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First Measurement of Antideuteron Number Fluctuations at Energies Available at the Large Hadron Collider

physical Review Letters 2023年第4期131卷 041901-041901页

作者： S. Acharya D. Adamová A. Adler G. Aglieri Rinella M. Agnello N. Agrawal Z. Ahammed S. Ahmad S. U. Ahn I. Ahuja A. Akindinov M. Al-Turany D. Aleksandrov B. Alessandro H. M. Alfanda R. Alfaro Molina B. Ali Y. Ali A. Alici N. Alizadehvandchali A. Alkin J. Alme G. Alocco T. Alt I. Altsybeev M. N. Anaam C. Andrei A. Andronic V. Anguelov F. Antinori P. Antonioli C. Anuj N. Apadula L. Aphecetche H. Appelshäuser S. Arcelli R. Arnaldi I. C. Arsene M. Arslandok A. Augustinus R. Averbeck S. Aziz M. D. Azmi A. Badalà Y. W. Baek X. Bai R. Bailhache Y. Bailung R. Bala A. Balbino A. Baldisseri B. Balis D. Banerjee Z. Banoo R. Barbera L. Barioglio M. Barlou G. G. Barnaföldi L. S. Barnby V. Barret L. Barreto C. Bartels K. Barth E. Bartsch F. Baruffaldi N. Bastid S. Basu G. Batigne D. Battistini B. Batyunya D. Bauri J. L. Bazo Alba I. G. Bearden C. Beattie P. Becht D. Behera I. Belikov A. D. C. Bell Hechavarria R. Bellwied S. Belokurova V. Belyaev G. Bencedi S. Beole A. Bercuci Y. Berdnikov A. Berdnikova L. Bergmann M. G. Besoiu L. Betev P. P. Bhaduri A. Bhasin I. R. Bhat M. A. Bhat B. Bhattacharjee L. Bianchi N. Bianchi J. Bielčík J. Bielčíková J. Biernat A. Bilandzic G. Biro S. Biswas J. T. Blair D. Blau M. B. Blidaru N. Bluhme C. Blume G. Boca F. Bock T. Bodova A. Bogdanov S. Boi J. Bok L. Boldizsár A. Bolozdynya M. Bombara P. M. Bond G. Bonomi H. Borel A. Borissov H. Bossi E. Botta L. Bratrud P. Braun-Munzinger M. Bregant M. Broz G. E. Bruno M. D. Buckland D. Budnikov H. Buesching S. Bufalino O. Bugnon P. Buhler Z. Buthelezi J. B. Butt A. Bylinkin S. A. Bysiak M. Cai H. Caines A. Caliva E. Calvo Villar J. M. M. Camacho R. S. Camacho P. Camerini F. D. M. Canedo M. Carabas F. Carnesecchi R. Caron J. Castillo Castellanos F. Catalano C. Ceballos Sanchez I. Chakaberia P. Chakraborty S. Chandra S. Chapeland M. Chartier S. Chattopadhyay T. G. Chavez T. Cheng C. Cheshkov B. Cheynis V. Chibante Barroso D. D. Chinellato E. S. Chizzali S. Cho P. Chochula P. Christakoglou C. H. Christensen P. Christiansen T. Chujo M. Ciacco C. Cicalo L. C Université Clermont Auvergne CNRS/IN2P3 LPC Clermont-Ferrand France Variable Energy Cyclotron Centre Homi Bhabha National Institute Kolkata India Nuclear Physics Institute of the Czech Academy of Sciences Husinec-Řež Czech Republic Johann-Wolfgang-Goethe Universität Frankfurt Institut für Informatik Fachbereich Informatik und Mathematik Frankfurt Germany European Organization for Nuclear Research (CERN) Geneva Switzerland Dipartimento DISAT del Politecnico and Sezione INFN Turin Italy INFN Sezione di Bologna Bologna Italy Department of Physics Aligarh Muslim University Aligarh India Korea Institute of Science and Technology Information Daejeon Republic of Korea Faculty of Science P.J. Šafárik University Košice Slovak Republic Affiliated with an institute covered by a cooperation agreement with CERN Research Division and ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH Darmstadt Germany INFN Sezione di Torino Turin Italy Central China Normal University Wuhan China Instituto de Física Universidad Nacional Autónoma de México Mexico City Mexico COMSATS University Islamabad Islamabad Pakistan Dipartimento di Fisica e Astronomia dell’Università and Sezione INFN Bologna Italy University of Houston Houston Texas USA Department of Physics and Technology University of Bergen Bergen Norway INFN Sezione di Cagliari Cagliari Italy Institut für Kernphysik Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany Horia Hulubei National Institute of Physics and Nuclear Engineering Bucharest Romania Westfälische Wilhelms-Universität Münster Institut für Kernphysik Münster Germany Physikalisches Institut Ruprecht-Karls-Universität Heidelberg Heidelberg Germany INFN Sezione di Padova Padova Italy Lawrence Berkeley National Laboratory Berkeley California USA SUBATECH IMT Atlantique Nantes Université CNRS-IN2P3 Nantes France Department of Physics University of Oslo Oslo Norway Yale University New Haven Connecticut USA L

The first measurement of event-by-event antideuteron number fluctuations in high energy heavy-ion collisions is presented. The measurements are carried out at midrapidity (|η|<0.8) as a function of collision centrality in Pb-Pb collisions at sNN=5.02 TeV using the ALICE detector. A significant negative correlation between the produced antiprotons and antideuterons is observed in all collision centralities. The results are compared with a state-of-the-art coalescence calculation. While it describes the ratio of higher order cumulants of the antideuteron multiplicity distribution, it fails to describe quantitatively the magnitude of the correlation between antiproton and antideuteron production. On the other hand, thermal-statistical model calculations describe all the measured observables within uncertainties only for correlation volumes that are different with respect to those describing proton yields and a similar measurement of net-proton number fluctuations.

关键词： Hadron-hadron interactions

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Chemical complexity of phosphorous bearing species in various regions of the interstellar medium

arXiv

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arXiv 2021年

作者： Sil, Milan Srivastav, Satyam Bhat, Bratati Mondal, Suman Kumar Gorai, Prasanta Ghosh, Rana Shimonishi, Takashi Chakrabarti, Sandip K. Sivaraman, Bhalamurugan Pathak, Amit Nakatani, Naoki Furuya, Kenji Das, Ankan Indian Centre for Space Physics 43 Chalantika Garia Station Road Kolkata700084 India Department of Physics Institute of Science Banaras Hindu University Varanasi221005 India Department of Space Earth & Environment Chalmers University of Technology GothenburgSE-412 96 Sweden Center for Transdisciplinary Research Niigata University Nishi-ku Niigata950-2181 Japan Environmental Science Program Department of Science Faculty of Science Niigata University Nishi-ku Niigata950-2181 Japan Physical Research Laboratory Navrangpura Ahmedabad380009 India Institute for Catalysis Hokkaido University N21W10 Kita-ku Sapporo Hokkaido001-0021 Japan Department of Chemistry Graduate School of Science and Engineering Tokyo Metropolitan University 1-1 Minami-Osawa Hachioji Tokyo192-0397 Japan Center for Computational Sciences University of Tsukuba Tsukuba305-8577 Japan National Astronomical Observatory of Japan Tokyo181-8588 Japan

Phosphorus related species are not known to be as omnipresent in space as hydrogen, carbon, nitrogen, oxygen, and sulfur-bearing species. Astronomers spotted very few P-bearing molecules in the interstellar medium and circumstellar envelopes. Limited discovery of the P-bearing species imposes severe constraints in modeling the P-chemistry. In this paper, we carry out extensive chemical models to follow the fate of P-bearing species in diffuse clouds, photon-dominated or photodissociation regions (PDRs), and hot cores/corinos. We notice a curious correlation between the abundances of PO and PN and atomic nitrogen. Since N atoms are comparatively abundant in diffuse clouds and PDRs than in the hot core/corino region, PO/PN reflects 1 in the late warm-up evolutionary phase of the hot core/corino regions. During the end of the post-warm-up phase, we obtain PO/PN > 1 for hot core and 3along with various impurities. We notice that SO2overlaps with the PH3bending-scissoring modes around ∼ (1000 - 1100) cm-1. We also find that the presence of CO2can strongly influence the intensity of the stretching modes around ∼ 2400 cm-1of PH3 © 2021, CC0.

关键词： Radiative transfer

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ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions − XVII. High-mass star-formation through a large-scale collapse in IRAS 15394−5358

arXiv

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arXiv 2024年

作者： Das, Swagat R. Merello, Manuel Bronfman, Leonardo Liu, Tie Garay, Guido Stutz, Amelia Mardones, Diego Zhou, Jian-Wen Sanhueza, Patricio Liu, Hong-Li Vázquez-Semadeni, Enrique Gómez, Gilberto C. Palau, Aina Tej, Anandmayee Xu, Feng-Wei Baug, Tapas Dewangan, Lokesh K. He, Jinhua Zhu, Lei Li, Shanghuo Juvela, Mika Saha, Anindya Issac, Namitha Hwang, Jihye Nazeer, Hafiz Toth, L. Viktor Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Departamento de Astronomía Universidad de Concepción Av. Esteban Iturra s/n Distrito Universitario 160-C Chile Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany 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 School of Physics and Astronomy Yunnan University Kunming650091 China Instituto de Radioastronomía y Astrofísica Universidad Nacional Autónoma de México Apdo. Postal 3-72 Michoacán Morelia58089 Mexico Indian Institute of Space Science and Technology Kerala Thiruvananthapuram695 547 India Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China S. N. Bose National Centre for Basic Sciences Block-JD Sector-III Salt Lake City Kolkata700106 India Physical Research Laboratory Navrangpura Ahmedabad380 009 India Yunnan Observatories Chinese Academy of Sciences 396 Yang-fangwang Guandu District Kunming650216 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Max Planck Institute of Astronoy Königstuhl 17 Heidelberg69117 Germany SOFIA Science Centre USRA NASA Ames Research Centre MS-12 N232 Moffett FieldCA94035 United States Department of Physics University of Helsinki PO Box 64 HelsinkiFI-00014 Finland Korea Astronomy and Space Science Institute 776 Daedeokdaero Yuseong-gu Daejeon34055 Korea Republic of Institute of Physics and Astronomy Eotvos Lorand University Pazmany Peter setany 1/A BudapestH-1117 Hungary

Hub-filament systems are considered as natural sites for high-mass star formation. Kinematic analysis of the surroundings of hub-filaments is essential to better understand high-mass star formation within such systems. In this work, we present a detailed study of the massive Galactic protocluster IRAS 15394−5358, using continuum and molecular line data from the ALMA Three-millimeter Observations of Massive Star-forming Regions (ATOMS) survey. The 3 mm dust continuum map reveals the fragmentation of the massive (M = 843 M☉) clump into six cores. The core C-1A is the largest (radius = 0.04 pc), the most massive (M = 157 M☉), and lies within the dense central region, along with two smaller cores (M = 7 and 3 M☉). The fragmentation process is consistent with the thermal Jeans fragmentation mechanism and virial analysis shows that all the cores have small virial parameter values (αvir 13CO+ shows that the massive clump is associated with a hub-filament system, where the central hub is linked with four filaments. A sharp velocity gradient is observed towards the hub, suggesting a global collapse where the filaments are actively feeding the hub. We discuss the role of global collapse and the possible driving mechanisms for the massive star formation activity in the protocluster. Copyright © 2024, The Authors. All rights reserved.

关键词： Kinematics

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The ALMA-QUARKS survey: – I. Survey description and data reduction

arXiv

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arXiv 2023年

作者： Liu, Xunchuan Liu, Tie Zhu, Lei Garay, Guido Liu, Hong-Li Goldsmith, Paul Evans, Neal Kim, Kee-Tae Liu, Sheng-Yuan Xu, Fengwei Lu, Xing Tej, Anandmayee Mai, Xiaofeng Bronfman, Leonardo Li, Shanghuo Mardones, Diego Stutz, Amelia Tatematsu, Kenichi Wang, Ke Zhang, Qizhou Qin, Sheng-Li Zhou, Jianwen Luo, Qiuyi Zhang, Siju Cheng, Yu He, Jinhua Gu, Qilao Li, Ziyang Zhang, Zhenying Zhang, Suinan Saha, Anindya Dewangan, Lokesh Sanhueza, Patricio Shen, Zhiqiang Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile School of Physics and Astronomy Yunnan University Kunming650091 China Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Department of Astronomy The University of Texas AustinTX78712-1205 United States Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Institute of Astronomy and Astrophysics Academia Sinica Roosevelt Road Taipei10617 Taiwan Kavli Institute for Astronomy and Astrophysics Peking University Haidian District Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Indian Institute of Space Science and Technology Kerala Thiruvananthapuram695 547 India Max Planck Institute for Astronomy Königstuhl 17 HeidelbergD-69117 Germany Departamento de Astronomía Universidad de Concepción Casilla 160-C Concepción Chile Nobeyama Radio Observatory National Astronomical Observatory of Japan National Institutes of Natural Sciences 462-2 Nobeyama Minamimaki Minamisaku Nagano384-1305 Japan Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53125 Germany School of Astronomy and Space Sciences University of Chinese Academy of Sciences Beijing100049 China National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Yunnan Observatories Chinese Academy of Sciences Yunnan Kunming650216 China Physical Research Laboratory Navrangpura Ahmedabad380 009 India GUAS Astronomical Science Program SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan

This paper presents an overview of the QUARKS survey, which stands for ‘Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures’. The QUARKS survey is observing 139 massive clumps covered by 156 pointings at ALMA Band 6 (λ ∼ 1.3 mm). In conjunction with data obtained from the ALMA-ATOMS survey at Band 3 (λ ∼ 3 mm), QUARKS aims to carry out an unbiased statistical investigation of massive star formation process within protoclusters down to a scale of 1000 au. This overview paper describes the observations and data reduction of the QUARKS survey, and gives a first look at an exemplar source, the mini-starburst Sgr B2(M). The wide-bandwidth (7.5 GHz) and high-angular-resolution (∼ 0.3′′) observations of the QUARKS survey allow to resolve much more compact cores than could be done by the ATOMS survey, and to detect previously unrevealed fainter filamentary structures. The spectral windows cover transitions of species including CO, SO, N2D+, SiO, H30α, H2CO, CH3CN and many other complex organic molecules, tracing gas components with different temperatures and spatial extents. QUARKS aims to deepen our understanding of several scientific topics of massive star formation, such as the mass transport within protoclusters by (hub-)filamentary structures, the existence of massive starless cores, the physical and chemical properties of dense cores within protoclusters, and the feedback from already formed high-mass young protostars. Copyright © 2023, The Authors. All rights reserved.

关键词： Data reduction

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Quantum tetrachotomous states: Superposition of four coherent states on a line in phase space

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physical Review A 2019年第6期99卷 063813-063813页

作者： Namrata Shukla Naeem Akhtar Barry C. Sanders Institute for Quantum Science and Technology University of Calgary Calgary Alberta Canada T2N 1N4 Shanghai Branch National Research Center for Physical Sciences at Microscale University of Science and Technology of China Shanghai 201315 China Program in Quantum Information Science Canadian Institute for Advanced Research Toronto Ontario Canada M5G 1M1

The well-studied quantum optical Schrödinger cat state is a superposition of two distinguishable states, with quantum coherence between these macroscopically distinguishable states being of foundational and, in the context of quantum-information processing, practical use. We refer to these quantum-optical cat states as quantum dichotomous states, reflecting that the state is a superposition of two options, and we introduce the term quantum multichotomous state to refer to a superposition of multiple macroscopically distinguishable options. For a single degree of freedom, such as position, we construct the quantum multichotomous states as a superposition of Gaussian states on the position line in phase space. Using this nomenclature, a quantum tetrachotomous state (QTS) is a coherent superposition of four macroscopically distinguishable states. We define, analyze, and show how to create such states, and our focus on the QTSs is due to their exhibition of much richer phenomena than for the quantum dichotomous states. Our characterization of the QTS involves the Wigner function, its marginal distributions, and the photon-number distribution, and we discuss the QTS's approximate realization in a multiple-coupled-well system.

关键词： Quantum coherence & coherence measures Quantum foundations Quantum information processing with continuous variables Quantum simulation

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Comparison of Functional Capability,Flexibility,Strength and Quality of Life in Aged Women Engaged in Resistance Exercise,Weight-Bearing Training or Hydro-Gymnastics

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Journal of Sports science 2019年第4期7卷 106-114页

作者： Otávio Augusto Soares Machado Waldecir Paula Lima Bruna Vieira de Souza Fábio Gianolla Luiz Francisco Killian Giovanna Athanásio Chaves Machado Renata Gorjao Physiology and Metabolism Research Center YMCA Physical Education FacultySorocaba-SPBrazil Federal Institute of Education Science and TechnologySao Paulo-SPBrazil Postgraduate Program in Interdisciplinary Health Science Cruzeiro do Sul UniversitySao Paulo-SPBrazil

Although any type or amount of physical exercise may reverse the cellular processes that lead to the aging,regular physical exercise can attenuate the decline in physical and functional abilities observed in ***,the most encouraged activities in gyms and clubs are resistance training,functional training,and *** main objective of this study was to compare the effects of the aforementioned exercises regarding muscle strength,flexibility,functional capability and quality of life of elderly *** divided 36 elderly women in four groups:Sedentary(S);Hydro-gymnastics(H);Functional Training(F);or Resistance Training(RT).The results reveal that the groups engaged in physical exercise showed a significant difference(p<0.05)in relation to S in all *** results also show that between the different exercises evaluated,resistance training practitioners have greater strength and better functional capability.

关键词： Aged exercise physical fitness quality of life

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SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). V. Confusion-limited Submillimeter Galaxy Number Counts at 450 µm and Data Release for the COSMOS Field

arXiv

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arXiv 2024年

作者： Gao, Zhen-Kai Lim, Chen-Fatt Wang, Wei-Hao Chen, Chian-Chou Smail, Ian Chapman, Scott C. Zheng, Xian Zhong Shim, Hyunjin Kodama, Tadayuki Ao, Yiping Chang, Siou-Yu Clements, David L. Dunlop, James S. Ho, Luis C. Hsu, Yun-Hsin Hwang, Chorng-Yuan Hwang, Ho Seong Koprowski, M.P. Scott, Douglas Serjeant, Stephen Toba, Yoshiki Urquhart, Sheona A. No. 1 Section 4 Roosevelt Rd. Taipei10617 Taiwan Graduate Institute of Astronomy National Central University 300 Zhongda Road Zhongli Taoyuan32001 Taiwan Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Department of Physics and Atmospheric Science Dalhousie University Halifax HalifaxNSB3H 3J5 Canada 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 Department of Earth Science Education Kyungpook National University 80 Daehak-ro Buk-gu Daegu41566 Korea Republic of Astronomical Institute Tohoku University 6-3 Aramaki Aoba Miyagi Sendai980-8578 Japan Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu30013 Taiwan Imperial College London Blackett Laboratory Prince Consort Road LondonSW7 2AZ United Kingdom SUPA Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Department of Philosophy National Taiwan University No. 1 Section 4 Roosevelt Rd. Taipei10617 Taiwan 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 Faculty of Physics Astronomy and Informatics Nicolaus Copernicus University Grudziadzka 5 Torun87-100 Poland Department of Physics and Astronomy University of British Columbia 6224 Agricultural Road VancouverBCV6T 1Z1 Canada School of Physical Sciences The Open University Milton KeynesMK7 6AA United Kingdom

We present confusion-limited SCUBA-2 450-µm observations in the COSMOS-CANDELS region as part of the JCMT Large program, SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). Our maps at 450 and 850 µm cover an area of 450 arcmin2. We achieved instrumental noise levels of σ450 = 0.59 mJy beam−1 and σ850 = 0.09 mJy beam−1 in the deepest area of each map. The corresponding confusion noise levels are estimated to be 0.65 and 0.36 mJy beam−1. Above the 4 (3.5) σ threshold, we detected 360 (479) sources at 450 µm and 237 (314) sources at 850 µm. We derive the deepest blank-field number counts at 450 µm, covering the flux-density range of 2 to 43 mJy. These are in agreement with other SCUBA-2 blank-field and lensing-cluster observations, but are lower than various model counts. We compare the counts with those in other fields and find that the field-to-field variance observed at 450 µm at the R = 6′ scale is consistent with Poisson noise, so there is no evidence of strong 2-D clustering at this scale. Additionally, we derive the integrated surface brightness at 450 µm down to 2.1 mJy to be (Equation presented) Jy deg−2, contributing to (41±4)% of the 450-µm extragalactic background light (EBL) measured by COBE and Planck. Our results suggest that the 450-µm EBL may be fully resolved at (Equation presented) mJy, which extremely deep lensing-cluster observations and next-generation submillimeter instruments with large aperture sizes may be able to achieve. © 2024, CC BY.

关键词： Galaxies

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Exploring the Strong Interaction of Three-Body Systems at the LHC

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physical Review X 2024年第3期14卷 031051页

作者： S. Acharya D. Adamová G. Aglieri Rinella M. Agnello N. Agrawal Z. Ahammed S. Ahmad S. U. Ahn I. Ahuja A. Akindinov M. Al-Turany D. Aleksandrov B. Alessandro H. M. Alfanda R. Alfaro Molina B. Ali A. Alici N. Alizadehvandchali A. Alkin J. Alme G. Alocco T. Alt A. R. Altamura I. Altsybeev J. R. Alvarado M. N. Anaam C. Andrei N. Andreou A. Andronic V. Anguelov F. Antinori P. Antonioli N. Apadula L. Aphecetche H. Appelshäuser C. Arata S. Arcelli M. Aresti R. Arnaldi J. G. M. C. A. Arneiro I. C. Arsene M. Arslandok A. Augustinus R. Averbeck M. D. Azmi H. Baba A. Badalà J. Bae Y. W. Baek X. Bai R. Bailhache Y. Bailung A. Balbino A. Baldisseri B. Balis D. Banerjee Z. Banoo R. Barbera F. Barile L. Barioglio M. Barlou B. Barman G. G. Barnaföldi L. S. Barnby V. Barret L. Barreto C. Bartels K. Barth E. Bartsch N. Bastid S. Basu G. Batigne D. Battistini B. Batyunya D. Bauri J. L. Bazo Alba I. G. Bearden C. Beattie P. Becht D. Behera I. Belikov A. D. C. Bell Hechavarria F. Bellini R. Bellwied S. Belokurova Y. A. V. Beltran G. Bencedi S. Beole Y. Berdnikov A. Berdnikova L. Bergmann M. G. Besoiu L. Betev P. P. Bhaduri A. Bhasin M. A. Bhat B. Bhattacharjee L. Bianchi N. Bianchi J. Bielčík J. Bielčíková J. Biernat A. P. Bigot A. Bilandzic G. Biro S. Biswas N. Bize J. T. Blair D. Blau M. B. Blidaru N. Bluhme C. Blume G. Boca F. Bock T. Bodova A. Bogdanov S. Boi J. Bok L. Boldizsár M. Bombara P. M. Bond G. Bonomi H. Borel A. Borissov A. G. Borquez Carcamo H. Bossi E. Botta Y. E. M. Bouziani L. Bratrud P. Braun-Munzinger M. Bregant M. Broz G. E. Bruno M. D. Buckland D. Budnikov H. Buesching S. Bufalino P. Buhler N. Burmasov Z. Buthelezi A. Bylinkin S. A. Bysiak M. Cai H. Caines A. Caliva E. Calvo Villar J. M. M. Camacho P. Camerini F. D. M. Canedo S. L. Cantway M. Carabas A. A. Carballo F. Carnesecchi R. Caron L. A. D. Carvalho J. Castillo Castellanos F. Catalano C. Ceballos Sanchez I. Chakaberia P. Chakraborty S. Chandra S. Chapeland M. Chartier S. Chattopadhyay T. Cheng C. Cheshkov B. Cheynis V. Chibante Barroso D. D. Chinellato E. Université Clermont Auvergne CNRS/IN2P3 LPC Clermont-Ferrand France Nuclear Physics Institute of the Czech Academy of Sciences Husinec-Řež Czech Republic Geneva Switzerland Dipartimento DISAT del Politecnico and Sezione INFN Turin Italy INFN Sezione di Bologna Bologna Italy Variable Energy Cyclotron Centre Homi Bhabha National Institute Kolkata India Department of Physics Aligarh Muslim University Aligarh India Korea Institute of Science and Technology Information Daejeon Republic of Korea Faculty of Science P.J. Šafárik University Košice Slovak Republic Affiliated with an institute covered by a cooperation agreement with CERN Research Division and ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH Darmstadt Germany INFN Sezione di Torino Turin Italy Central China Normal University Wuhan China Instituto de Física Universidad Nacional Autónoma de México Mexico City Mexico Dipartimento di Fisica e Astronomia dell’Università Bologna Italy and Sezione INFN Bologna Italy University of Houston Houston Texas USA Department of Physics and Technology University of Bergen Bergen Norway INFN Sezione di Cagliari Cagliari Italy Institut für Kernphysik Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany INFN Sezione di Bari Bari Italy Physik Department Technische Universität München Munich Germany High Energy Physics Group Universidad Autónoma de Puebla Puebla Mexico Horia Hulubei National Institute of Physics and Nuclear Engineering Bucharest Romania University of Derby Derby United Kingdom Universität Münster Institut für Kernphysik Münster Germany Physikalisches Institut Ruprecht-Karls-Universität Heidelberg Heidelberg Germany INFN Sezione di Padova Padova Italy Lawrence Berkeley National Laboratory Berkeley California USA SUBATECH IMT Atlantique Nantes Université CNRS-IN2P3 Nantes France Laboratoire de Physique Subatomique et de Cosmologie Université Grenoble-Alpes CNRS-IN2P3 Grenoble France Dipar

Deuterons are atomic nuclei composed of a neutron and a proton held together by the strong interaction. Unbound ensembles composed of a deuteron and a third nucleon have been investigated in the past using scattering experiments, and they constitute a fundamental reference in nuclear physics to constrain nuclear interactions and the properties of nuclei. In this work, K+−d and p−d femtoscopic correlations measured by the ALICE Collaboration in proton-proton (pp) collisions at s=13 TeV at the Large Hadron Collider (LHC) are presented. It is demonstrated that correlations in momentum space between deuterons and kaons or protons allow us to study three-hadron systems at distances comparable with the proton radius. The analysis of the K+−d correlation shows that the relative distances at which deuterons and protons or kaons are produced are around 2 fm. The analysis of the p−d correlation shows that only a full three-body calculation that accounts for the internal structure of the deuteron can explain the data. In particular, the sensitivity of the observable to the short-range part of the interaction is demonstrated. These results indicate that correlations involving light nuclei in pp collisions at the LHC will also provide access to any three-body system in the strange and charm sectors.

关键词： Hadron-hadron interactions

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ATOMS: ALMA three-millimeter observations of massive star-forming regions – XVIII. On the origin and evolution of dense gas fragments in molecular shells of compact H ii regions

arXiv

引用

arXiv 2024年

作者： Zhang, Siju Liu, Tie Wang, Ke Zavagno, Annie Garay, Guido Liu, Hongli Xu, Fengwei Liu, Xunchuan Sanhueza, Patricio Soam, Archana Zhou, Jian-Wen Li, Shanghuo Goldsmith, Paul F. Zhang, Yong Chibueze, James O. Lee, Chang Won Hwang, Jihye Bronfman, Leonardo Dewangan, Lokesh K. Kavli Institute for Astronomy and Astrophysics Peking University 5 Yiheyuan Road Haidian District Beijing100871 China Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Key Laboratory for Research in Galaxies and Cosmology Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Aix Marseille Univ CNRS CNES LAM Marseille France Institut Universitaire de France Paris 1 rue Descartes Paris75231 Cedex 05 France Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China School of Physics and Astronomy Yunnan University Kunming650091 China Department of Astronomy School of Physics Peking University Beijing100871 China National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Indian Institute of Astrophysics II Block Koramangala Bengaluru560034 India Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany Max Planck Institute for Astronomy Konigstuhl 17 HeidelbergD-69117 Germany Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States School of Physics and Astronomy Sun Yat-sen University 2 Daxue Road Tangjia Guangdong Province Zhuhai China Department of Mathematical Sciences University of South Africa Cnr Christian de Wet Rd and Pioneer Avenue Florida Park Roodepoort1709 South Africa Department of Physics and Astronomy Faculty of Physical Sciences University of Nigeria Carver Building 1 University Road Nsukka410001 Nigeria Korea Astronomy and Space Science Institute 776 Daedeokdaero Yuseong-gu Daejeon34055 Korea Republic of 217 Gajeong-ro Yuseong-gu Daejeon341

Fragmentation and evolution for the molecular shells of the compact H ii regions are less explored compared to their evolved counterparts. We map nine compact H ii regions with a typical diameter of 0.4 pc that are surrounded by molecular shells traced by CCH. Several to a dozen dense gas fragments probed by H13CO+ are embedded in these molecular shells. These gas fragments, strongly affected by the H ii region, have a higher surface density, mass, and turbulence than those outside the shells but within the same pc-scale natal clump. These features suggest that the shells swept up by the early H ii regions can enhance the formation of massive dense structures that may host the birth of higher-mass stars. We examine the formation of fragments and find that fragmentation of the swept-up shell is unlikely to occur in these early H ii regions, by comparing the expected time scale of shell fragmentation with the age of H ii region. We propose that the appearance of gas fragments in these shells is probably the result of sweeping up pre-existing fragments into the molecular shell that has not yet fragmented. Taken together, this work provides a basis for understanding the interplay of star-forming sites with an intricate environment containing ionization feedback such as those observed in starburst regions. © 2024, CC BY.

关键词： Giant stars

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Transverse ultrafast laser inscription in bulk silicon

arXiv

引用

arXiv 2021年

作者： Chambonneau, Maxime Blothe, M. Li, Q. Fedorov, V.Yu. Heuermann, T. Gebhardt, M. Gaida, C. Tertelmann, S. Sotier, F. Limpert, J. Tzortzakis, S. Nolte, S. Abbe Center of Photonics Institute of Applied Physics Friedrich-Schiller-University Jena Albert-Einstein-Strae 15 Jena07745 Germany Science Program Texas A and M University at Qatar P.O. Box 23874 Doha Qatar P. N. Lebedev Physical Institute of Russian Academy of Sciences 53 Leninskiy Prospekt Moscow119991 Russia Helmholtz-Institute Jena Frobelstieg 3 Jena07743 Germany Active Fiber Systems GmbH Ernst-Ruska-Ring 17 Jena07745 Germany Innolas Photonics GmbH Justus-von-Liebig-Ring 8 Krailling82152 Germany Center of Excellence in Photonics Fraunhofer Institute for Applied Optics and Precision Engineering Iof Albert-Einstein-Strae 7 Jena07745 Germany P.O. Box 1527 HeraklionGR-71110 Greece Materials Science and Technology Department University of Crete Heraklion71003 Greece

In-volume ultrafast laser direct writing of silicon is generally limited by strong nonlinear propagation effects preventing the initiation of modifications. By employing a triple-optimization procedure in the spectral, temporal and spatial domains, we demonstrate that modifications can be repeatably produced inside silicon. Our approach relies on irradiation at 2-μm wavelength with temporallydistorted femtosecond pulses. These pulses are focused in a way that spherical aberrations of different origins counterbalance, as predicted by point spread function analyses and in good agreement with nonlinear propagation simulations. We also establish the laws governing modification growth on a pulse-to-pulse basis, which allows us to demonstrate transverse inscription inside silicon with various line morphologies depending on the irradiation conditions. We finally show that the production of single-pulse repeatable modifications is a necessary condition for reliable transverse inscription inside silicon. © 2021, CC BY.

关键词： Silicon

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