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作者： Kopacz, Monika Breeze, Victoria Kondragunta, Shobha Frost, Gregory Anenberg, Susan Bruhwiler, Lori Davis, Sean da Silva, Arlindo de Gouw, Joost Duren, Riley Flynn, Lawrence Gaudel, Audrey Geigert, Michael Goldman, Gretchen Joiner, Joanna McDonald, Brian Ott, Lesley Peuch, Vincent-Henri Pusede, Sally E. Stajner, Ivanka Seftor, Colin Sweeney, Colm Valin, Lukas C. Wang, Jun Whetstone, James Kalluri, Satya NOAA/OAR Climate Program Office Silver SpringMD United States NOAA/NESDIS Center for Satellite Applications and Research GreenbeltMD United States NOAA/OAR Climate Program Office Silver Spring Maryland and NOAA/OAR/Chemical Sciences Laboratory BoulderCO United States Milken Institute School of Public Health George Washington University WashingtonDC United States NOAA/OAR Global Monitoring Laboratory BoulderCO United States NOAA/OAR/Chemical Sciences Laboratory BoulderCO United States NASA Goddard Space Flight Center GreenbeltMD United States Cooperative Institute for Research in Environmental Sciences Department of Chemistry University of Colorado Boulder BoulderCO United States Carbon Mapper Inc. Pasadena California and Arizona Institute for Resilient Environments and Societies and Research The University of Arizona TucsonAZ United States Connecticut Department of Energy and Environmental Protection HartfordCT United States Office of Science and Technology Policy WashingtonDC United States European Centre for Medium-Range Weather Forecasts Reading United Kingdom Department of Environmental Sciences University of Virginia CharlottesvilleVA United States NOAA/NWS/Environmental Modeling Center College ParkMD United States Center for Environmental Measurements and Modeling U.S. EPA Research Triangle ParkNC United States Department of Chemical and Biochemical Engineering University of Iowa Iowa CityIA United States National Institute of Standards and Technology GaithersburgMD United States

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JCMT 850 µm continuum observations of density structures in the G35 molecular complex

arXiv

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arXiv 2024年

作者： Shen, Xianjin Liu, Hong-Li Ren, Zhiyuan Tej, Anandmayee Li, Di Liu, Hauyu Baobab Fuller, Gary A. Xie, Jinjin Jiao, Sihan Yang, Aiyuan Koch, Patrick M. Xu, Fengwei Sanhueza, Patricio Diep, Pham Ngoc Peretto, Nicolas Yadav, Ram K. Kramer, Busaba H. Sugiyama, Koichiro Rawlings, Mark G. Lee, Chang Won Tatematsu, Kenichi Harsono, Daniel Eden, David Kwon, Woojin Tsai, Chao-Wei White, Glenn J. Kim, Kee-Tae Liu, Tie Wang, Ke Zhang, Siju Jiao, Wenyu Yang, Dongting Swagat, R. Das Wu, Jingwen Wang, Chen School of Physics and Astronomy Yunnan University Kunming650091 China National Astronomical Observatories Chinese Academy of Sciences Datun Road A20 Beijing China CAS Key Laboratory of FAST NAOC Chinese Academy of Sciences Beijing China University of Chinese Academy of Sciences Beijing China Indian Institute of Space Science and Technology Kerala Thiruvananthapuram695 547 India University of KwaZulu-Natal Durban4000 South Africa Department of Physics National Sun Yat-Sen University No. 70 Lien-Hai Road Kaohsiung City80424 Taiwan Center of Astronomy and Gravitation National Taiwan Normal University Taipei116 Taiwan Jodrell Bank Centre for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Physikalisches Institut University of Cologne Zülpicher Str. 77 KölnD-50937 Germany Key Laboratory of Radio Astronomy and Technology Chinese Academy of Sciences A20 Datun Road Datun Road A20 Beijing China Max-Plank-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Academia Sinica Institute of Astronomy and Astrophysics No. 1 Sec. 4 Roosevelt Road Taipei10617 Taiwan Kavli Institute for Astronomy and Astrophysics Peking University 5 Yiheyuan Road Haidian District Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China National Astronomical Observatory of Japan National Institutes of Natural Sciences 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 Vietnam National Space Center Vietnam Academy of Science and Technology 18 Hoang Quoc Viet Hanoi Viet Nam Cardiff Hub for Astrophysics Research & Technology School of Physics & Astronomy Cardiff University Queens Buildings The Parade CardiffCF24 3AA United Kingdom Sirindhorn AstroPark 260 Moo 4 T. Donkaew A. Maerim Chiangmai50180 Thailand Gemini Observato

Filaments are believed to play a key role in high-mass star formation. We present a systematic study of the filaments and their hosting clumps in the G35 molecular complex using JCMT SCUBA-2 850 µm continuum data. We identified five clouds in the complex and 91 filaments within them, some of which form 10 hub-filament systems (HFSs), each with at least 3 hub-composing filaments. We also compiled a catalogue of 350 dense clumps, 183 of which are associated with the filaments. We investigated the physical properties of the filaments and clumps, such as mass, density, and size, and their relation to star formation. We find that the global mass-length trend of the filaments is consistent with a turbulent origin, while the hub-composing filaments of high line masses (ml > 230 M☉ pc−1) in HFSs deviate from this relation, possibly due to feedback from massive star formation. We also find that the most massive and densest clumps (R > 0.2 pc, M > 35 M☉, Σ > 0.05 g cm−2) are located in the filaments and in the hubs of HFS with the latter bearing a higher probability of occurrence of high-mass star-forming signatures, highlighting the preferential sites of HFSs for high-mass star formation. We do not find significant variation in the clump mass surface density across different evolutionary environments of the clouds, which may reflect the balance between mass accretion and stellar feedback. Copyright © 2024, The Authors. All rights reserved.

关键词： Giant stars

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Application of artificial intelligence in endoscopic image analysis for the diagnosis of a gastric cancer pathogen-Helicobacter pylori infection

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Scientific Reports 2023年第1期13卷 1-12页

作者： Lin, Chih-Hsueh Hsu, Ping-I Tseng, Chin-Dar Chao, Pei-Ju Wu, I-Ting Ghose, Supratip Shih, Chih-An Lee, Shen-Hao Ren, Jia-Hong Shie, Chang-Bih Lee, Tsair-Fwu Department of Electronic Engineering National Kaohsiung University of Science and Technology Kaohsiung 80778 Taiwan Medical Physics and Informatics Laboratory of Electronic Engineering National Kaohsiung University of Science and Technology Kaohsiung 80778 Taiwan Division of Gastroenterology Department of Medicine An Nan Hospital China Medical University Tainan Taiwan Department of Education and Research An Nan Hospital China Medical University Tainan Taiwan Division of Gastroenterology and Hepatology Department of Internal Medicine Antai Medical Care Corporation Antai Tian-Sheng Memorial Hospital Pingtung County Donggan Taiwan Department of Nursing Meiho University Pingtung County Neipu Taiwan Department of Radiation Oncology Linkou Chang Gung Memorial Hospital and Chang Gung University College of Medicine Linkou Taiwan Department of Medical Imaging and Radiological Sciences Kaohsiung Medical University Kaohsiung 80708 Taiwan PhD Program in Biomedical Engineering Kaohsiung Medical University Kaohsiung 80708 Taiwan School of Dentistry College of Dental Medicine Kaohsiung Medical University Kaohsiung 80708 Taiwan

Helicobacter pylori (H. pylori) infection is the principal cause of chronic gastritis, gastric ulcers, duodenal ulcers, and gastric cancer. In clinical practice, diagnosis of H. pylori infection by a gastroenterologists’ impression of endoscopic images is inaccurate and cannot be used for the management of gastrointestinal diseases. The aim of this study was to develop an artificial intelligence classification system for the diagnosis of H. pylori infection by pre-processing endoscopic images and machine learning methods. Endoscopic images of the gastric body and antrum from 302 patients receiving endoscopy with confirmation of H. pylori status by a rapid urease test at An Nan Hospital were obtained for the derivation and validation of an artificial intelligence classification system. The H. pylori status was interpreted as positive or negative by Convolutional Neural Network (CNN) and Concurrent Spatial and Channel Squeeze and Excitation (scSE) network, combined with different classification models for deep learning of gastric images. The comprehensive assessment for H. pylori status by scSE-CatBoost classification models for both body and antrum images from same patients achieved an accuracy of 0.90, sensitivity of 1.00, specificity of 0.81, positive predictive value of 0.82, negative predicted value of 1.00, and area under the curve of 0.88. The data suggest that an artificial intelligence classification model using scSE-CatBoost deep learning for gastric endoscopic images can distinguish H. pylori status with good performance and is useful for the survey or diagnosis of H. pylori infection in clinical practice. © 2023, Springer Nature Limited.

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The SCUBA-2 Large eXtragalactic Survey: 850 μm map, catalogue and the bright-end number counts of the XMM-LSS field

arXiv

引用

arXiv 2023年

作者： Garratt, T.K. Geach, J.E. Tamura, Y. Coppin, K.E.K. Franco, M. Ao, Y. Chen, C.-C. Cheng, C. Clements, D.L. Dai, Y.S. Dannerbauer, H. Greve, T.R. Hatsukade, B. Hwang, H.S. Jiang, L. Kohno, K. Koprowski, M.P. Michalowski, M.J. Sawicki, M. Scott, D. Shim, H. Takeuchi, T.T. Wang, W.-H. Xue, Y.Q. Yang, C. Centre for Astrophysics Research University of Hertfordshire HatfieldAL10 9AB United Kingdom Division of Particle and Astrophysical Science Nagoya University Aichi Nagoya464-8602 Japan Purple Mountain Observatory Key Laboratory for Radio Astronomy Chinese Academy of Sciences 10 Yuanhua Road Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China Academia Sinica Institute of Astronomy and Astrophysics No. 1 Section 4 Roosevelt Road Taipei10617 Taiwan Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Imperial College London Blackett Lab Prince Consort Road LondonSW7 2AZ United Kingdom National Astronomical Observatories Chinese Academy of Sciences 20A Datun RoadChaoyang District Beijing100101 China Tenerife La LagunaE-38205 Spain Universidad de La Laguna Dpto. Astrofísica Tenerife La LagunaE-38206 Spain National Space Institute DTU Space Technical University of Denmark Elektrovej 327 Kgs. LyngbyDK-2800 Denmark Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Institute of Astronomy Graduate School of Science The University of Tokyo 2-21-1 Osawa Tokyo Mitaka181-0015 Japan Astronomy Program Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Center Astronomy Program Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Kavli Institute for Astronomy and Astrophysics Peking University No. 5 Yiheyuan Road Haidian District Beijing100871 China Institute of Astronomy Faculty of Physics Astronomy and Informatics Nicolaus Copernicus University Grudziadzka 5 Torun87-100 Poland Astronomical Observatory Institute Faculty of Physics Adam Mickiewicz University ul. Sloneczna 36 Poznań60-286 Poland Department of Astronomy and P

We present 850 μm imaging of the XMM-LSS field observed for 170 hours as part of the James Clerk Maxwell Telescope SCUBA-2 Large eXtragalactic Survey (S2LXS). S2LXS XMM-LSS maps an area of 9 deg2, reaching a moderate depth of 1σ 4 mJy beam−1. This is the largest contiguous area of extragalactic sky mapped by JCMT at 850 μm to date. The wide area of the S2LXS XMM-LSS survey allows us to probe the ultra-bright (S850μm & 15 mJy), yet rare submillimetre population. We present the S2LXS XMM-LSS catalogue, which comprises 40 sources detected at >5σ significance, with deboosted flux densities in the range of 7 mJy to 48 mJy. We robustly measure the bright-end of the 850 μm number counts at flux densities >7 mJy, reducing the Poisson errors compared to existing measurements. The S2LXS XMM-LSS observed number counts show the characteristic upturn at bright fluxes, expected to be motivated by local sources of submillimetre emission and high-redshift strongly lensed galaxies. We find that the observed 850 μm number counts are best reproduced by model predictions that include either strong lensing or source blending from a 15 arcsec beam, indicating that both may make an important contribution to the observed over-abundance of bright single dish 850 μm selected sources. We make the S2LXS XMM-LSS 850 μm map and >5σ catalogue presented here publicly available. Copyright © 2023, The Authors. All rights reserved.

关键词： Blending

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The ALMA-QUARKS survey: Detection of two extremely dense substructures in a massive prestellar core

arXiv

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arXiv 2024年

作者： Mai, Xiaofeng Liu, Tie Liu, Xunchuan Zhu, Lei Garay, Guido Goldsmith, Paul F. Juvela, Mika Liu, Hongli Mannfors, Emma Tej, Anandmayee Sanhueza, Patricio Li, Shanghuo Xu, Fengwei Semadeni, Enrique Vazquez Jiao, Wenyu Peng, Yaping Baug, T. Yang, Aiyuan Dewangan, Lokesh Bronfman, Leonardo Gómez, Gilberto C. Palau, Aina Lee, Chang Won Qin, Sheng-Li Tatematsu, Ken'ichi Chibueze, James O. Yang, Dongting Lu, Xing Luo, Qiuyi Gu, Qilao Issac, Namitha Zhang, Suinan Li, Pak-Shing Zhang, Bo Tóth, L. Viktor Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China School of Astronomy and Space Sciences University of Chinese Academy of Sciences No. 19A Yuquan Road Beijing100049 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Department of Physics University of Helsinki P.O. box 64 FI-00014 Finland Department of Astronomy Yunnan University Kunming650091 China Indian Institute of Space Science and Technology Thiruvananthapuram695 547 India National Astronomical Observatory of Japan National Institutes of Natural Sciences 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 Max Planck Institute for Astronomy Königstuhl 17 HeidelbergD-69117 Germany Kavli Institute for Astronomy and Astrophysics Peking University 5 Yiheyuan Road Haidian District Beijing100871 China Instituto de Radioastronomía y Astrofísica Universidad Nacional Autónoma de México Antigua Carretera a Pátzcuaro 8701 Ex-Hda. San José de la Huerta Michoacán Morelia58089 Mexico Department of Astronomy School of Physics Peking University Beijing100871 China Department of Physics Faculty of Science Kunming University of Science and Technology Kunming650500 China S. N. Bose National Centre for Basic Sciences Block JD Sector III Salt Lake Kolkata700106 India National Astronomical Observatories Chinese Academy of Sciences A20 Datun Road Chaoyang District Beijing100101 China Physical Research Laboratory Navrangpura Ahmedabad380009 India Departamento de Astronomá Universidad de Chile Las Condes Santiago7591245 Chile Korea Astronomy and Space Scien

Only a handful of massive starless core candidates have been discovered so far, but none of them have been fully confirmed. Within the MM1 clump in the filamentary infrared dark cloud G34.43+0.24 that was covered by the ALMA-ATOMS survey at Band 3 (∼ 2'', 6000 au) and the ALMA-QUARKS survey at Band 6 (∼ 0.3'', 900 au), two prestellar core candidates MM1-C and E1 with masses of 71 and 20 Mo and radii of 2100-4400 au were discovered. The two cores show no obvious sign of star-formation activities. In particular, MM1-C is a very promising massive prestellar core candidate with a total gas mass of 71 Mo. Within MM1-C, we detected two extremely dense substructures, C1 and C2, as characterized by their high densities of nH2 ∼ 108-9cm-3. Moreover, evidence of further fragmentation in C2 was also revealed. We have detected the primordial fragmentation in the earliest stage of massive star formation, and we speculate that MM1-C would be the birthplace of a massive multiple system. However, we cannot fully rule out the possibility that the massive prestellar core MM1-C will just form a cluster of low-mass stars if it undergoes further fragmentation. Copyright © 2024, The Authors. All rights reserved.

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Analysis of in-flight spatial disorientation among military pilots in taiwan

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Journal of Medical sciences (Taiwan) 2021年第1期41卷 22-28页

作者： Tu, Min-Yu Cheng, Chao-Chien Hsin, Yi-Hsiang Huang, Wun-Wei Li, Fang-Ling Hu, Je-Ming Chiang, Kwo-Tsao Lai, Chung-Yu Aviation Physiology Research Laboratory Kaohsiung Armed Forces General Hospital Gangshan Branch Kaohsiung City Taiwan Department of Health Business Administration Meiho University Pingtung County Taiwan Department of Life Sciences and PhD Program in Translational Medicine National Chung Hsing University Taichung City Taiwan Institute of Medical Science and Technology National Sun Yat-sen University Kaohsiung City Taiwan Department of Psychiatry Tri-Service General Hospital Beitou Branch National Defense Medical Center Taipei City Taiwan Division of Colorectal Surgery Department of Surgery Tri-Service General Hospital National Defense Medical Center Taipei City Taiwan Graduate Institute of Medical Sciences National Defense Medical Center Taipei City Taiwan Graduate Institute of Aerospace and Undersea Medicine National Defense Medical Center Taipei City Taiwan

Background: In-flight spatial disorientation (SD) is a predominant threat to flight safety in aviation. This study was conducted to understand the prevalence, severity, and frequency of in-flight SD among military pilots in Taiwan. Methods: A survey was conducted to collect tri-service pilots' experiences of SD during flight. Participants completed anonymous SD questionnaires during refresher physiology training. There were 486 questionnaires delivered to trainees and the completion rate was 97.1% (n = 472). All data were processed using SPSS version 24 software (IBM, Armonk, NY, USA). Results: Of the 472 participants, the average age of the pilots was 36.7 so 7.3 years and 97.7% were male. About 80% of participants experienced in-flight SD events. There was a significant difference between prevalence of SD in fighter (87.0%), trainer (89.8%), transporter (70.6%), and helicopter (66.7%) pilots (P < 0.001). Less than 10% of the events were severe, and there was no obvious variation between aircraft types (P = 0.126). Pilots were sensitive to SD in clouds and under low visibility. Over 70% of pilots experienced visual illusions, especially loss of horizon during bad weather (45.1%), followed by leans (44.5%), false horizon (44.1%), false sense in clouds (39.6%), Coriolis illusion (25.0%), and confusion on entry to instrument meteorological conditions (25.0%). Conclusions: Our survey showed that SD is a common physiological problem among military pilots, who were easily disoriented by in-flight SD without visual cues. Visual illusion was relatively more frequent, especially for trainer and fighter pilots. © 2021 Wolters Kluwer Medknow Publications. All rights reserved.

关键词： coriolis illusion illusion instrument meteorological conditions Spatial disorientation visibility

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Cerium features in kilonova near-infrared spectra: implication from a chemically peculiar star

arXiv

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arXiv 2023年

作者： Tanaka, Masaomi Domoto, Nanae Aoki, Wako Ishigaki, Miho N. Wanajo, Shinya Hotokezaka, Kenta Kawaguchi, Kyohei Kato, Daiji Lee, Jae-Joon Lee, Ho-Gyu Hirano, Teruyuki Kotani, Takayuki Kuzuhara, Masayuki Nishikawa, Jun Omiya, Masashi Tamura, Motohide Ueda, Akitoshi Astronomical Institute Tohoku University Aoba Sendai980-8578 Japan Division for the Establishment of Frontier Sciences Organization for Advanced Studies Tohoku University Sendai980-8577 Japan 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 Am Mühlenberg 1 Potsdam-GolmD-14476 Germany Research Center for the Early Universe Graduate School of Science University of Tokyo Bunkyo Tokyo113-0033 Japan UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Institute for Cosmic Ray Research The University of Tokyo Chiba Kashiwa277-8582 Japan Center for Gravitational Physics Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan National Institute for Fusion Science 322-6 Oroshi-cho Toki509-5292 Japan Interdisciplinary Graduate School of Engineering Sciences Kyushu University Fukuoka Kasuga816-8580 Japan Korea Astronomy and Space Science Institute 776 Daedeok-daero Yuseong-gu Daejeon34055 Korea Republic of Space Policy Research Center Science and Technology Policy Institute 370 Sicheong-daero Sejong30147 Korea Republic of Astrobiology Center 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan

Observations of the kilonova from a neutron star merger event GW170817 opened a way to directly study r-process nucleosynthesis by neutron star mergers. It is, however, challenging to identify the individual elements in the kilonova spectra due to lack of complete atomic data, in particular, at near-infrared wavelengths. In this paper, we demonstrate that spectra of chemically peculiar stars with enhanced heavy element abundances can provide us with an excellent astrophysical laboratory for kilonova spectra. We show that the photosphere of a late B-type chemically peculiar star HR 465 has similar lanthanide abundances and ionization degrees with those in the line forming region in a kilonova at ∼ 2.5 days after the merger. The near-infrared spectrum of HR 465 taken with Subaru/IRD indicates that Ce III lines give the strongest absorption features around 16,000 Å and there are no other comparably strong transitions around these lines. The Ce III lines nicely match with the broad absorption features at 14,500 Å observed in GW170817 with a blueshift of v = 0.1c, which supports recent identification of this feature as Ce III by Domoto et al. (2022). © 2023, CC BY.

关键词： Absorption spectroscopy

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ANTARCTICA AND THE SOUTHERN OCEAN

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BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY 2023年第9期104卷 S322-S365页

作者： Clem, Kyle R. Raphael, Marilyn N. School of Geography Environment and Earth Sciences Victoria University of Wellington Wellington New Zealand Scripps Institution of Oceanography University of California San Diego La Jolla California Department of Atmospheric and Oceanic Sciences University of Colorado Boulder Boulder Colorado Earth Science Observation Center Cooperative Institute for Research in Environmental Sciences (ESOC/CIRES) University of Colorado Boulder Boulder Colorado Argentine Naval Hydrographic Service Buenos Aires Argentina Department of Earth and Environmental Science Temple University Philadelphia Pennsylvania Department of Meteorology University of Valparaíso Valparaíso Chile Center for Climate and Resilience Research (CR)2 Santiago Chile British Antarctic Survey Cambridge United Kingdom Science Systems and Applications Inc. Lanham Maryland NASA Goddard Space Flight Center Greenbelt Maryland Royal Netherlands Meteorological Institute (KNMI) DeBilt The Netherlands Department of Marine Sciences University of Gothenburg Gothenburg Sweden Department of Geography Ohio University Athens Ohio NASA Jet Propulsion Laboratory Pasadena California NOAA/OAR Earth System Research Laboratory Global Monitoring Division Boulder Colorado University of Colorado Boulder Boulder Colorado National Oceanography Centre Southampton United Kingdom. Antarctic Meteorological Research and Data Center Space Science and Engineering Center University of Wisconsin-Madison Madison Wisconsin Department of Physical Sciences School of Arts and Sciences Madison Area Technical College Madison Wisconsin Australian Bureau of Meteorology and Institute for Marine and Antarctic Studies (IMAS) University of Tasmania Hobart Australia Earth Science and Observation Center CIRES University of Colorado Boulder Colorado University of St. Andrews St Andrews United Kingdom Princeton University Princeton New Jersey Australian Antarctic Division Australian Antarctic Program Partnership (AAPP) and Australian Centre fo

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GLOBAL OCEANS

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Bulletin of the American Meteorological Society 2024年第8期105卷 S156-S213页

作者： Johnson, G.C. Lumpkin, R. NOAA/OAR Pacific Marine Environmental Laboratory Seattle Washington NOAA/OAR Atlantic Oceanographic and Meteorological Laboratory Miami Florida NOAA/OAR Physical Sciences Laboratory Boulder Colorado KBR Inc. Greenbelt Maryland NASA Goddard Space Flight Center Greenbelt Maryland NOAA/NESDIS National Centers for Environmental Information Silver Spring Maryland Cooperative Institute for Climate Ocean and Ecosystem Studies University of Washington Seattle Washington Universities Space Research Association Columbia Maryland College of Marine Science University of South Florida St. Petersburg Florida School of Ocean and Earth Science University of Southampton Southampton United Kingdom International Center for Climate and Environment Sciences Institute of Atmospheric Physics Chinese Academy of Sciences Beijing China Rosenstiel School of Marine Atmospheric and Earth Science University of Miami Miami Florida School of Earth and Atmospheric Sciences Georgia Institute of Technology Atlanta Georgia Science Systems and Applications Inc. Lanham Maryland ADNET Systems Inc. Hampton Virginia Department of Atmospheric and Oceanic Sciences University of Colorado Boulder Boulder Colorado Scripps Institution of Oceanography University of California San Diego La Jolla California Cooperative Institute for Marine and Atmospheric Studies University of Miami Miami Florida Cooperative Institute for Satellite Earth System Studies North Carolina State University Asheville North Carolina Center for Coastal Physical Oceanography Old Dominion University Norfolk Virginia Australian Antarctic Program Partnership Institute for Marine and Antarctic Studies Australian Research Council Centre of Excellence for Climate Extremes University of Tasmania Hobart Australia NOAA/NWS National Centers for Environmental Prediction Climate Prediction Center College Park Maryland NOAA/NESDIS National Centers for Environmental Information Asheville North Carolina Department of Atmosphere Ocean an

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JASMINE image simulator for high-precision astrometry and photometry

arXiv

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arXiv 2024年

作者： Kamizuka, Takafumi Kawahara, Hajime Ohsawa, Ryou Kataza, Hirokazu Kawata, Daisuke Yamada, Yoshiyuki Hirano, Teruyuki Miyakawa, Kohei Aizawa, Masataka Omiya, Masashi Yano, Taihei Kano, Ryouhei Wada, Takehiko Löffler, Wolfgang Biermann, Michael Ramos, Pau Isobe, Naoki Usui, Fumihiko Hattori, Kohei Yoshioka, Satoshi Tatekawa, Takayuki Izumiura, Hideyuki Fukui, Akihiko Miyoshi, Makoto Tatsumi, Daisuke Gouda, Naoteru Institute of Astronomy Graduate School of Science The University of Tokyo 2-21-1 Osawa Tokyo Mitaka181-0015 Japan Institute of Space and Astronautical Science Japan Aerospace Exploration Agency 3-1-1 Yoshinodai Chuo-ku Kanagawa Sagamihara252-5210 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Tokyo Mitaka181-8588 Japan Mullard Space Science Laboratory University College London Holmbury St. Mary Surrey DorkingRH5 6NT United Kingdom Department of Physics Kyoto University Kitashirakawa-oiwake-cho Sakyo-ku Kyoto606-8502 Japan Astrobiology Center 2-21-1 Osawa Tokyo Mitaka181-8588 Japan Tsung-Dao Lee Institute Shanghai Jiao Tong University Shengrong Road 520 Shanghai201210 China Astronomisches Rechen-Institut Zentrum für Astronomie Der Universität Heidelberg Mönchhofstr. 12-14 Heidelberg69120 Germany The Institute of Statistical Mathematics 10-3 Midori-cho Tokyo Tachikawa190-8562 Japan Department of Marine Electronics and Mechanical Engineering Tokyo University of Marine Science and Technology 4-5-7 Konan Minato-ku Tokyo108-8477 Japan Kochi College 200-1 Monobe Kochi Nankoku783-8508 Japan Waseda Research Institute for Science and Engineering Waseda University 1-104 Totsukamachi Shinjuku-ku Tokyo169-8050 Japan Subaru Telescope Okayama Branch National Astronomical Observatory of Japan 3037-5 Honjo Kamogata Okayama Asakuchi719-0232 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Tokyo Mitaka181-8588 Japan

JASMINE is a Japanese planned space mission that aims to reveal the formation history of our Galaxy and discover habitable exoEarths. For these objectives, the JASMINE satellite performs high-precision astrometric observations of the Galactic bulge and high-precision transit monitoring of M-dwarfs in the near-infrared (1.0—1.6 µm in wavelength). For feasibility studies, we develop an image simulation software named JASMINE-imagesim, which produces realistic observation images. This software takes into account various factors such as the optical point spread function (PSF), telescope jitter caused by the satellite’s attitude control error (ACE), detector flat patterns, exposure timing differences between detector pixels, and various noise factors. As an example, we report a simulation for the feasibility study of astrometric observations using JASMINE-imagesim. The simulation confirms that the required position measurement accuracy of 4 milliarcseconds for a single exposure of 12.5-mag objects is achievable if the telescope pointing jitter uniformly dilutes the PSF across all stars in the field of view. On the other hand, the simulation also demonstrates that the combination of realistic pointing jitter and exposure timing differences in the detector can significantly degrade accuracy and prevent achieving the requirement. This means that certain countermeasures against this issue must be developed. This result implies that this kind of simulation is important for mission planning and advanced developments to realize more realistic simulations help us to identify critical issues and also devise effective solutions. © 2024, CC BY.

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