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arXiv 2024年

作者： Gupta, Rahul Pandey, S.B. Gupta, S. Chattopadhayay, T. Bhattacharya, D. Bhalerao, V. Castro-Tirado, A.J. Valeev, A. Ror, A.K. Sharma, V. Racusin, J. Aryan, A. Iyyani, S. Vadawale, S. Astrophysics Science Division NASA Goddard Space Flight Center Mail Code 661 GreenbeltMD20771 United States NASA Postdoctoral Program Manora Peak Nainital263002 India Bhabha Atomic Research Center Maharashtra Mumbai400094 India Homi Bhabha National Institute Maharashtra Mumbai400094 India Kavli Institute of Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall StanfordCA94305 United States Department of Physics Ashoka University Haryana Sonipat131029 India Indian Institute of Technology Bombay Powai Maharashtra Mumbai400076 India Glorieta de la Astronomía s/n GranadaE-18008 Spain Departamento de Ingeniería de Sistemas y Automática Escuela de Ingenierías Universidad de Málaga C. Dr. Ortiz Ramos sn MálagaE-29071 Spain Special Astrophysical Observatory of Russian Academy of Sciences Nizhniy Arkhyz Russia University of Maryland Baltimore County BaltimoreMD21250 United States Center for Research and Exploration in Space Science and Technology NASA/GSFC GreenbeltMD20771 United States Graduate Institute of Astronomy National Central University 300 Jhongda Road Jhongli32001 Taiwan Indian Institute of Science Education and Research Kerala Thiruvananthapuram695551 India Physical Research Laboratory Thaltej Gujarat Ahmedabad380009 India

The radiation mechanism underlying the prompt emission remains unresolved and can be resolved using a systematic and uniform time-resolved spectro-polarimetric study. In this paper, we investigated the spectral, temporal, and polarimetric characteristics of five bright GRBs using archival data from AstroSat CZTI, Swift BAT, and Fermi GBM. These bright GRBs were detected by CZTI in its first year of operation, and their average polarization characteristics have been published in Chattopadhyay et al. (2022). In the present work, we examined the time-resolved (in 100-600 keV) and energyresolved polarization measurements of these GRBs with an improved polarimetric technique such as increasing the effective area and bandwidth (by using data from low-gain pixels), using an improved event selection logic to reduce noise in the double events and extend the spectral bandwidth. In addition, we also separately carried out detailed time-resolved spectral analyses of these GRBs using empirical and physical synchrotron models. By these improved time-resolved and energy-resolved spectral and polarimetric studies (not fully coupled spectro-polarimetric fitting), we could pin down the elusive prompt emission mechanism of these GRBs. Our spectro-polarimetric analysis reveals that GRB 160623A, GRB 160703A, and GRB 160821A have Poynting flux-dominated jets. On the other hand, GRB 160325A and GRB 160802A have baryonic-dominated jets with mild magnetization. Furthermore, we observe a rapid change in polarization angle by ∼ 90 degrees within the main pulse of very bright GRB 160821A, consistent with our previous results. Our study suggests that the jet composition of GRBs may exhibit a wide range of magnetization, which can be revealed by utilizing spectro-polarimetric investigations of the bright GRBs. Copyright © 2024, The Authors. All rights reserved.

关键词： Polarimeters

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A fuzzy expert system-based adaptive learning approach to improving students’ learning performances by considering affective and cognitive factors

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Computers and education: Artificial Intelligence 2020年 1卷

作者： Hwang, Gwo-Jen Sung, Han-Yu Chang, Shao-Chen Huang, Xing-Ci Graduate Institute of Digital Learning and Education National Taiwan University of Science and Technology 43 Sec.4 Keelung Rd. Taipei106 Taiwan Department of Allied Health Education and Digital Learning National Taipei University of Nursing and Health Sciences No.365 Ming-te Road Peitou District Taipei City Taiwan Department of International Bachelor Program in Informatics and the Department of Information Communication Yuan Ze University No. 135 Yuandong Rd. Zhongli Dist. Taoyuan City320 Taiwan

Scholars have indicated the importance of providing guidance and support for individual learners. In the past decades, most studies have developed adaptive learning systems to address this issue mainly based on students’ cognitive status, such as their learning achievements. However, several educators have pointed out the need to take learners’ affective status into account. Therefore, this study proposed an expert system approach by taking into account both the affective and cognitive status of individual learners. An adaptive learning system was implemented based on the proposed approach. In addition, an experiment was conducted in a fifth-grade Mathematics course to compare the learning performances and perceptions of the students who learned with the adaptive learning system with affective and cognitive status analysis, a cognitive-status-based adaptive learning system, and a conventional learning system. The ANCOVA results revealed that the adaptive learning model with the affective and cognitive performance analysis mechanism outperformed the other two approaches in terms of improving the students’ learning achievement (F = 3.12, p © 2020 The Author(s)

关键词： expert systems

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The ALMA Survey of 70 μm Dark High-mass Clumps in early Stages (ASHeS). X. Hot Gas Reveals Deeply embedded Star Formation

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Astrophysical Journal 2024年第2期963卷 163-163页

作者： Izumi, Natsuko Sanhueza, Patricio Koch, Patrick M. Lu, Xing Li, Shanghuo Sabatini, Giovanni Olguin, Fernando A. Zhang, Qizhou Nakamura, Fumitaka Tatematsu, Ken’ichi Morii, Kaho Sakai, Takeshi Tafoya, Daniel Institute of Astronomy and Astrophysics Academia Sinica No. 1 Section 2 Roosevelt Road Taipei 10617 Taiwan National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai 200030 China Max Planck Institute for Astronomy Konigstuhl 17 Heidelberg D-69117 Germany INAF Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze I-50125 Italy Institute of Astronomy National Tsing Hua University Hsinchu 30013 Taiwan Center for Astrophysics Harvard & Smithsonian 60 Garden Street Cambridge 02138 MA United States Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan Graduate School of Informatics and Engineering The University of Electro-Communications Chofu Tokyo 182-8585 Japan Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory Onsala SE-439 92 Sweden

Massive infrared dark clouds (IRDCs) are considered to host the earliest stages of high-mass star formation. In particular, 70 μm dark IRDCs are the colder and more quiescent clouds. At a scale of about 5000 au using formaldehyde (H₂CO) emission, we investigate the kinetic temperature of dense cores in 12 IRDCs obtained from the pilot Atacama Large Millimeter/submillimeter Array Survey of 70 μm dark High-mass clumps in early Stages (ASHeS). Compared to the 1.3 mm dust continuum and other molecular lines, such as C¹⁸O and deuterated species, we find that H₂CO is mainly sensitive to low-velocity outflow components rather than to quiescent gas expected in the early phases of star formation. The kinetic temperatures of these components range from 26 to 300 K. The Mach number reaches about 15 with an average value of about 4, suggesting that the velocity distribution of gas traced by H₂CO is significantly influenced by a supersonic nonthermal component. In addition, we detect warm line emission from HC₃N and OCS in 14 protostellar cores, which requires high excitation temperatures (e _u/k ∼ 100 K). These results show that some of the embedded cores in the ASHeS fields are in an advanced evolutionary stage, previously unexpected for 70 μm dark IRDCs. © 2024. The Author(s). Published by the American Astronomical Society.

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The Japanese Vision for the Black Hole explorer Mission

arXiv

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arXiv 2024年

作者： Akiyama, Kazunori Niinuma, Kotaro Hada, Kazuhiro Doi, Akihiro Hagiwara, Yoshiaki Higuchi, Aya e. Honma, Mareki Kawashima, Tomohisa Kolev, Dimitar Koyama, Shoko Masui, Sho Ohsuga, Ken Sano, Hidetoshi Takami, Hideki Tsunetoe, Yuh Uzawa, Yoshinori Akahori, Takuya Akiyama, Yuto Galison, Peter Hayashi, Takayuki J. Hirota, Tomoya Inoue, Makoto Iwata, Yuhei Johnson, Michael D. Kino, Motoki Kofuji, Yutaro Mizuno, Yosuke Moriyama, Kotaro Nagai, Hiroshi Nakamura, Kenta Notsu, Shota Ono, Fumie Oya, Yoko Oyama, Tomoaki Rana, Hannah Saida, Hiromi Saito, Ryo Saito, Yoshihiko Sasada, Mahito Sawada-Satoh, Satoko Takahashi, Mikiya M. Takamura, Mieko Tong, edward Tsuji, Hiroyuki Yoshioka, Shogo Watanabe, Yoshimasa Massachusetts Institute of Technology Haystack Observatory WestfordMA01886 United States Mizusawa VLBI Observatory National Astronomical Observatory of Japan Iwate023-0861 Japan Black Hole Initiative Harvard University CambridgeMA02138 United States Graduate School of Sciences and Technology for Innovation Yamaguchi University Yamaguchi753-8512 Japan The Graduate School of Science Nagoya City University Aichi467-0001 Japan Institute of Space and Astronautical Science Japan Aerospace Exploration Agency Kanagawa252-5210 Japan Department of Space and Astronautical Science The Graduate University for Advanced Studies SOKENDAI Kanagawa229-8510 Japan Natural Science Laboratory Toyo University Tokyo112-8606 Japan Division of Science School of Science and Engineering Tokyo Denki University Saitama350-0394 Japan Department of Astronomy Graduate School of Science The University of Tokyo Tokyo113-0033 Japan Institute for Cosmic Ray Research The University of Tokyo Chiba277-8582 Japan Space Communication Systems Laboratory Wireless Networks Research Center National Institute of Information and Communications Technology Tokyo184-8795 Japan Graduate School of Science and Technology Niigata University Niigata950-2181 Japan Advanced Technology Center National Astronomical Observatory of Japan Tokyo181-8588 Japan Center for Computational Sciences University of Tsukuba Ibaraki305-8577 Japan Faculty of Engineering Gifu University Gifu501-1193 Japan Harvard University CambridgeMA02138 United States Azabu Junior and Senior High School Tokyo106-0046 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI Tokyo181-8588 Japan Institute of Astronomy and Astrophysics Academia Sinica Taipei10617 Taiwan Center for Astrophysics Harvard & Smithsonian CambridgeMA02138 United States Kogakuin University of Technology & Engineering Academic Support Center 2665-1 Nakano Hachioji Tokyo192-0015 Japan Tsung-Dao Lee Institut

The Black Hole explorer (BHeX) is a next-generation space very long baseline interferometry (VLBI) mission concept that will extend the ground-based millimeter/submillimeter arrays into space. The mission, closely aligned with the science priorities of the Japanese VLBI community, involves an active engagement of this community in the development of the mission, resulting in the formation of the Black Hole explorer Japan Consortium. Here we present the current Japanese vision for the mission, ranging from scientific objectives to instrumentation. The Consortium anticipates a wide range of scientific investigations, from diverse black hole physics and astrophysics studied through the primary VLBI mode, to the molecular universe explored via a potential single-dish observation mode in the previously unexplored 50-70 GHz band that would make BHeX the highest-sensitivity explorer ever of molecular oxygen. A potential major contribution for the onboard instrument involves supplying essential elements for its high-sensitivity dual-band receiving system, which includes a broadband 300 GHz SIS mixer and a space-certified multi-stage 4.5K cryocooler akin to those used in the Hitomi and XRISM satellites by the Japan Aerospace exploration Agency. Additionally, the Consortium explores enhancing and supporting BHeX operations through the use of millimeter/submillimeter facilities developed by the national Astronomical Observatory of Japan, coupled with a network of laser communication stations operated by the national Institute of Information and Communication technology. Copyright © 2024, The Authors. All rights reserved.

关键词： Radio astronomy

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The ALMA Survey of 70 μm Dark High-mass Clumps in early Stages (ASHeS). XI. Statistical Study of early Fragmentation

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Astrophysical Journal 2024年第2期966卷 171-171页

作者： Morii, Kaho Sanhueza, Patricio Zhang, Qizhou Nakamura, Fumitaka Li, Shanghuo Sabatini, Giovanni Olguin, Fernando A. Beuther, Henrik Tafoya, Daniel Izumi, Natsuko Tatematsu, Ken’ichi Sakai, Takeshi Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Center for Astrophysics Harvard & Smithsonian 60 Garden Street Cambridge 02138 MA United States Max Planck Institute for Astronomy Königstuhl 17 Heidelberg D-69117 Germany INAF-Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze I-50125 Italy Institute of Astronomy National Tsing Hua University Hsinchu 30013 Taiwan Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory Onsala 439 92 Sweden Academia Sinica Institute of Astronomy and Astrophysics 11F of AS/NTU Astronomy-Mathematics Building No.1 Section 4 Roosevelt Road Taipei 10617 Taiwan Graduate School of Informatics and Engineering The University of Electro-Communications Chofu Tokyo 182-8585 Japan

Fragmentation during the early stages of high-mass star formation is crucial for understanding the formation of high-mass clusters. We investigated fragmentation within 39 high-mass star-forming clumps as part of the Atacama Large Millimeter/submillimeter Array Survey of 70 μm Dark High-mass Clumps in early Stages (ASHeS) survey. Considering projection effects, we have estimated core separations for 839 cores identified from the continuum emission and found mean values between 0.08 and 0.32 pc within each clump. We find compatibility of the observed core separations and masses with the thermal Jeans length and mass, respectively. We also present subclump structures revealed by the 7 m array continuum emission. Comparison of the Jeans parameters using clump and subclump densities with the separation and masses of gravitationally bound cores suggests that they can be explained by clump fragmentation, implying the simultaneous formation of subclumps and cores within rather than a step-by-step hierarchical fragmentation. The number of cores in each clump positively correlates with the clump surface density and the number expected from the thermal Jeans fragmentation. We also find that the higher the fraction of protostellar cores, the larger the dynamic range of the core mass, implying that the cores are growing in mass as the clump evolves. The ASHeS sample exhibits various fragmentation patterns: aligned, scattered, clustered, and subclustered. Using the Q -parameter, which can help distinguish between centrally condensed and subclustered spatial core distributions, we finally find that in the early evolutionary stages of high-mass star formation, cores tend to follow a subclustered distribution. © 2024. The Author(s). Published by the American Astronomical Society.

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The ALMA Survey of 70 µm Dark High-mass Clumps in early Stages (ASHeS). X: Hot Gas Reveals Deeply embedded Star Formation

arXiv

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arXiv 2023年

作者： Izumi, Natsuko Sanhueza, Patricio Koch, Patrick M. Lu, Xing Li, Shanghuo Sabatini, Giovanni Olguin, Fernando A. Zhang, Qizhou Nakamura, Fumitaka Tatematsu, Ken'ichi Morii, Kaho Sakai, Takeshi Tafoya, Daniel Institute of Astronomy and Astrophysics Academia Sinica No. 1 Section 4 Roosevelt Road Taipei10617 Taiwan 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 Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Max Planck Institute for Astronomy Konigstuhl 17 HeidelbergD-69117 Germany INAF Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 FirenzeI-50125 Italy Institute of Astronomy National Tsing Hua University Hsinchu30013 Taiwan Center for Astrophysics |Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Astronomy Graduate School of Science The University of Tokyo Bunkyo-ku Tokyo113-0033 Japan Graduate School of Informatics and Engineering The University of Electro-Communications Chofu Tokyo182-8585 Japan Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory OnsalaSE-439 92 Sweden

Massive infrared dark clouds (IRDCs) are considered to host the earliest stages of high-mass star formation. In particular, 70 µm dark IRDCs are the colder and more quiescent clouds. At a scale of about 5000 au using formaldehyde (H2CO) emission, we investigate the kinetic temperature of dense cores in 12 IRDCs obtained from the pilot ALMA Survey of 70 µm dark High-mass clumps in early Stages (ASHeS). Compared to 1.3 mm dust continuum and other molecular lines, such as C18O and deuterated species, we find that H2CO is mainly sensitive to low-velocity outflow components rather than to quiescent gas expected in the early phases of star formation. The kinetic temperatures of these components range from 26 to 300 K. The Mach number reaches about 15 with an average value of about 4, suggesting that the velocity distribution of gas traced by H2CO is significantly influenced by a supersonic non-thermal component. In addition, we detect warm line emission from HC3N and OCS in 14 protostellar cores, which requires high excitation temperatures (eu/k ∼ 100 K). These results show that some of the embedded cores in the ASHeS fields are in an advanced evolutionary stage, previously unexpected for 70 µm dark IRDCs. Copyright © 2023, The Authors. All rights reserved.

关键词： Giant stars

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The magnetic field in quiescent star-forming filament G16.96+0.27

arXiv

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arXiv 2024年

作者： Gu, Qi-Lao Liu, Tie Shen, Zhi-Qiang Jiao, Sihan Montillaud, Julien Juvela, Mika Lu, Xing Lee, Chang Won Liu, Junhao Li, Pak Shing Liu, Xunchuan Johnstone, Doug Kwon, Woojin Kim, Kee-Tae Tatematsu, Ken’ichi Sanhueza, Patricio Ristorcelli, Isabelle Koch, Patrick Zhang, Qizhou Pattle, Kate Hirano, Naomi Alina, Dana Di Francesco, James Shanghai Astronomical Observatory Chinese Academy of Sciences No.80 Nandan Road Xuhui Shanghai200030 China National Astronomical Observatories Chinese Academy of Sciences A20 Datun Road Chaoyang Beijing100101 China Université de Franche-Comté CNRS Institut UTINAM OSU THETA BesançonF-25000 France Department of Physics University of Helsinki PO box 64 FI-00014 Finland Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of University of Science and Technology 217 Gajeong-ro Yuseong-gu Daejeon34113 Korea Republic of National Astronomical Observatory of Japan 2-21-1 Osawa Tokyo Mitaka181-8588 Japan NRC Herzberg Astronomy and Astrophysics 5071 West Saanich Rd VictoriaBCV9E 2E7 Canada Department of Physics and Astronomy University of Victoria VictoriaBCV8P 5C2 Canada Department of Earth Science Education Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of The Center for Educational Research Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Nobeyama Radio Observatory National Astronomical Observatory of Japan National Institutes of Natural Sciences Nobeyama Minamimaki Minamisaku Nagano384-1305 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Tokyo Mitaka181-8588 Japan IRAP Université de Toulouse CNRS 9 avenue du Colonel Roche BP 44346 Toulouse31028 Cedex 4 France Academia Sinica Institute of Astronomy and Astrophysics No. 1 Section 4 Roosevelt Road Taipei10617 Taiwan Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department of Physics School of Science and Technology Nazarbayev University Astana010000 Kazakhs

We present 850 µm thermal dust polarization observations with a resolution of 14.4′′(∼ 0.13 pc) towards an infrared dark cloud G16.96+0.27 using JCMT/POL-2. The average magnetic field orientation, which roughly agrees with the larger-scale magnetic field orientation traced by the Planck 353 GHz data, is approximately perpendicular to the filament structure. The estimated plane-of-sky magnetic field strength is ∼ 96 µG and ∼ 60 µG using two variants of the Davis-Chandrasekhar-Fermi methods. We calculate the virial and magnetic critical parameters to evaluate the relative importance of gravity, the magnetic field, and turbulence. The magnetic field and turbulence are both weaker than gravity, but magnetic fields and turbulence together are equal to gravity, suggesting that G16.96+0.27 is in a quasi-equilibrium state. The cloud-magnetic-field alignment is found to have a trend moving away from perpendicularity in the dense regions, which may serve as a tracer of potential fragmentation in such quiescent filaments. © 2024, CC BY.

关键词： Stars

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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

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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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Correction to: Species-level characterization of gut microbiota and their metabolic role in kidney stone formation using full-length 16S rRNA sequencing

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Urolithiasis 2024年第1期52卷 150页

作者： Bashir Hussain Chin-Chia Wu Hsin-Chi Tsai Jung-Sheng Chen Aslia Asif Ming-Chin Cheng Yeong-Chin Jou Bing-Mu Hsu Department of Earth and Environmental Sciences National Chung Cheng University Chiayi County Taiwan. Department of Biomedical Sciences National Chung Cheng University Chiayi County Taiwan. Division of Colorectal Surgery Dalin Tzu Chi Hospital Buddhist Tzu Chi Medical Foundation Chiayi County Taiwan. College of Medicine Tzu Chi University Hualien Taiwan. School of Post-Baccalaureate Chinese Medicine Tzu Chi University Hualien Taiwan. Department of Psychiatry School of Medicine Tzu Chi University Hualien Taiwan. Department of Psychiatry Tzu-Chi General Hospital Hualien Taiwan. Department of Medical Research E-Da Hospital I-Shou University Kaohsiung Taiwan. nicky071214@***. Doctoral Program in Science Technology Environment and Mathematics National Chung Cheng University Chiayi Taiwan. Department of Urology Ditmanson Medical Foundation Chiayi Christian Hospital Chiayi County Taiwan. Department of Urology St. Martin De Porres Hospital Chiayi County Taiwan. Department of Medical Research Dalin Tzu Chi Hospital The Buddhist Tzu Chi Medical Foundation Chiayi County Taiwan.

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Pruritus and Its Association With Cancer and Mortality in Dermatomyositis and Polymyositis: A Nationwide Cohort Study in taiwan From 2005 to 2022

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Dermatologic Therapy 2025年第1期2025卷

作者： Der-Jr Huang Yu-Hsuan Joni Shao Yi-Hsien Shih Woan-Ruoh Lee Ling-Ya Huang Yu-Min Kuo Quoc Thao Trang Pham Hao-Jui Weng Department of Dermatology Taipei Medical University-Shuang Ho Hospital New Taipei City Taiwan shh.org.tw Graduate Institute of Biomedical Informatics College of Medical Science and Technology Taipei Medical University Taipei Taiwan tmu.edu.tw Clinical Big Data Research Center Taipei Medical University Hospital Taipei Taiwan tmuh.org.tw Health Data Analytics and Statistics Center Office of Data Science Taipei Medical University Taipei Taiwan tmu.edu.tw Department of Dermatology School of Medicine College of Medicine Taipei Medical University Taipei Taiwan tmu.edu.tw Graduate Institute of Medical Sciences College of Medicine Taipei Medical University Taipei Taiwan tmu.edu.tw Division of Allergy Immunology and Rheumatology Department of Internal Medicine National Taiwan University Hospital and National Taiwan University Taipei Taiwan ntu.edu.tw Graduate Institute of Clinical Medicine College of Medicine National Taiwan University Taipei Taiwan ntu.edu.tw International Ph.D. Program in Cell Therapy and Regenerative Medicine College of Medicine Taipei Medical University Taipei Taiwan tmu.edu.tw Department of Dermatology Faculty of Medicine University of Medicine and Pharmacy at Ho Chi Minh City Ho Chi Minh City Vietnam hcmut.edu.vn Graduate Institute of Clinical Medicine College of Medicine Taipei Medical University Taipei Taiwan medcol.mw

Background: Pruritus is the most common initial symptom reported by patients with dermatomyositis (DM) and polymyositis (PM). However, there is limited data regarding the impact of pruritus on cancer and mortality in patients with DM and PM. In this study, we aimed to investigate how pruritus is associated with cancer and mortality in patients with DM and PM. Methods: This nationwide, population-based retrospective cohort study included adult DM and PM patients from taiwan’s national Health Insurance Research Database between 2005 and 2022. Sex- and age-matched pruritic patients, identified by over 6 weeks of antipruritic medication use, and nonpruritic patients were analyzed. The primary outcome was cancer occurrence or all-cause mortality. The association between pruritus and these outcomes was estimated using Cox proportional hazards models. Results: Among 919 matched pairs of pruritic and nonpruritic patients, cancer was observed in 19.96% in the long-term pruritic group (LPG), 14.63% in the short-term pruritic group (SPG), and 10.34% in the non-pruritic group (NPG) ( p < 0.0001). All-cause mortality was documented as 30.37% in the LPG, 29.69% in the SPG, and 37.76% in the NPG ( p < 0.0001). After adjusting for sex, age, and other comorbidities, pruritus was associated with an increased risk of cancer (hazard ratio (HR) 1.708, 95% confidence interval (CI) 1.229–2.374) and a lower risk of all-cause mortality (HR 0.483, 95% CI 0.409–0.569). Conclusion: This population-based study revealed that pruritus appeared to be associated with increased risks of cancer and decreased all-cause mortality. Thus, pruritus may serve as a pragmatic factor for risk stratification and tailored treatment strategies in DM and PM. Cancer screening, particularly for nasopharyngeal and breast cancers in east Asian populations, is recommended for patients with DM or PM, especially those presenting with pruritus. Meanwhile, patients without pruritus may require vigilant management for pote

关键词： cancer dermatomyositis idiopathic inflammatory myopathies mortality polymyositis pruritus

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