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arXiv 2021年

作者： Klein, Matthias Oguri, M. Mohr, J.J. Grandis, S. Ghirardini, V. Liu, T. Liu, A. Bulbul, E. Wolf, J. Comparat, J. Ramos-Ceja, M.E. Buchner, J. Chiu, I. Clerc, N. Merloni, A. Miyatake, H. Miyazaki, S. Okabe, N. Ota, N. Pacaud, F. Salvato, M. Driver, S.P. Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Research Center for the Early Universe University of Tokyo Tokyo113-0033 Japan Department of Physics University of Tokyo Tokyo113-0033 Japan University of Tokyo Chiba277-8582 Japan Max Planck Institute for Extraterrestrial Physics Giessenbachstrasse 1 Garching85748 Germany Tsung-Dao Lee Institute Key Laboratory for Particle Physics Astrophysics and Cosmology Ministry of Education Shanghai Jiao Tong University Shanghai200240 China Department of Astronomy School of Physics and Astronomy Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai Jiao Tong University Shanghai200240 China 11F of AS/NTU Astronomy-Mathematics Building No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan IRAP Université de Toulouse CNRS UPS CNES Toulouse France Nagoya University Nagoya464-8602 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Mitaka Tokyo181-8588 Japan Physics Program Graduate School of Advanced Science and Engineering Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Core Research for Energetic Universe Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Universität Bonn Auf dem Hügel 71 Bonn53121 Germany Department of Physics Nara Women’s University Kitauoyanishimachi Nara630-8506 Japan CRAR The University of Western Australia 7 Fairway CrawleyWA6009 Australia Exzellenzcluster ORIGINS Boltzmannstr. 2 GarchingD-85748 Germany

Context. In 2019, the eROSITA telescope on board of the Russian-German satellite Spectrum-Roentgen-Gamma (SRG), has started to perform a deep all-sky X-ray survey with the aim of identifying ∼ 100, 000 clusters and groups over the course of four years. As part of its performance verification phase a ∼ 140 deg2 survey called eROSITA Final Equatorial-Depth Survey (eFEDS) was performed. With a depth typical of the all-sky survey after four years, it allows tests of tools and methods as well as improved predictions for the all-sky survey. Aims. As part of this effort, a catalog of 542 X-ray extent selected galaxy group and cluster candidates was constructed. In this paper we present the optical follow-up with the aim of providing redshifts and cluster confirmation for the full sample. Further we aim to provide additional information on cluster dynamical state, cluster richness and cluster optical centre. Finally we aim to evaluate the impact of optical cluster confirmation on the purity and completeness of the X-ray selected sample. Methods. We use optical imaging data from the Hyper Suprime-Cam Subaru Strategic program and from the Legacy Survey to identify optical counterparts to the X-ray detected cluster candidates. We make use of the red sequence based cluster redshift and confirmation tool MCMF as well as the optical cluster finder CAMIRA to derive cluster redshifts and richnesses. MCMF provided probabilities of an optical structure being a chance super position with the X-ray candidate is used to identify the best optical counter part as well as to confirm an X-ray candidate as a cluster. The impact of this confirmation process on catalog purity and completeness is estimated using optical to X-ray scaling relations as well as simulations. The resulting catalog is further matched with public group and cluster catalogs. Optical estimators of cluster dynamical state are constructed based on density maps of the red sequence galaxies at the cluster redshift. Results.

关键词： Surveys

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The eROSITA Final Equatorial-Depth Survey (eFEDS): Catalog of galaxy clusters and groups

arXiv

引用

arXiv 2021年

作者： Liu, Ang Bulbul, E. Ghirardini, V. Liu, T. Klein, M. Clerc, N. Özsoy, Y. Ramos-Ceja, M.E. Pacaud, F. Comparat, J. Okabe, N. Bahar, Y.E. Biffi, V. Brunner, H. Brüggen, M. Buchner, J. Ider Chitham, J. Chiu, I. Dolag, K. Gatuzz, E. Gonzalez, J. Hoang, D.N. Lamer, G. Merloni, A. Nandra, K. Oguri, M. Ota, N. Predehl, P. Reiprich, T.H. Salvato, M. Schrabback, T. Sanders, J.S. Seppi, R. Thibaud, Q. Max Planck Institute for Extraterrestrial Physics Giessenbachstrasse 1 Garching85748 Germany Universitaets-Sternwarte Muenchen Fakultaet fuer Physik LMU Munich Scheinerstr. 1 Munich81679 Germany IRAP Université de Toulouse CNRS UPS CNES Toulouse France Universität Bonn Auf dem Hügel 71 Bonn53121 Germany Physics Program Graduate School of Advanced Science and Engineering Hiroshima University 1-3-1 Kagamiyama Hiroshima Higashi-Hiroshima739-8526 Japan Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Hiroshima Higashi-Hiroshima739-8526 Japan Core Research for Energetic Universe Hiroshima University 1-3-1 Kagamiyama Hiroshima Higashi-Hiroshima739-8526 Japan INAF - Osservatorio Astronomico di Trieste via Tiepolo 11 TriesteI-34143 Italy IFPU - Institute for Fundamental Physics of the Universe Via Beirut 2 TriesteI-34014 Italy University of Hamburg Hamburger Sternwarte Gojenbergsweg 112 Hamburg21029 Germany Tsung-Dao Lee Institute Key Laboratory for Particle Physics Astrophysics and Cosmology Ministry of Education Shanghai Jiao Tong University Shanghai200240 China Department of Astronomy School of Physics and Astronomy Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai Jiao Tong University Shanghai200240 China 11F of AS/NTU Astronomy-Mathematics Building No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan An der Sternwarte 16 Potsdam14482 Germany Research Center for the Early Universe The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Department of Physics The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan Department of Physics Nara Women's University Kitauoyanishimachi Nara630-8506 Japan

Aims. The eROSITA Final Equatorial-Depth Survey has been carried out during the performance verification phase of the Spectrum-Roentgen-Gamma/eROSITA telescope and was completed in November 2019. This survey is designed to provide the first eROSITA-selected sample of clusters and groups and to test the predictions for the all-sky survey in the context of cosmological studies with clusters of galaxies. Methods. In the area of ∼140 square degrees covered by eFEDS, 542 candidate clusters and groups of galaxies were detected as extended X-ray sources with the eSASS source detection algorithm. We performed imaging and spectral analysis of the 542 cluster candidates with eROSITA X-ray data and studied the properties of the sample. Results. We provide the catalog of candidate galaxy clusters and groups detected by eROSITA in the eFEDS field down to a flux of ∼ 10−14 erg s−1 cm−2 in the soft band (0.5-2 keV) within 10. The clusters are distributed in the redshift range z =[0.01, 1.3] with a median redshift zmedian = 0.35. With eROSITA X-ray data, we measured the temperature of the intracluster medium within two radii, 300 kpc and 500 kpc, and constrained the temperature with > 2σ confidence level for ∼ 1/5 (102 out of 542) of the sample. The average temperature of these clusters is ∼2 keV. Radial profiles of flux, luminosity, electron density, and gas mass were measured from the precise modeling of the imaging data. The selection function, the purity, and the completeness of the catalog are examined and discussed in detail. The contamination fraction is ∼ 1/5 in this sample and is dominated by misidentified point sources. The X-ray luminosity function of the clusters agrees well with the results obtained from other recent X-ray surveys. We also find 19 supercluster candidates in this field, most of which are located at redshifts between 0.1 and 0.5, including one cluster at z ∼ 0.36 that was presented previously. Conclusions. The eFEDS cluster and group catalog at the final

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A New Master Supernovae Ia sample and the investigation of the Hubble tension

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Journal of High Energy Astrophysics 2025年 48卷

作者： Dainotti, M.G. De Simone, B. Garg, A. Kohri, K. Bashyal, A. Aich, A. Mondal, A. Nagataki, S. Montani, G. Jareen, T. Jabir, V.M. Khanjani, S. Bogdan, M. Fraija, N. do E.S. Pedreira, A.C.C. Dejrah, R.H. Singh, A. Parakh, M. Mandal, R. Jarial, K. Lambiase, G. Sarkar, H. Division of Science National Astronomical Observatory of Japan 2 Chome-21-1 Osawa Tokyo Mitaka 181-8588 Japan The Graduate University for Advanced Studies SOKENDAI Shonankokusaimura Miura District Kanagawa Hayama 240-0115 Japan Space Science Institutes 4765 Walnut St Ste B Boulder 80301 CO United States Nevada Center for Astrophysics University of Nevada 89154 4505 Maryland Parkway Las Vegas 80301 NV United States Dipartimento di Fisica “E.R. Caianiello” Università di Salerno Via Giovanni Paolo II 132 Salerno Fisciano 84084 Italy INFN Gruppo Collegato di Salerno Sezione di Napoli. c/o Dipartimento di Fisica “E.R. Caianiello” Università di Salerno Via Giovanni Paolo II 132 Salerno Fisciano 84084 Italy Department of Astronomy Astrophysics and Space Engineering Indian Institute of Technology Madhya Pradesh Indore 403552 India Theory Center IPNS and QUP (WPI) KEK 1-1 Oho Tsukuba 305-0801 Japan Kavli IPMU (WPI) UTIAS The University of Tokyo Chiba Kashiwa 277-8583 Japan Central Department of Physics Tribhuvan University Kathmandu Kirtipur 44618 Nepal Pokhara Astronomical Society Pokhara 33700 Nepal Prayoga Institute of Education Research Kanakapura Rd off Ravgodlu Post Karnataka Bengaluru 560082 India Indian Institute of Science Education and Research Homi Bhabha Road Pashan Maharashtra Pune 411008 India Astrophysical Big Bang Laboratory (ABBL) RIKEN Cluster for Pioneering Research 2-1 Hirosawa Saitama Wako 351-0198 Japan RIKEN Interdisciplinary Theoretical & Mathematical Science Program (iTHEMS) 2-1 Hirosawa Saitama Wako 351-0198 Japan Astrophysical Big Bang Group (ABBG) Okinawa Institute of Science and Technology (OIST) 1919-1 Tancha Onna-son Okinawa Kunigami-gun 904-0495 Japan Physics Department “Sapienza” University of Rome P.le Aldo Moro 5 Rome 00185 Italy ENEA Fusion and Nuclear Safety Department C.R. Frascati Via E. Fermi 45 Frascati 00044 Italy The Thanu Padmanabhan Centre for Cosmology and Science Popul

Modern cosmological research still thoroughly debates the discrepancy between local probes and the Cosmic Microwave Background observations in the Hubble constant (H0) measurements, ranging from 4 to 6σ. In the current study, we examine this tension using the Supernovae Ia (SNe Ia) data from the Pantheon, Pantheon+ (P+), Joint Lightcurve Analysis (JLA), and Dark Energy Survey, (DES) catalogs combined together into the so-called Master Sample. The sample contains 3714 SNe Ia, and is divided all of them into redshift-ordered bins. Three binning techniques are presented: the equi-population, the moving window (MW), and the equi-spacing in the log⁡−z. We perform a Markov-Chain Monte Carlo analysis (MCMC) for each bin to determine the H0 value, estimating it within the standard flat ΛCDM and the w0waCDM models. These H0 values are then fitted with the following phenomenological function: H0(z)=H˜0/(1+z)^α, where H˜0 is a free parameter representing H0(z) fitted in z=0, and α is the evolutionary parameter. Our results indicate a decreasing trend characterized by α∼0.01, whose consistency with zero ranges from 1σ in 5 cases to 1 case at 3 σ and 11 cases at >3σ in several samples and configurations. Such a trend in the SNe Ia catalogs could be due to evolution with redshift for the astrophysical variables or unveiled selection biases. Alternatively, intrinsic physics, possibly the f(R) theory of gravity, could be responsible for this trend.

关键词： Cosmology Hubble constant Hubble tension SNe Ia

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On the Scarcity of Dense Cores (n>105 cm-3) in High latitude Planck Galactic Cold Clumps

arXiv

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arXiv 2024年

作者： Xu, Fengwei Wang, Ke Liu, Tie Eden, David Liu, Xunchuan Juvela, Mika He, Jinhua Johnstone, Doug Goldsmith, Paul Garay, Guido Wu, Yuefang Soam, Archana Traficante, Alessio Ristorcelli, Isabelle Falgarone, Edith Chen, Huei-Ru Vivien Hirano, Naomi Doi, Yasuo Kwon, Woojin White, Glenn J. Whitworth, Anthony Sanhueza, Patricio Rawlings, Mark G. Alina, Dana Ren, Zhiyuan Lee, Chang Won Tatematsu, Ken'ichi Zhang, Chuan-Peng Zhou, Jianjun Lai, Shih-Ping Ward-Thompson, Derek Liu, Sheng-Yuan Gu, Qilao Chakali, Eswaraiah Zhu, Lei Mardones, Diego Tóth, L. Viktor Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Armagh Observatory and Planetarium College Hill ArmaghBT61 9DG United Kingdom Department of Physics University of Helsinki PO Box 64 HelsinkiFI-00014 Finland Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile NRC Herzberg Astronomy and Astrophysics 5071 West Saanich Road VictoriaBCV9E 2E7 Canada Department of Physics and Astronomy University of Victoria 3800 Finnerty Road Elliot Building VictoriaBCV8P 5C2 Canada Jet Propulsion Laboratory California Institute of Technology PasadenaCA91109 United States Indian Institute of Astrophysics II Block Koramangala Bengaluru560034 India IAPS-INAF Via Fosso del Cavaliere 100 RomeI-00133 Italy Université de Toulouse UPS-OMP IRAP ToulouseF-31028 Cedex 4 France LPENS Ecole Normale Supérieure Université PSL CNRS Sorbonne Université Université de Paris Paris75005 France Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu30013 Taiwan Institute of Astronomy and Astrophysics Academia Sinica No.1 Sec. 4 Roosevelt Road Taipei10617 Taiwan Department of Earth Science and Astronomy Graduate School of Arts and Sciences The University of Tokyo 3-8-1 Komaba Tokyo Meguro153-8902 Japan 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 School of Physical Sciences The Open Un

High-latitude (|b| > 30◦) molecular clouds have virial parameters that exceed 1, but whether these clouds can form stars has not been studied systematically. Using JCMT SCUBA-2 archival data, we surveyed 70 fields that target high-latitude Planck Galactic cold clumps (HLPCs) to find dense cores with density of 105–106 cm-3 and size of 1 × 1021 cm-2). At an average rms of 15 mJy beam-1, we detected Galactic dense cores in only one field, G6.04+36.77 (L183) while also identifying 12 extragalactic objects and two young stellar objects. Compared to the low-latitude clumps, dense cores are scarce in HLPCs. With synthetic observations, the densities of cores are constrained to be nc 105 cm-3 should they exist in HLPCs. Low-latitude clumps, Taurus clumps, and HLPCs form a sequence where a higher virial parameter corresponds to a lower dense-core detection rate. If HLPCs were affected by the Local Bubble, the scarcity should favor turbulence-inhibited rather than supernova-driven star formation. Studies of the formation mechanism of the L183 molecular cloud are warranted. © 2024, CC BY.

关键词： Supernovae

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On the Scarcity of Dense Cores (n > 10⁵cm^-3) in High-latitude Planck Galactic Cold Clumps

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Astrophysical Journal Letters 2024年第1期963卷 L9-L9页

作者： Xu, Fengwei Wang, Ke Liu, Tie Eden, David Liu, Xunchuan Juvela, Mika He, Jinhua Johnstone, Doug Goldsmith, Paul Garay, Guido Wu, Yuefang Soam, Archana Traficante, Alessio Ristorcelli, Isabelle Falgarone, Edith Chen, Huei-Ru Vivien Hirano, Naomi Doi, Yasuo Kwon, Woojin White, Glenn J. Whitworth, Anthony Sanhueza, Patricio Rawlings, Mark G. Alina, Dana Ren, Zhiyuan Lee, Chang Won Tatematsu, Ken'ichi Zhang, Chuan-Peng Zhou, Jianjun Lai, Shih-Ping Ward-Thompson, Derek Liu, Sheng-Yuan Gu, Qilao Chakali, Eswaraiah Zhu, Lei Mardones, Diego Tóth, L. Viktor Kavli Institute for Astronomy and Astrophysics Peking University Beijing 100871 China Department of Astronomy School of Physics Peking University Beijing 100871 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai 200030 China Armagh Observatory and Planetarium College Hill Armagh BT61 9DB United Kingdom Department of Physics University of Helsinki P.O. Box 64 Helsinki FI-00014 Finland Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing 100101 China Departamento de Astronomía Universidad de Chile Las Condes Santiago 7591245 Chile NRC Herzberg Astronomy and Astrophysics 5071 West Saanich Road Victoria V9E 2E7 BC Canada Department of Physics and Astronomy University of Victoria 3800 Finnerty Road Elliot Building Victoria V8P 5C2 BC Canada Jet Propulsion Laboratory California Institute of Technology Pasadena 91109 CA United States Indian Institute of Astrophysics II Block Koramangala Bengaluru 560034 India IAPS-INAF Via Fosso del Cavaliere 100 Rome I-00133 Italy IRAP Université de Toulouse CNRS UPS 9 Av. du Colonel Roche BP 44346 Toulouse cedex 4 31028 France LPENS Ecole Normale Supérieure Université PSL CNRS Sorbonne Université Université de Paris Paris 75005 France Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu 30013 Taiwan Institute of Astronomy and Astrophysics Academia Sinica No.1 Sec. 4 Roosevelt Road Taipei 10617 Taiwan Department of Earth Science and Astronomy Graduate School of Arts and Sciences The University of Tokyo 3-8-1 Komaba Meguro Tokyo 153-8902 Japan Department of Earth Science Education Seoul National University 1 Gwanak-ro Gwanak-gu Seoul 08826 South Korea SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul 08826 South Ko

High-latitude (\b\ > 30°) molecular clouds have virial parameters that exceed 1, but whether these clouds can form stars has not been studied systematically. Using JCMT SCUBA-2 archival data, we surveyed 70 fields that target high-latitude Planck Galactic cold clumps (HLPCs) to find dense cores with density of 10⁵-10⁶ cm-³ and size of <0.1 pc. The sample benefits from both the representativeness of the parent sample and its coverage of the densest clumps at the high column density end (>1 × 10²¹ cm^-2). At an average rms of 15mJybeam^-1, we detected Galactic dense cores in only one field, G6.04+36.77 (L183) while also identifying 12 extragalactic objects and two young stellar objects. Compared to the low-latitude clumps, dense cores are scarce in HLPCs. With synthetic observations, the densities of cores are constrained to be n_c ≲ 10⁵ cm^-3 should they exist in HLPCs. Low-latitude clumps, Taurus clumps, and HLPCs form a sequence where a higher virial parameter corresponds to a lower dense-core detection rate. If HLPCs were affected by the Local Bubble, the scarcity should favor turbulence-inhibited rather than supernova-driven star formation. Studies of the formation mechanism of the L183 molecular cloud are warranted. © 2024. The Author(s). Published by the American Astronomical Society.

关键词： High latitude field (737) Molecular clouds (1072) Supporting material: figure set, machine-readable table Unified Astronomy Thesaurus concepts: Star formation (1569)

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Erratum: “Two-dimensional porous graphitic carbon nitride C6N7 monolayer: First-principles calculations” [Appl. Phys. Lett. 119, 142102 (2021)]

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Applied Physics Letters 2022年第18期120卷

作者： A. Bafekry M. Faraji M. M. Fadlallah I. Abdolhosseini Sarsari H. R. Jappor S. Fazeli M. Ghergherehchi 1Department of Radiation Application Shahid Beheshti University Tehran Iran 2Micro and Nanotechnology Graduate Program TOBB University of Economics and Technology Sogutozu Caddesi No 43 Sogutozu 06560 Ankara Turkey 3Department of Physics Faculty of Science Benha University 13518 Benha Egypt 4Department of Physics Isfahan University of Technology Isfahan 84156-83111 Iran 5Department of Physics College of Education for Pure Sciences University of Babylon Hilla Iraq 6Department of Material Science and Engineering Sharif University of Technology PO Box 11155-9466 Tehran Iran 7Department of Electrical and Computer Engineering Sungkyunkwan University 16419 Suwon South Korea

The original article1 contains misprints in the values of the elastic parameters. The values of C11 = 258.6 GPa, C22 = 290.8 GPa, and C12 = 70.73 GPa and C13 =

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Examination of Cs tolerant bacteria interaction with Cs+ in aqueous solution and soil by using 137Cs tracer

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AIP Conference Proceedings 2020年第1期2295卷

作者： Triyono Basuki Kuninobu Inada Satoru Nakashima 1Radioactivity Environmental Protection Course Phoenix leader Education Program Hiroshima University 1-1-1 Kagamiyama Higashi-Hiroshima 739-8524 Japan 2Department of Chemistry Graduate School of Science Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima 739-8526 Japan 3Natural Science Center for Basic Research and Development Hiroshima University 1-4-2 Kagamiyama Higashi-Hiroshima 739-8526 Japan

The interaction of microorganisms with Cs in aqueous solution and soil is a key for Cs bioremediation as an alternative of physical and chemical remediation and for understanding the Cs mobility in the environment. In the present study, we isolated cesium tolerant bacteria (CsT-tb) strain having very high tolerance level toward Cs, although it has relatively low Cs sorption capacity from the solution. The effect of CsT-tb strain for bioremediation was analyzed by adding CsT-tb strain solution to the broth containing Cs adsorbed soil, revealing the comparable Cs removal with H2S04 treatment. The Cs desorption enhancement from the silt and clay soil fraction by CsT-tb strain showed its potential for Cs bioremediation and important information of Cs migration promoted by microorganism. From the phylogenetic tree of the 16S rDNA, the CsT-tb strain was closely related to Bacillus sp.

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Amplification and cloning of arabidopsis 6xhis-tagged mpk6 fusion encoded gene to characterize biochemical mitogen-activated protein kinase in disease resistance role against Fusarium graminearum

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IOP Conference Series: Earth and Environmental science 2020年第1期575卷

作者： M H Rahmah T Nishiuchi Study Program of Biology Education Faculty of Teacher Training and Education Universitas Sulawesi Barat Majene Sulawesi Barat Indonesia Division of Functional Genomics Advanced Science Research Center Kanazawa University 13-1 Takaramachi Kanazawa 920-0934 Japan Division of Functional Genomics Advanced Science Research Center Kanazawa University 13-1 Takaramachi Kanazawa 920-0934 Japan Division of Life Science Graduate School of Natural Science and Technology Kanazawa University Kanazawa 920-1192 Japan

The Mitogen-Activated Protein Kinase (MPK) cascade plays an important role in the intracellular signaling transduction pathway leading to resistance against phytopathogens produced by Fusarium graminearum. In the cascade, there are three prominent kinase protein groups involved, an MPK kinase kinase (MPKKK), MPK kinase (MPKK), and an MPK. Recognitions of pathogen-derived molecules in plants trigger rapid activation of some MPKs including MPK6 which are found in a wide variety of plant species, including in Arabidopsis thaliana. The structure of MPK6 contains kinase domain and common docking (CD) domain. CD domain is phosphorylated by interact with MPKK. Moreover, the MPKK which binds to MPK6 and its phosphorylation mechanism are still unknown, so as initial study is needed to investigate biochemical characterization by prepare MPK6 protein. In this research, mpk 6 was amplified by using a pair primer and subsequently was ligated into pET160/GW/D-TOPO vector which contained with sequence encoded 6xHistidine tag protein for protein purification assay.

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Control of microswimmers by spiral nematic vortices: transition from individual to collective motion and contraction, expansion, and stable circulation of bacterial swirls

arXiv

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arXiv 2020年

作者： Koizumi, Runa Turiv, Taras Genkin, Mikhail M. Lastowski, Robert J. Yu, Hao Chaganava, Irakli Wei, Qi-Huo Aranson, Igor S. Lavrentovich, Oleg D. Advanced Materials and Liquid Crystal Institute Materials Science Graduate Program Kent State University KentOH44242 United States Cold Spring Harbor Laboratory 1 Bungtown Rd Cold Spring HarborNY11724 United States Department of Chemistry University of Scranton ScrantonPA18510 United States Institute of Cybernetics of Georgian Technical University TbilisiGA0186 United States Georgian State Teaching University of Physical Education and Sport TbilisiGA0162 United States Department of Physics Kent State University KentOH44242 United States Department of Biomedical Engineering Pennsylvania State University University ParkPA16802 United States

Active systems comprised of self-propelled units show fascinating transitions from Brownian-like dynamics to collective coherent motion. Swirling of swimming bacteria is a spectacular example. This study demonstrates that a nematic liquid crystal environment patterned as a spiral vortex controls individual-to-collective transition in bacterial swirls and defines whether they expand or shrink. In dilute dispersions, the bacteria swim along open spiral trajectories, following the pre-imposed molecular orientation. The trajectories are nonpolar. As their concentration exceeds some threshold, the bacteria condense into unipolar circular swirls resembling stable limit cycles. This collective circular motion is controlled by the spiral angle that defines the splay-to-bend ratio of the background director. Vortices with dominating splay shrink the swirls towards the center, while vortices with dominating bend expand them to the periphery. 45o spiraling vortices with splay-bend parity produce the most stable swirls. All the dynamic scenarios are explained by hydrodynamic interactions of bacteria mediated by the patterned passive nematic environment and by the coupling between the concentration and orientation. The acquired knowledge of how to control individual and collective motion of microswimmers by a nematic environment can help in the development of microscopic mechanical systems. Copyright © 2020, The Authors. All rights reserved.

关键词： Vortex flow

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The evolution of merger fraction of galaxies at z < 0.6 depending on the star formation mode in the AKARI NEP–Wide field

arXiv

引用

arXiv 2021年

作者： Kim, Eunbin Hwang, Ho Seong Jeong, Woong-Seob Kim, Seong Jin Burgarella, Denis Goto, Tomotsugu Hashimoto, Tetsuya Jo, Young-Soo Lee, Jong Chul Malkan, Matthew Pearson, Chris Shim, Hyunjin Toba, Yoshiki Ho, Simon C.-C. Santos, Daryl Joe Ikeda, Hiroyuki Kim, Helen K. Miyaji, Takamitsu Matsuhara, Hideo Oi, Nagisa Takagi, Toshinobu Wang, Ting-Wen Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of 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 Institute of Astronomy National Tsing Hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Aix Marseille Université CNRS Laboratoire d’Astrophysique de Marselle UMR 7326 Marseille13388 France National Tsing Hua University 101 Section 2. Kuang-Fu Road Hsinchu30013 Taiwan Department of Earth Science Education Kyungpook National University 80 Daehakro Bukgu Daegu41566 Korea Republic of Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan Academia Sinica Institute of Astronomy and Astrophysics 11F of Astronomy-Mathematics Building AS/NTU No.1 Section 4 Roosevelt Road Taipei10617 Taiwan Research Center for Space and Cosmic Evolution Ehime University 2-5 Bunkyo-cho MatsuyamaEhime790-8577 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan National Institute of Technology Wakayama College Gobo Wakayama644-0023 Japan Department of Physics and Astronomy UCLA 475 Portola Plaza Los AngelesCA90095-1547 United States Km 107 Carret. Tij.-Ens. EnsenadaBC22060 Mexico Leibniz Institut für Astrophysik Potsdam An der Sternwarte 16 Potsdam14482 Germany Department of Space and Astronautical Science Graduate University for Advanced Studies SOKENDAI 3-1-1 Yoshinodai Chuo-ku Sagamihara Kanagawa252-5210 Japan Institute of Space and Astronautical Science Japan Aerospace Exploration Agency 3-1-1 Yoshinodai Chuo-ku Sagamihara Kanagawa252-5210 Japan Tokyo University of Science 1-3 Kagurazaka Shinjuku-ku Tokyo162-8601 Japan RAL Space STFC Rutherford Appleton Laboratory Didcot OxfordshireOX11 0QX U

We study the galaxy merger fraction and its dependence on star formation mode in the 5.4 square degrees of the North Ecliptic Pole-Wide field. We select 6352 galaxies with AKARI 9 µm detections, and identify mergers among them using the Gini coefficient and M20 derived from the Subaru/HSC optical images. We obtain the total infrared luminosity and star formation rate of galaxies using the spectral energy distribution templates based on one band, AKARI 9 µm. We classify galaxies into three different star formation modes (i.e. starbursts, main sequence, and quiescent galaxies) and calculate the merger fractions for each. We find that the merger fractions of galaxies increase with redshift at z © 2021, CC BY.

关键词： Galaxies

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