G. lukyanchenko l. lukyanchenko I. Machulin J. Martyn E. Meroni M. Meyer l. Miramonti M. Misiaszek V. Muratova B. Neumair M. Nieslony R. Nugmanov l. Oberauer V. Orekhov F. Ortica M. Pallavicini l. Papp l. Pelicci Ö. Penek l. Pietrofaccia N. Pilipenko A. Pocar G. Raikov M. T. Ranalli G. Ranucci A. Razeto A. Re M. Redchuk A. Romani N. Rossi S. Schönert d. Semenov G. Settanta M. Skorokhvatov A. Singhal O. Smirnov A. Sotnikov Y. Suvorov R. Tartaglia G. Testera J. Thurn E. Unzhakov A. Vishneva R. B. Vogelaar F. von Feilitzsch A. Wessel M. Wojcik B. Wonsak M. Wurm S. Zavatarelli K. Zuber G. Zuzel Department of Physics and Astronomy University College London London WC1E 6BT United Kingdom Physik-Department Technische Universität München 85748 Garching Germany National Research Centre Kurchatov Institute 123182 Moscow Russia Institut für Kernphysik Forschungszentrum Jülich 52425 Jülich Germany Dipartimento di Fisica Università degli Studi e INFN 20133 Milano Italy Chemical Engineering Department Princeton University Princeton New Jersey 08544 USA INFN Laboratori Nazionali del Gran Sasso 67010 Assergi (AQ) Italy Physics Department Princeton University Princeton New Jersey 08544 USA Dipartimento di Fisica Università degli Studi e INFN 16146 Genova Italy Physics Department Virginia Polytechnic Institute and State University Blacksburg Virginia 24061 USA Lomonosov Moscow State University Skobeltsyn Institute of Nuclear Physics 119234 Moscow Russia St. Petersburg Nuclear Physics Institute NRC Kurchatov Institute 188350 Gatchina Russia Joint Institute for Nuclear Research 141980 Dubna Russia APC Université de Paris CNRS Astroparticule et Cosmologie Paris F-75013 France Gran Sasso Science Institute 67100 L’Aquila Italy III. Physikalisches Institut B RWTH Aachen University 52062 Aachen Germany Institute of Physics and Cluster of Excellence PRISMA+ Johannes Gutenberg-Universität Mainz 55099 Mainz Germany M. Smoluchowski Institute of Physics Jagiellonian University 30348 Krakow Poland Institute for Nuclear Research of NAS Ukraine 03028 Kyiv Ukraine Department of Physics School of Engineering Physical and Mathematical Sciences Royal Holloway University of London Egham TW20 OEX United Kingdom Institute of Nuclear Research (Atomki) Debrecen 4026 Hungary National Research Nuclear University MEPhI (Moscow Engineering Physics Institute) 115409 Moscow Russia Department of Physics Technische Universität Dresden 01062 Dresden Germany Dipartimento di Chimica Biologia e Biotecnologie Università degli Studi e INFN 06123 Perugia Italy Amherst Center for Funda

liquid scintillator detectors play a central role in the detection of neutrinos from various sources. In particular, it is the only technique used so far for the precision spectroscopy of sub-MeV solar neutrinos, as demonstrated by the Borexino experiment at the Gran Sasso National laboratory in Italy. The benefit of a high light yield, and thus a low energy threshold and a good energy resolution, comes at the cost of the directional information featured by water Cherenkov detectors, measuring B8 solar neutrinos above a few MeV. In this paper we provide the first directionality measurement of sub-MeV solar neutrinos which exploits the correlation between the first few detected photons in each event and the known position of the Sun for each event. This is also the first signature of directionality in neutrinos elastically scattering off electrons in a liquid scintillator target. This measurement exploits the subdominant, fast Cherenkov light emission that precedes the dominant yet slower scintillation light signal. Through this measurement, we have also been able to extract the rate of Be7 solar neutrinos in Borexino. The demonstration of directional sensitivity in a traditional liquid scintillator target paves the way for the possible exploitation of the Cherenkov light signal in future kton-scale experiments using liquid scintillator targets. directionality is important for background suppression as well as the disentanglement of signals from various sources.

关键词： Neutrinos Cherenkov detectors Neutrino detectors Particle data analysis Scintillators

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OGlE-2014-BlG-0221lb: A Jupiter Mass Ratio Companion Orbiting either a late-Type Star or a Stellar Remnant

arXiv

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arXiv 2023年

作者： Kirikawa, Rintaro Sumi, Takahiro Bennett, david P. Suzuki, daisuke Koshimoto, Naoki Miyazaki, Shota Bond, Ian A. Udalski, Andrzej Rattenbury, Nicholas J. Abe, Fumio Barry, Richard Bhattacharya, Aparna Fujii, Hirosane Fukui, Akihiko Hamada, Ryusei Hirao, Yuki Silva, Stela Ishitani Itow, Yoshitaka Matsubara, Yutaka Muraki, Yasushi Olmschenk, Greg Ranc, Clément Satoh, Yuki K. Tomoyoshi, Mio Tristram, Paul J. Vandorou, Aikaterini Yama, Hibiki Yamashita, Kansuke Mróz, Przemek Poleski, Radoslaw Skowron, Jan Szymański, Michal K. Soszyński, Igor Pietrukowicz, Pawel Kozlowski, Szymon Ulaczyk, And Krzysztof Department of Earth and Space Science Graduate School of Science Osaka University Toyonaka Osaka560-0043 Japan MOA collaboration Code 667 NASA Goddard Space Flight Center GreenbeltMD20771 United States Department of Astronomy University of Maryland College ParkMD20742 United States Institute of Space and Astronautical Science Japan Aerospace Exploration Agency 3-1-1 Yoshinodai Chuo Kanagawa Sagamihara252-5210 Japan Institute of Natural and Mathematical Sciences Massey University Auckland0745 New Zealand Warsaw University Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland OGLE collaboration Department of Physics University of Auckland Private Bag 92019 Auckland New Zealand Institute for Space-Earth Environmental Research Nagoya University Nagoya464-8601 Japan Department of Earth and Planetary Science Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Instituto de Astrofísica de Canarias Vía Láctea s/n Tenerife La LagunaE-38205 Spain Institute of Astronomy Graduate School of Science The University of Tokyo 2-21-1 Osawa Mitaka Tokyo181-0015 Japan Department of Physics The Catholic University of America WashingtonDC20064 United States Sorbonne Université CNRS UMR 7095 Institut d’Astrophysique de Paris 98 bis bd Arago Paris75014 France College of Science and Engineering Kanto Gakuin University 1-50-1 Mutsuurahigashi Kanazawa-ku Kanagawa Yokohama236-8501 Japan University of Canterbury Mt. John Observatory P.O. Box 56 Lake Tekapo8770 New Zealand Department of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom

We present the analysis of microlensing event OGlE-2014-BlG-0221, a planetary candidate event discovered in 2014. The photometric light curve is best described by a binary-lens single-source model. Our light curve modeling finds two degenerate models, with event timescales of tE ∼ 70 days and ∼ 110 days. These timescales are relatively long, indicating that the discovered system would possess a substantial mass. The two models are similar in their planetary parameters with a Jupiter mass ratio of q ∼ 10−3 and a separation of s ∼ 1.1. While the shorter timescale model shows marginal detection of a microlensing parallax signal, the longer timescale model requires a higher order effect of microlensing parallax, lens orbital motion or xallarap to explain the deviation in the light curve. However, the modeling shows significant correlation between the higher order effects and suffers the ecliptic degeneracy that results in a failure to determine the parallax parameters. Bayesian inference is used to estimate the physical parameters of the lens, revealing the lens to be either a late-type star supported by the shorter timescale model or a stellar remnant supported by the longer timescale model. If the lens is a remnant, this would be the second planet found by microlensing around a stellar remnant. Since the models predict different values for relative proper motion and source flux, future high angular resolution follow-up observations (e.g. Keck adaptive optics) are required to rule out either of the models. Copyright © 2023, The Authors. All rights reserved.

关键词： Inference engines

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A new approach of MHd flows for UCM fluid over a permeable moving plate with space and temperature dependent internal heat generation/absorption

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AIP Conference Proceedings 2020年第1期2236卷

作者： Jagadish Vaijinath Tawade Mahadev Malikarjun Biradar Shaila Sangangouda Benal 1Department of Mathematics Bheemanna Khandre Institute of Technology Bhalki-585328 Karnataka INDIA 2Department of Mathematics Basaveshwar Engineering College (Autonomous) Bagalkot-587103 Karnataka INDIA 3Department of Mathematics B.L.D.E.A’s V. P. Dr. P. G. Halakatti College of Engineering and Technology Vijayapur-586103 Karnataka INDIA

Present paper investigates a new approach for the MHd boundary layer flow of an incompressible upper-convected Maxwell fluid over a permeable horizontal moving plate influenced by non-uniform heat source/sink parameter. We have reduced the governing PdE’s into a kind of nonlinear OdE’s using similarity transformations. These OdE’s are solved with appropriate boundary conditions by efficient shooting with Runge-Kutta method. The obtained values are tabulated and compared with the earlier published papers.

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Analysis of Wave Propagation Characteristics of a Metamaterial Rod Waveguide

Analysis of Wave Propagation Characteristics of a Metamateri...

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International conference of Electronics, Communication and Aerospace Technology (ICECA)

作者： Palak Patel dipayan Chatterjee S.K. Pathak M.C. Sahoo Department of Electronics and Communication Engineering L. D. College of Engineering Ahmedabad India Microwave and Electron Cyclotron Emission Group Institute for Plasma Research Gandhinagar India

ISBN: (纸本)9781538609668

Metamaterial is an artificial material with negative permittivity and negative permeability. In this paper, the analytical theory of meta material rod has been formulated and dispersion relation is numerically investigated for lower order transverse magnetic modes (TM), transverse electric modes (TE) and hybrid modes (HE and EH) in guided mode. Also, the comparison is given between dielectric rod waveguide and metamaterial rod waveguide.

关键词： Metamaterials Magnetic materials dielectrics Optical waveguides dispersion Permittivity

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2d Theoretically Twistable Material database

arXiv

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arXiv 2024年

作者： Jiang, Yi Petralanda, Urko Skorupskii, Grigorii Xu, Qiaoling Pi, Hanqi Călugăru, dumitru Hu, Haoyu Xie, Jiaze Mustaf, Rose Albu Höhn, Peter Haase, Vicky Vergniory, Maia G. Claassen, Martin Elcoro, luis Regnault, Nicolas Shan, Jie Mak, Kin Fai Efetov, dmitri K. Morosan, Emilia Kennes, dante M. Rubio, Angel Xian, lede Felser, Claudia Schoop, leslie M. Bernevig, B. Andrei Paseo Manuel de Lardizábal San Sebastián20018 Spain Department of Physics University of the Basque Country UPV/EHU Apartado 644 Bilbao48080 Spain Department of Chemistry Princeton University PrincetonNJ08544 United States College of Physics and Electronic Engineering Center for Computational Sciences Sichuan Normal University Chengdu610068 China Tsientang Institute for Advanced Study Zhejiang310024 China Department of Physics Princeton University PrincetonNJ08544 United States Department of Physics Princeton University PrincetonNJ08544 United States Department of Physics and Astronomy Rice University HoustonTX77005 United States Rice University HoustonTX77005 United States Smalley-Curl Institute Rice University HoustonTX77005 United States Max Planck Institute for Chemical Physics of Solids Nöthnitzer Str. 40 Dresden01187 Germany Département de Physique et Institut Quantique Université de Sherbrooke SherbrookeQCJ1K 2R1 Canada Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Center for Computational Quantum Physics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Laboratoire de Physique de l'Ecole normale supérieure ENS Université PSL CNRS Sorbonne Université Université Paris-Diderot Sorbonne Paris Cité Paris75005 France School of Applied and Engineering Physics Cornell University IthacaNY14850 United States Department of Physics Cornell University IthacaNY14850 United States Kavli Institute at Cornell for Nanoscale Science IthacaNY14850 United States Faculty of Physics Ludwig-Maximilians-University Munich Munich80799 Germany Ludwig-Maximilians-University Munich Munich80799 Germany Institut für Theorie der Statistischen Physik RWTH Aachen University JARA-Fundamentals of Future Information Technology Aachen52056 Germany Max Planck Institute for the Structure and Dynamics of Matter Luruper Chaussee 149 Hamburg22761 Germany Nano-Bio Spectroscopy G

The study of twisted two-dimensional (2d) materials, where twisting layers create moiré superlattices, has opened new opportunities for investigating topological phases and strongly correlated physics. While systems such as twisted bilayer graphene (TBG) and twisted transition metal dichalcogenides (TMds) have been extensively studied, the broader potential of a seemingly infinite set of other twistable 2d materials remains largely unexplored. In this paper, we define "theoretically twistable materials" as single- or multi-layer structures that allow for the construction of simple continuum models of their moiré structures. This excludes, for example, materials with a "spaghetti" of bands or those with numerous crossing points at the Fermi level, for which theoretical moiré modeling is unfeasible. We present a high-throughput algorithm that systematically searches for theoretically twistable semimetals and insulators based on the Topological 2d Materials database (2d-TQCdB). By analyzing key electronic properties, we identify thousands of new candidate materials that could host rich topological and strongly correlated phenomena when twisted. We propose representative twistable materials for realizing different types of moiré systems, including materials with different Bravais lattices, valleys, and strength of spin-orbital coupling. We provide examples of crystal growth for several of these materials and showcase twisted bilayer band structures along with simplified twisted continuum models. Our results significantly broaden the scope of moiré heterostructures and provide a valuable resource for future experimental and theoretical studies on novel moiré systems. © 2024, CC BY.

关键词： Continuum mechanics

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Water modeling quantifies the complex role of argon flow on tundish open eye formation

Water modeling quantifies the complex role of argon flow on ...

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AISTech 2018 Iron and Steel Technology Conference and Exposition

作者： Sengupta, Joydeep li, donghui leung, Jackie Chattopadhyay, Kinnor ArcelorMittal Global R and D Hamilton 1390 Burlington Street East HamiltonONL8N 3J5 Canada Department of Materials Science and Engineering University of Toronto 184 College Street TorontoONM5S 3E4 Canada

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Cold dust and low [OIII]/[CII] Ratios: an Evolved Star-forming Population at Redshift 7

arXiv

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arXiv 2023年

作者： Algera, Hiddo S.B. Inami, Hanae Sommovigo, laura Fudamoto, Yoshinobu Schneider, Raffaella Graziani, luca dayal, Pratika Bouwens, Rychard Aravena, Manuel da Cunha, Elisabete Ferrara, Andrea Hygate, Alexander P.S. van leeuwen, Ivana de looze, Ilse Palla, Marco Pallottini, Andrea Smit, Renske Stefanon, Mauro Topping, Michael van der Werf, Paul P. Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Tokyo Mitaka Japan Scuola Normale Superiore Piazza dei Cavalieri 7 PisaI-56126 Italy Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Dipartimento di Fisica Sapienza Universita di Roma Piazzale Aldo Moro 5 RomaI-00185 Italy INAF/Osservatorio Astronomico di Roma via Frascati 33 Monte Porzio Catone RomaI-00078 Italy Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Leiden Observatory Leiden University LeidenNL-2300 RA Netherlands Departamento de Astronomia Universidad de Chile Camino del Observatorio 1515 Las Condes Santiago7591245 Chile International Centre for Radio Astronomy Research University of Western Australia 35 Stirling Hwy CrawleyWA266009 Australia Australia Sterrenkundig Observatorium Ghent University Krijgslaan 281 - S9 Gent9000 Belgium Dept. of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom INAF Osservatorio Astronomico di Trieste Via G.B. Tiepolo 11 Trieste34131 Italy Dipartimento di Fisica Sezione di Astronomia Universitá di Trieste Via G.B. Tiepolo 11 Trieste34131 Italy Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Departament d’Astronomia i Astrofìsica Universitat de València C. Dr. Moliner 50 Burjassot ValènciaE-46100 Spain Spain Steward Observatory University of Arizona 933 N Cherry Ave TucsonAZ85721 United States

We present new AlMA Band 8 (rest-frame 90 μm) observations of three massive (M★ ≈ 1010 Mo) galaxies at z ≈ 7 previously detected in [CII]158 μm and underlying dust continuum emission in the Reionization Era Bright Emission line Survey (REBElS). We detect the dust continuum emission of two of our targets in Band 8 (REBElS-25 and REBElS-38), while REBElS-12 remains undetected. Through modified blackbody fitting we determine cold dust temperatures (Tdust ≈ 30−35 K) in both of the dual-band detected targets, given a fiducial model of optically thin emission with β = 2.0. Their dust temperatures are lower than most z ∼ 7 galaxies in the literature, and consequently their dust masses are higher (Mdust ≈ 108 Mo). Nevertheless, these large dust masses are still consistent with predictions from models of dust production in the early Universe. In addition, we target and detect [OIII]88 μm emission in both REBElS-12 and REBElS-25, and find l[OIII]/l[CII]ratios of approximately unity, low compared to the l[OIII]/l[CII] 2 − 10 observed in the known z 6 population thus far. We argue the lower line ratios are due to a comparatively weaker ionizing radiation field resulting from the less starbursty nature of our targets. This low burstiness supports the cold dust temperatures and below average [OIII]λλ4959, 5007 + Hβ equivalent widths of REBElS-25 and REBElS-38, compared to the known high-redshift population. Overall, this provides evidence for the existence of a massive, dust-rich galaxy population at z ≈ 7 which has previously experienced vigorous star formation, but is currently forming stars in a steady, as opposed to bursty, manner. Copyright © 2023, The Authors. All rights reserved.

关键词： dust

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