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Cover Image, Volume 5, Number 3, March 2023

Carbon Energy 2023年第3期5卷

作者： Jun Yang Xing Li Ke Qu Yixian Wang Kangqi Shen Changhuan Jiang Bo Yu Pan Luo Zhuangzhi Li Mingyang Chen Bingshu Guo Mingshan Wang Junchen Chen Zhiyuan Ma Yun Huang Zhenzhong Yang Pengcheng Liu Rong Huang Xiaodi Ren David Mitlin School of New Energy and Materials Southwest Petroleum University Chengdu China Energy Storage Research Institute Southwest Petroleum University Chengdu China Ke Qu Shenzhen Key Laboratory of Nanobiomechanics Shenzhen Institutes of Advanced Technology Chinese Academy of Sciences Shenzhen 518055 China. China Key Laboratory of Polar Materials and Devices (MOE) and Department of Electronics East China Normal University Shanghai 200062 China. Mingyang Chen Beijing Computational Science Research Center Beijing 100193 China. Center for Green Innovation School of Materials Science and Engineering University of Science and Technology Beijing Beijing 100083 China. Rong Huang China Key Laboratory of Polar Materials and Devices (MOE) and Department of Electronics East China Normal University Shanghai 200062 China. Xiaodi Ren Hefei National Research Center for Physical Sciences at the Microscale Department of Materials Science and Engineering University of Science and Technology of China Hefei Anhui 230026 China. David Mitlin Materials Science Program and Texas Materials Institute The University of Texas at Austin Austin Texas 78712-1591 USA. Shenzhen Key Laboratory of Nanobiomechanics Shenzhen Institutes of Advanced Technology Chinese Academy of Sciences Shenzhen China China Key Laboratory of Polar Materials and Devices (MOE) Department of Electronics East China Normal University Shanghai China Xing Li School of New Energy and Materials Southwest Petroleum University Chengdu China. Materials Science Program and Texas Materials Institute The University of Texas at Austin Austin Texas USA Beijing Computational Science Research Center Beijing China School of Materials Science and Engineering Center for Green Innovation University of Science and Technology Beijing Beijing China Department of Materials Science and Engineering Hefei National Research Center for Physical Sciences at the Microscale University of Science and Technology of China Hefei Anhui China

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Core collapse supernova gravitational wave emission for progenitors of 9.6, 15, and 25M⊙

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Physical Review D 2023年第4期107卷 043008-043008页

作者： Anthony Mezzacappa Pedro Marronetti Ryan E. Landfield Eric J. Lentz R. Daniel Murphy W. Raphael Hix J. Austin Harris Stephen W. Bruenn John M. Blondin O. E. Bronson Messer Jordi Casanova Luke L. Kronzer Department of Physics and Astronomy University of Tennessee 1408 Circle Drive Knoxville Tennessee 37996-1200 USA Physics Division National Science Foundation Alexandria Virginia 22314 USA National Center for Computational Sciences Oak Ridge National Laboratory P.O. Box 2008 Oak Ridge Tennessee 37831-6164 USA Physics Division Oak Ridge National Laboratory P.O. Box 2008 Oak Ridge Tennessee 37831-6354 USA Joint Institute for Nuclear Physics and its Applications Oak Ridge National Laboratory P.O. Box 2008 Oak Ridge Tennessee 37831-6374 USA Department of Physics Florida Atlantic University 777 Glades Road Boca Raton Florida 33431-0991 USA Department of Physics North Carolina State University Raleigh North Carolina 27695-8202 USA Physics Program Community College of Denver P.O. Box 173363 Denver Colorado 80217-3363 USA Department of Aerospace Engineering and Mechanics University of Alabama Box 870280 Tuscaloosa Alabama 35487-0280 USA

We present gravitational wave emission predictions based on three core collapse supernova simulations corresponding to three different progenitor masses. The masses span a large range, between 9.6 and 25M⊙, are all initially nonrotating, and are of two metallicities: zero and solar. We compute both the temporal evolution of the gravitational wave strains for both the plus and the cross polarizations, as well as their spectral decomposition and characteristic strains. The temporal evolution of our zero metallicity 9.6M⊙ progenitor model is distinct from the temporal evolution of our solar metallicity 15M⊙ progenitor model and our zero metallicity 25M⊙ progenitor model. In the former case, the high-frequency gravitational wave emission is largely confined to a brief time period ∼75 ms after bounce, whereas in the latter two cases high-frequency emission does not commence until ∼125 ms after bounce or later. The excitation mechanisms of the high-frequency emission in all three cases correspond to proto-neutron star convection and accretion onto the proto-neutron star from the convective gain layer above it, with the former playing the dominant role for most of the evolution. The low-frequency emission in all three models exhibits very similar behavior. At frequencies below ∼250 Hz, gravitational waves are emitted by neutrino-driven convection and the standing accretion shock instability (SASI). This emission extends throughout the simulations when a gain region is present. In all three models, explosion is observed at ∼125, ∼500, and ∼250 ms after bounce in the 9.6, 15, and 25M⊙ progenitor models, respectively. At these times, the low-frequency gravitational wave emission is joined by very low-frequency emission, below ∼10 Hz. These very low-frequency episodes are the result of explosion and begin at the above designated explosion times in each of our models. Our characteristic strains tell us that, in principle, all three gravitational wave signals would be detec

关键词： Gravitation Gravitational waves Novae & supernovae Transient & explosive astronomical phenomena

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An Open-Source Knowledge Graph Ecosystem for the Life sciences

arXiv

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arXiv 2023年

作者： Callahan, Tiffany J. Tripodi, Ignacio J. Stefanski, Adrianne L. Cappelletti, Luca Taneja, Sanya B. Wyrwa, Jordan M. Casiraghi, Elena Matentzoglu, Nicolas A. Reese, Justin Silverstein, Jonathan C. Hoyt, Charles Tapley Boyce, Richard D. Malec, Scott A. Unni, Deepak R. Joachimiak, Marcin P. Robinson, Peter N. Mungall, Christopher J. Cavalleri, Emanuele Fontana, Tommaso Valentini, Giorgio Mesiti, Marco Gillenwater, Lucas A. Santangelo, Brook Vasilevsky, Nicole A. Hoehndorf, Robert Bennett, Tellen D. Ryan, Patrick B. Hripcsak, George Kahn, Michael G. Bada, Michael Baumgartner, William A. Hunter, Lawrence E. Computational Bioscience Program University of Colorado Anschutz Medical Campus AuroraCO80045 United States Department of Biomedical Informatics Columbia University Irving Medical Center New YorkNY10032 United States Computer Science Department Interdisciplinary Quantitative Biology University of Colorado Boulder BoulderCO80301 United States AnacletoLab Computer Science Department University of Milan 20122 Italy Intelligent Systems Program University of Pittsburgh PittsburghPA15260 United States Department of Physical Medicine and Rehabilitation School of Medicine University of Colorado Anschutz Medical Campus AuroraCO80045 United States Division of Environmental Genomics and Systems Biology Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Semanticly Ltd Athens Greece Department of Biomedical Informatics University of Pittsburgh School of Medicine PittsburghPA15206 United States Laboratory of Systems Pharmacology Harvard Medical School BostonMA02115 United States Division of Translational Informatics University of New Mexico School of Medicine AlbuquerqueNM87131 United States SIB Swiss Institute of Bioinformatics Basel Switzerland Berlin Institute of Health at Charité-Universitatsmedizin Berlin10117 Germany ELLIS European Laboratory for Learning and Intelligent Systems Germany Department of Biomedical Informatics University of Colorado School of Medicine AuroraCO80045 United States Data Collaboration Center Critical Path Institute 1840 E River Rd. Suite 100 TucsonAZ85718 United States Computer Electrical and Mathematical Sciences & Engineering Division Computational Bioscience Research Center King Abdullah University of Science and Technology Thuwal23955-6900 Saudi Arabia Department of Pediatrics University of Colorado School of Medicine AuroraCO80045 United States Janssen Research and Development RaritanNJ08869 United States Division of General Internal Medicine University of Colorado School of Medicine A

Translational research requires data at multiple scales of biological organization. Advancements in sequencing and multi-omics technologies have increased the availability of these data, but researchers face significant integration challenges. Knowledge graphs (KGs) are used to model complex phenomena, and methods exist to construct them automatically. However, tackling complex biomedical integration problems requires flexibility in the way knowledge is modeled. Moreover, existing KG construction methods provide robust tooling at the cost of fixed or limited choices among knowledge representation models. PheKnowLator (Phenotype Knowledge Translator) is a semantic ecosystem for automating the FAIR (Findable, Accessible, Interoperable, and Reusable) construction of ontologically grounded KGs with fully customizable knowledge representation. The ecosystem includes KG construction resources (e.g., data preparation APIs), analysis tools (e.g., SPARQL endpoints and abstraction algorithms), and benchmarks (e.g., prebuilt KGs and embeddings). We evaluated the ecosystem by systematically comparing it to existing open-source KG construction methods and by analyzing its computational performance when used to construct 12 large-scale KGs. With flexible knowledge representation, PheKnowLator enables fully customizable KGs without compromising performance or usability. © 2023, CC BY.

关键词： Ecosystems

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Integrating spatially-resolved transcriptomics data across tissues and individuals: challenges and opportunities

arXiv

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arXiv 2024年

作者： Guo, Boyi Ling, Wodan Kwon, Sang Ho Panwar, Pratibha Ghazanfar, Shila Martinowich, Keri Hicks, Stephanie C. Department of Biostatistics Johns Hopkins Bloomberg School of Public Health BaltimoreMD United States Division of Biostatistics Department of Population Health Sciences Weill Cornell Medicine NY United States Lieber Institute for Brain Development Johns Hopkins Medical Campus BaltimoreMD United States Solomon H. Snyder Department of Neuroscience Johns Hopkins School of Medicine BaltimoreMD United States Biochemistry Cellular and Molecular Biology Graduate Program Johns Hopkins School of Medicine BaltimoreMD United States School of Mathematics and Statistics The University of Sydney NSW2006 Australia Sydney Precision Data Science Centre University of Sydney NSW2006 Australia Charles Perkins Centre The University of Sydney NSW2006 Australia Department of Psychiatry and Behavioral Sciences Johns Hopkins School of Medicine BaltimoreMD United States Johns Hopkins Kavli Neuroscience Discovery Institute BaltimoreMD United States Department of Biomedical Engineering Johns Hopkins University BaltimoreMD United States Center for Computational Biology Johns Hopkins University BaltimoreMD United States Malone Center for Engineering in Healthcare Johns Hopkins University BaltimoreMD United States

Advances in spatially-resolved transcriptomics (SRT) technologies have propelled the development of new computational analysis methods to unlock biological insights. As the cost of generating these data decreases, these technologies provide an exciting opportunity to create large-scale atlases that integrate SRT data across multiple tissues, individuals, species, or phenotypes to perform population-level analyses. Here, we describe unique challenges of varying spatial resolutions in SRT data, as well as highlight the opportunities for standardized preprocessing methods along with computational algorithms amenable to atlas-scale datasets leading to improved sensitivity and reproducibility in the future. © 2024, CC BY-NC-ND.

关键词： Biotic

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Author Correction: The lactate receptor HCAR1 drives the recruitment of immunosuppressive PMN-MDSCs in colorectal cancer

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Nature immunology 2025年第4期26卷 635页

作者： Jiacheng He Xiaolei Chai Qiansen Zhang Yang Wang Yijie Wang Xinyu Yang Jingbo Wu Bo Feng Jing Sun Weiwei Rui Shuyin Ze Yuanyuan Fu Yumiao Zhao Ying Zhang Yao Zhang Meizhen Liu Chuang Liu Meifu She Xiangfei Hu Xueyun Ma Huaiyu Yang Dawei Li Senlin Zhao Guichao Li Zhen Zhang Zhonghui Tian Yanlin Ma Lingyan Cao Bo Yi Dali Li Ruth Nussinov Charis Eng Timothy A Chan Eytan Ruppin J Silvio Gutkind Feixiong Cheng Mingyao Liu Weiqiang Lu Shanghai Key Laboratory of Regulatory Biology Institute of Biomedical Sciences and School of Life Sciences East China Normal University Shanghai China. Department of Urology and Department of Pathology The Fifth People's Hospital of Shanghai Fudan University Shanghai China. Department of General Surgery and Department of Pathology Ruijin Hospital Shanghai Jiaotong University School of Medicine Shanghai China. Research Center for Complexity Sciences Hangzhou Normal University Hangzhou China. Department of Colorectal Surgery Department of Radiation Oncology Fudan University Shanghai Cancer Center Shanghai China. School of Life Sciences Fudan University Shanghai China. Hainan Provincial Key Laboratory for Human Reproductive Medicine and Genetic Research Hainan Provincial Clinical Research Center for Thalassemia Department of Reproductive Medicine Key Laboratory of Reproductive Health Diseases Research and Translation (Hainan Medical University) Ministry of Education The First Affiliated Hospital of Hainan Medical University Haikou China. Shanghai Ninth People's Hospital Shanghai Jiao Tong University School of Medicine College of Stomatology Shanghai Jiao Tong University Shanghai China. Department of Gastrointestinal Surgery The Third Xiangya Hospital Central South University Changsha China. Computational Structural Biology Section Basic Science Program Frederick National Laboratory for Cancer Research National Cancer Institute at Frederick Frederick MD USA. Department of Human Molecular Genetics and Biochemistry Sackler School of Medicine Tel Aviv University Tel Aviv Israel. Genomic Medicine Institute Lerner Research Institute Cleveland Clinic Cleveland OH USA. Department of Molecular Medicine Cleveland Clinic Lerner College of Medicine Case Western Reserve University Cleveland OH USA. Case Comprehensive Cancer Center Case Western Reserve University School of Medicine Cleveland OH USA. Center for Immunotherapy and Precision Immuno-Oncology Cleveland Clini

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EMPRESS. IX. Extremely Metal-Poor Galaxies are Very Gas-Rich Dispersion-Dominated Systems: Will JWST Witness Gaseous Turbulent High-z Primordial Galaxies?

arXiv

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arXiv 2022年

作者： Isobe, Yuki Ouchi, Masami Nakajima, Kimihiko Ozaki, Shinobu Bouché, Nicolas F. Wise, John H. Xu, Yi Emsellem, Eric Kusakabe, Haruka Hattori, Takashi Nagao, Tohru Chiaki, Gen Fukushima, Hajime Harikane, Yuichi Hayashi, Kohei Hirai, Yutaka Kim, Ji Hoon Maseda, Michael V. Nagamine, Kentaro Shibuya, Takatoshi Sugahara, Yuma Yajima, Hidenobu Aoyama, Shohei Fujimoto, Seiji Fukushima, Keita Hatano, Shun Inoue, Akio K. Ishigaki, Tsuyoshi Kawasaki, Masahiro Kojima, Takashi Komiyama, Yutaka Koyama, Shuhei Koyama, Yusei Lee, Chien-Hsiu Matsumoto, Akinori Mawatari, Ken Moriya, Takashi J. Motohara, Kentaro Murai, Kai Nishigaki, Moka Onodera, Masato Ono, Yoshiaki Rauch, Michael Saito, Tomoki Sasaki, Rin Suzuki, Akihiro Takeuchi, Tsutomu T. Umeda, Hiroya Umemura, Masayuki Watanabe, Kuria Yabe, Kiyoto Zhang, Yechi Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan Department of Physics Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan University of Tokyo Chiba Kashiwa277-8583 Japan Univ Lyon Univ Lyon1 ENS de Lyon CNRS Centre de Recherche Astrophysique de Lyon UMR5574 Saint-Genis-LavalF-69230 France Center for Relativistic Astrophysics School of Physics Georgia Institute of Technology AtlantaGA30332 United States Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan European Southern Observatory Karl-Schwarzschild-Straße 2 Garching85748 Germany Observatoire de Genéve Université de Genéve 51 Ch. des Maillettes Versoix1290 Switzerland 650 North A'ohoku Place HiloHI96720 United States Research Center for Space and Cosmic Evolution Ehime University Bunkyo-cho 2-5 Ehime Matsuyama790-8577 Japan Center for Computational Sciences University of Tsukuba Ten-nodai 1-1-1 Tsukuba Ibaraki305-8577 Japan Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom National Institute of Technology Ichinoseki College Hagisho Ichinoseki021-8511 Japan Astronomical Institute Tohoku University 6-3 Aoba Aramaki Aoba-ku Miyagi Sendai980-8578 Japan Department of Physics and Astronomy University of Notre Dame 225 Nieuwland Science Hall Notre DameIN46556 United States Astronomy Program Department of Physics and Astronomy 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 Department of Astronomy University of Wisconsin-Madison 475 N. Charter Street MadisonWI53706 United States Theoretical Astrophysics Department of Earth & Space S

We present kinematics of 6 local extremely metal-poor galaxies (EMPGs) with low metallicities (0.016 − 0.098 Z☉) and low stellar masses (104.7 − 107.6M☉). Taking deep medium-high resolution (R ∼ 7500) integral-field spectra with 8.2-m Subaru, we resolve the small inner velocity gradients and dispersions of the EMPGs with Hα emission. Carefully masking out sub-structures originated by inflow and/or outflow, we fit 3-dimensional disk models to the observed Hα flux, velocity, and velocity-dispersion maps. All the EMPGs show rotational velocities (vrot) of 5-23 km s−1 smaller than the velocity dispersions (σ0) of 17-31 km s−1, indicating dispersion-dominated (vrot/σ0 = 0.29−0.80 gas 0.9 − 1.0. Comparing our results with other Hα kinematics studies, we find that vrot/σ0 decreases and fgas increases with decreasing metallicity, decreasing stellar mass, and increasing specific star-formation rate. We also find that simulated high-z (z ∼ 7) forming galaxies have gas fractions and dynamics similar to the observed EMPGs. Our EMPG observations and the simulations suggest that primordial galaxies are gas-rich dispersion-dominated systems, which would be identified by the forthcoming James Webb Space Telescope (JWST) observations at z ∼ 7. Copyright © 2022, The Authors. All rights reserved.

关键词： Galaxies

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EMPRESS. XII. Statistics on the Dynamics and Gas Mass Fraction of Extremely-Metal Poor Galaxies

arXiv

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arXiv 2023年

作者： Xu, Yi Ouchi, Masami Isobe, Yuki Nakajima, Kimihiko Ozaki, Shinobu Bouché, Nicolas F. Wise, John H. Emsellem, Eric Kusakabe, Haruka Hattori, Takashi Nagao, Tohru Chiaki, Gen Fukushima, Hajime Harikane, Yuichi Hayashi, Kohei Hirai, Yutaka Kim, Ji Hoon Maseda, Michael V. Nagamine, Kentaro Shibuya, Takatoshi Sugahara, Yuma Yajima, Hidenobu Aoyama, Shohei Fujimoto, Seiji Fukushima, Keita Hatano, Shun Inoue, Akio K. Ishigaki, Tsuyoshi Kawasaki, Masahiro Kojima, Takashi Komiyama, Yutaka Koyama, Shuhei Koyama, Yusei Lee, Chien-Hsiu Matsumoto, Akinori Mawatari, Ken Moriya, Takashi J. Motohara, Kentaro Murai, Kai Nishigaki, Moka Onodera, Masato Ono, Yoshiaki Rauch, Michael Saito, Tomoki Sasaki, Rin Suzuki, Akihiro Takeuchi, Tsutomu T. Umeda, Hiroya Umemura, Masayuki Watanabe, Kuria Yabe, Kiyoto Zhang, Yechi Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan University of Tokyo Chiba Kashiwa277-8583 Japan Department of Physics Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan Univ Lyon Univ Lyon1 ENS de Lyon CNRS Centre de Recherche Astrophysique de Lyon UMR5574 Saint-Genis-LavalF-69230 France Center for Relativistic Astrophysics School of Physics Georgia Institute of Technology AtlantaGA30332 United States European Southern Observatory Karl-Schwarzschild-Straße 2 Garching85748 Germany Observatoire de Genéve Université de Genéve 51 Ch. des Maillettes Versoix1290 Switzerland 650 North A’ohoku Place HiloHI96720 United States Research Center for Space and Cosmic Evolution Ehime University Bunkyo-cho 2-5 Ehime Matsuyama790-8577 Japan Center for Computational Sciences University of Tsukuba Ten-nodai 1-1-1 Tsukuba Ibaraki305-8577 Japan Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom National Institute of Technology Ichinoseki College Hagisho Ichinoseki021-8511 Japan Astronomical Institute Tohoku University 6-3 Aoba Aramaki Aoba-ku Miyagi Sendai980-8578 Japan Department of Physics and Astronomy University of Notre Dame 225 Nieuwland Science Hall Notre DameIN46556 United States Astronomy Program Department of Physics and Astronomy 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 Department of Astronomy University of Wisconsin-Madison 475 N. Charter Street MadisonWI53706 United States Theoretical Astrophysics Department of Earth & Space S

We present demography of the dynamics and gas-mass fraction of 33 extremely metal-poor galaxies (EMPGs) with metallicities of 0.015 − 0.195 Zo and low stellar masses of 104 − 108 Mo in the local universe. We conduct deep optical integral-field spectroscopy (IFS) for the low-mass EMPGs with the medium high resolution (R = 7500) grism of the 8m-Subaru FOCAS IFU instrument by the EMPRESS 3D survey, and investigate Hα emission of the EMPGs. Exploiting the resolution high enough for the low-mass galaxies, we derive gas dynamics with the Hα lines by the fitting of 3-dimensional disk models. We obtain an average maximum rotation velocity (vrot) of 15 ± 3 km s−1 and an average intrinsic velocity dispersion (σ0) of 27 ± 10 km s−1 for 15 spatially resolved EMPGs out of the 33 EMPGs, and find that all of the 15 EMPGs have vrot/σ0 rot/σ0 with the decreasing stellar mass and metallicity. We derive the gas mass fraction (fgas) for all of the 33 EMPGs, and find no clear dependence on stellar mass and metallicity. These vrot/σ0 and fgas trends should be compared with young high-z galaxies observed by the forthcoming JWST IFS programs to understand the physical origins of the EMPGs in the local universe. © 2023, CC BY.

关键词： Galaxies

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Abstracts from the 15th International Myopia Conference

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Eye and Vision 2016年第1期3卷 211-221页

作者： Alexandra Benavente-Perez Ann Nour Tobin Ansel Kathleen Abarr Luying Yan Keisha Roden David Troilo Chanyi Lu Miaozhen Pan Min Zheng Jia Qu Xiangtian Zhou Christine F. Wildsoet Fan Lu Jie Chen Jinhua Bao Liang Hu Qinmei Wang Zibing Jin Frances Rucker Stephanie Britton Stephan Hanowsky Molly Spatcher Hui-Ying Kuo Ching-Hsiu Ke I-Hsin Kuo Chien-Chun Peng Han-Yin Sun Ian G. Morgan Jeremy A. Guggenheim Rupal L. Shah Cathy Williams Jinglei Yang Peter S. Reinach Sen Zhang Wenfeng Sun Bo Liu Fen Li Xiaoqing Li Aihua Zhao Tianlu Chen Wei Jia Jun Jiang Haoran Wu Kazuo Tsubota Hiroko Ozawa Hidemasa Torii Shigemasa Takamizawa Toshihide Kurihara Kazuno Negishi Klaus Graef Daniel Rathbun Frank Schaeffel Ladan Ghodsi William K. Stell Machelle T. Pardue Ranjay Chakraborty Han na Park Curran S. Sidhu P. Michael Iuvone Michael J Collins Nethrajeith Srinvasalu Sally A. McFadden Paul N. Baird Pablo Artal Pauline Cho SW Cheung Pei-Chang Wu Quan V. Hoang Duk C. Lee Erica G. Landis Michael A. Bergen Curran Sidhu Samer Hattar Richard A. Stone Ravi Metlapally Ruiqin Li Qinglin Xu Hong Zhong Chenglin Pan Weizhong Lan Xiaoning Li Ling Chen Zhikuan Yang Scott A. Read Seang-Mei Saw Shi-Jun Weng Xiao-Hua Wu Kang-Wei Qian Yun-Yun Li Guo-Zhong Xu Furong Huang Xiong-Li Yang Yong-Mei Zhong Earl L Smith, III Baskar Arumugam Li-Fang Hung Lisa A. Ostrin Klaus Trier Monica Jong Brien A. Holden Thomas Chuen Lam Samantha Shan Bing Zuo Dennis Yan-yin Tse Jingfang Bian King-Kit Li Quan Liu Chi-ho To Timothy J. Gawne John T. Siegwart, Jr. Alexander H. Ward Thomas T. Norton Yan Zhang Yue Liu Carol Ho Eileen Phan Abraham Hang Emily Eng Christine Wildsoet Department of Biological Sciences SUNY College of Optometry New York NY 10036 USA School of Optometry and Ophthalmology and Eye Hospital Wenzhou Medical University Wenzhou Zhejiang 325027 China Center for Eye Disease & Development School of Optometry & Vision Science Program University of California Berkeley Berkeley CA 94720-2020 USA Wenzhou Medical University Wenzhou Zhejiang 325027 China Biomedical Science and Disease New England College of Optom Boston MA USA School of Optometry Chung Shan Medical University Taichung City 402 Taiwan Institute of Medicine Chung Shan Medical University Taichung City 402 Taiwan Division of Biochemistry and Molecular Biology Research School of Biology Australian National University Canberra Australia State Key Laboratory of Ophthalmology and Division of Preventive Ophthalmology Zhongshan Ophthalmic Center Sun Yat-Sen University Guangzhou China School of Optometry & Vision Sciences Cardiff University Cardiff UK School of Social and Community Medicine University of Bristol Bristol UK School of and Eye Hospital Wenzhou Medical University Wenzhou Zhejiang 325027 China State Key Laboratory Cultivation Base and Key Laboratory of Vision Science Ministry of Health and Zhejiang Provincial Key Laboratory of Ophthalmology and Optometry Wenzhou Zhejiang 325027 People’s Republic of China Shanghai Key Laboratory of Diabetes Mellitus and Center for Translational Medicine Shanghai Jiao Tong University Affiliated Sixth People’s Hospital Shanghai 200233 China Eye Hospital of Wenzhou Medical University Wenzhou Zhejiang 325027 China Department of Ophthalmology Keio University School of Medicine Shinjuku-ku Tokyo 160-8582 Japan General Medicine Ichikawa Medical Center Urayasu City Chiba 279-0001 Japan Ophthalmic Research Institute University of Tuebingen 72076 Tuebingen Germany Bernstein Center for Computational Neuroscience Tuebingen 72076 Tuebingen Germany Werner Reichardt Centre for Integrative Neuroscience Otfried-Mueller-Straße 25 Tueb

To assess the peripheral refractive changes that occur when eye growth decelerates in *** We measured peripheral refraction and on-axis vitreous chamber depth on a total of 53 marmosets;36 treated monocularly for 12 weeks 9 hrs/day(26 with-5 D contact lenses,10 with+5 D)and 17 untreated *** the 26 marmosets treated with-5 D,10 wore contact lenses 9 hrs/day without interruptions and were mea-sured at the end of 10 weeks of treatment(T10)and after 4 weeks of recovery(R14).Eight had both contact lenses removed for 30 mins twice/day(mid-morning and mid-afternoon)during the first four weeks of treatment(early interruption group)and eight had the lenses removed during the second four weeks of treatment(late interruption group).The two interruption groups were measured after 4,8 and 12 weeks of treatment only(T4,T8,T12).

关键词： removed treatment untreated

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EMPRESS. X. Spatially resolved mass-metallicity relation in extremely metal-poor galaxies: Evidence of episodic star-formation fueled by a metal-poor gas infall

arXiv

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arXiv 2024年

作者： Nakajima, Kimihiko Ouchi, Masami Isobe, Yuki Xu, Yi Ozaki, Shinobu Nagao, Tohru Inoue, Akio K. Rauch, Michael Kusakabe, Haruka Onodera, Masato Nishigaki, Moka Ono, Yoshiaki Sugahara, Yuma Hattori, Takashi Hirai, Yutaka Hashimoto, Takuya Kim, Ji Hoon Moriya, Takashi J. Yanagisawa, Hiroto Aoyama, Shohei Fujimoto, Seiji Fukushima, Hajime Fukushima, Keita Harikane, Yuichi Hatano, Shun Hayashi, Kohei Ishigaki, Tsuyoshi Kawasaki, Masahiro Kojima, Takashi Komiyama, Yutaka Koyama, Shuhei Koyama, Yusei Lee, Chien-Hsiu Matsumoto, Akinori Mawatari, Ken Motohara, Kentaro Murai, Kai Nagamine, Kentaro Nakane, Minami Saito, Tomoki Sasaki, Rin Shibuya, Takatoshi Suzuki, Akihiro Takeuchi, Tsutomu T. Umeda, Hiroya Umemura, Masayuki Watanabe, Kuria Yabe, Kiyoto Yajima, Hidenobu Zhang, Yechi National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan Osawa 2-21-1 Mitaka Tokyo181-8588 Japan University of Tokyo Chiba Kashiwa277-8583 Japan Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Cavendish Laboratory University of Cambridge 19 JJ Thomson Avenue CambridgeCB3 0HE United Kingdom Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Department of Physics Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan Research Center for Space and Cosmic Evolution Ehime University Bunkyo-cho 2-5 Ehime Matsuyama790-8577 Japan Department of Physics School of Advanced Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Observatoire de Genève Université de Genève 51 Chemin de Pégase Versoix1290 Switzerland 650 North Aohoku Place HiloHI96720 United States Department of Physics and Astronomy University of Notre Dame 225 Nieuwland Science Hall Notre DameIN46556 United States Astronomical Institute Tohoku University 6-3 Aoba Aramaki Aoba-ku Miyagi Sendai980-8578 Japan Division of Physics Faculty of Pure and Applied Sciences University of Tsukuba Ibaraki Tsukuba305-8571 Japan Faculty of Pure and Applied Sciences University of Tsukuba Ibaraki Tsukuba305-8571 Japan Astronomy Program Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Cent

Using the Subaru/FOCAS IFU capability, we examine the spatially resolved relationships between gas-phase metallicity, stellar mass, and star-formation rate surface densities (Σ★ and ΣSFR, respectively) in extremely metal-poor galaxies (EMPGs) in the local universe. Our analysis includes 24 EMPGs, comprising 9,177 spaxels, which span a unique parameter space of local metallicity (12 + log(O/H) 6.9 to 7.9) and stellar mass surface density (Σ★ ∼ 105 to 107 Mo kpc−2), extending beyond the range of existing large integral-field spectroscopic surveys. Through spatially resolved emission line diagnostics based on the [N ii] BPT-diagram, we verify the absence of evolved active galactic nuclei in these EMPGs. Our findings reveal that, while the resolved mass-metallicity relation exhibits significant scatter in the low-mass regime, this scatter is closely correlated with local star-formation surface density. Specifically, metallicity decreases as ΣSFR increases for a given Σ★. Notably, half of the EMPGs show a distinct metal-poor horizontal branch on the resolved mass-metallicity relation. This feature typically appears at the peak clump with the highest Σ★ and ΣSFR and is surrounded by a relatively metal-enriched ambient region. These findings support a scenario in which metal-poor gas infall fuels episodic star formation in EMPGs, consistent with the kinematic properties observed in these systems. In addition, we identify four EMPGs with exceptionally low central metallicities (12 + log(O/H) 7.2), which display only a metal-poor clump without a surrounding metal-rich region. This suggests that such ultra-low metallicity EMPGs, at less than a few percent of the solar metallicity, may serve as valuable analogs for galaxies in the early stages of galaxy evolution. Copyright © 2024, The Authors. All rights reserved.

关键词： Spectroscopic analysis

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The structure of the stellar halo of the Andromeda galaxy explored with the NB515 for Subaru/HSC. I.: New insights on the stellar halo up to 120 kpc

arXiv

引用

arXiv 2024年

作者： Ogami, Itsuki Tanaka, Mikito Komiyama, Yutaka Chiba, Masashi Guhathakurta, Puragra Kirby, Evan N. Wyse, Rosemary F.G. Filion, Carrie Gilbert, Karoline M. Escala, Ivanna Mori, Masao Kirihara, Takanobu Tanaka, Masayuki Ishigaki, Miho N. Hayashi, Kohei Lee, Myung Gyoon Sharma, Sanjib Kalirai, Jason S. Lupton, Robert H. 2-21-1 Osawa Mitaka Tokyo181-8588 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Advanced Sciences Faculty of Science and Engineering Hosei University 3-7-2 Kajino-cho Koganei Tokyo184-8584 Japan Astronomical Institute Tohoku University Aoba-ku Miyagi Sendai980-8578 Japan Department of Astronomy and Astrophysics University of California Santa Cruz University of California Observatories 1156 High Street Santa CruzCA95064 United States Department of Physics and Astronomy University of Notre Dame Notre DameIN46556 United States Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States John Hopkins Applied Physics Laboratory 11100 Johns Hopkins Road LaurelMD20723 United States Space Telescope Science Institute 3700 San Martin Dr. BaltimoreMD21218 United States The Observatories of the Carnegie Institution for Science 813 Santa Barbara Street PasadenaCA91101 United States Faculty of Pure and Applied Physics University of Tsukuba Tennodai 1-1-1 Ibaraki Tsukuba305-8577 Japan Center for Computational Sciences University of Tsukuba Tennodai 1-1-1 Ibaraki Tsukuba305-8577 Japan Kitami Institute of Technology 165 Koen-cho Hokkaido Kitami090-8507 Japan National Institute of Technology Sendai College Miyagi Natori981-1239 Japan Astronomy Program Department of Physics and Astronomy SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States

We analyse the M31 halo and its substructure within a projected radius of 120 kpc using a combination of Subaru/HSC NB515 and CFHT/MegaCam g- & i-bands. We succeed in separating M31’s halo stars from foreground contamination with ∼ 90 % accuracy by using the surface gravity sensitive NB515 filter. Based on the selected M31 halo stars, we discover three new substructures, which associate with the Giant Southern Stream (GSS) based on their photometric metallicity estimates. We also produce the distance and photometric metallicity estimates for the known substructures. While these quantities for the GSS are reproduced in our study, we find that the North-Western stream shows a steeper distance gradient than found in an earlier study, suggesting that it is likely to have formed in an orbit closer to the Milky Way. For two streams in the eastern halo (Stream C and D), we identify distance gradients that had not been resolved. Finally, we investigate the global halo photometric metallicity distribution and surface brightness profile using the NB515-selected halo stars. We find that the surface brightness of the metal-poor and metal-rich halo populations, and the all population can be fitted to a power-law profile with an index of α = −1.65 ± 0.02, −2.82 ± 0.01, and −2.44 ± 0.01, respectively. In contrast to the relative smoothness of the halo profile, its photometric metallicity distribution appears to be spatially non-uniform with nonmonotonic trends with radius, suggesting that the halo population had insufficient time to dynamically homogenize the accreted populations. Copyright © 2024, The Authors. All rights reserved.

关键词： Luminance

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