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arXiv 2022年

作者： Jiménez-Serra, Izaskun Rodríguez-Almeida, Lucas F. Martín-Pintado, Jesús Rivilla, Víctor M. Melosso, Mattia Zeng, Shaoshan Colzi, Laura Kawashima, Yoshiyuki Hirota, Eizi Puzzarini, Cristina Tercero, Belén de Vicente, Pablo Rico-Villas, Fernando Requena-Torres, Miguel A. Martín, Sergio Ctra. de Torrejón a Ajalvir km 4 Torrejón de Ardoz E-28806 Spain INAF-Osservatorio Astrofisico di Arcetri Largo Enrico Fermi 5 Florence50125 Italy Dipartimento di Chimica "Giacomo Ciamician" Universitá di Bologna via F. Selmi 2 Bologna40126 Italy Star and Planet Formation Laboratory Cluster for Pioneering Research RIKEN 2-1 Hirosawa Wako Saitama351-0198 Japan Department of Applied Chemistry Faculty of Engineering Kanagawa Institute of Technology Kanagawa Atsugi240-0292 Japan The Graduate University for Advanced Studies Kanagawa Hayama240-0193 Japan Cerro de la Palera s/n GuadalajaraE-19141 Spain University of Maryland ND College Park20742-2421 United States Department of Physics Astronomy and Geosciences Towson University MD21252 United States European Southern Observatory Alonso de Córdova 3107 Vitacura Santiago763 0355 Chile Joint ALMA Observatory Alonso de Córdova 3107 Vitacura Santiago763 0355 Chile

Context. Theories on the origins of life propose that early cell membranes were synthesized from amphiphilic molecules simpler than phospholipids such as fatty alcohols. The discovery in the interstellar medium (ISM) of ethanolamine, the simplest phospholipid head group, raises the question whether simple amphiphilic molecules are also synthesized in space. Aims. We investigate whether precursors of fatty alcohols are present in the ISM. Methods. For this, we have carried out a spectral survey at 7, 3, 2 and 1 mm toward the Giant Molecular Cloud G+0.693-0.027 located in the Galactic Center using the IRAM 30 m and Yebes 40 m telescopes. Results. Here, we report the detection in the ISM of the primary alcohol n-propanol (in both conformers Ga-n-C3H7OH and Aan-C3H7OH), a precursor of fatty alcohols. The derived column densities of n-propanol are (5.5±0.4)×1013 cm−2 for the Ga conformer and (3.4±0.3)×1013 cm−2 for the Aa conformer, which imply molecular abundances of (4.1±0.3)×10−10 for Ga-n-C3H7OH and of (2.5±0.2)×10−10 for Aa-n-C3H7OH. We also searched for the AGa conformer of n-butanol [AGa-n-C4H9OH] without success yielding an upper limit to its abundance of ≤4.1×10−11. The inferred CH3OH:C2H5OH:C3H7OH:C4H9OH abundance ratios go as 1:0.04:0.006:≤0.0004 toward G+0.693-0.027, i.e. they decrease roughly by one order of magnitude for increasing complexity. We also report the detection of both syn and anti conformers of vinyl alcohol, with column densities of (1.11±0.08)×1014 cm−2 and (1.3±0.4)×1013 cm−2, and abundances of (8.2±0.6)×10−10 and (9.6±3.0)×10−11, respectively. Conclusions. The detection of n-propanol, together with the recent discovery of ethanolamine in the ISM, opens the possibility that precursors of lipids according to theories of the origin of life, could have been brought to Earth from outer space. © 2022, CC BY.

关键词： Alcohols

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Classification of datasets with imputed missing values: does imputation quality matter?

arXiv

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arXiv 2022年

作者： Shadbahr, Tolou Roberts, Michael Stanczuk, Jan Gilbey, Julian Teare, Philip Dittmer, Sören Thorpe, Matthew Torné, Ramon Viñas Sala, Evis Lió, Pietro Patel, Mishal Rudd, James H.F. Mirtti, Tuomas Rannikko, Antti Sakari Aston, John A.D. Tang, Jing Schönlieb, Carola-Bibiane Selby, Ian Breger, Anna Weir-McCall, Jonathan R. Gkrania-Klotsas, Effrossyni Korhonen, Anna Jefferson, Emily Langs, Georg Yang, Guang Prosch, Helmut Preller, Jacobus Stanczuk, Jan Babar, Judith Sánchez, Lorena Escudero Wassin, Marcel Holzer, Markus Walton, Nicholas Research Program in Systems Oncology Faculty of Medicine University of Helsinki Helsinki Finland Department of Applied Mathematics and Theoretical Physics University of Cambridge Cambridge United Kingdom Data Science & Artificial Intelligence AstraZeneca Cambridge United Kingdom Department of Mathematics University of Manchester Manchester United Kingdom Department of Computer Science and Technology University of Cambridge Cambridge United Kingdom Department of Radiology University of Cambridge Cambridge United Kingdom Clinical Pharmacology & Safety Sciences AstraZeneca Cambridge United Kingdom Department of Medicine University of Cambridge Cambridge United Kingdom Department of Pathology University of Helsinki Helsinki University Hospital Finland iCAN-Digital Precision Cancer Medicine Flagship Helsinki Finland Department of Urology University of Helsinki Helsinki University Hospital Helsinki Finland Department of Pure Mathematics and Mathematical Statistics University of Cambridge Cambridge United Kingdom ZeTeM University of Bremen Bremen Germany Faculty of Mathematics University of Vienna Austria Royal Papworth Hospital Cambridge Royal Papworth Hospital NHS Foundation Trust Cambridge United Kingdom Addenbrooke’s Hospital Cambridge University Hospitals NHS Trust Cambridge United Kingdom Language Technology Laboratory University of Cambridge Cambridge United Kingdom Population Health and Genomics School of Medicine University of Dundee Dundee United Kingdom Department of Biomedical Imaging and Image-guided Therapy Computational Imaging Research Lab Medical University of Vienna Vienna Austria National Heart and Lung Institute Imperial College London London United Kingdom Contextflow GmbH Vienna Austria Institute of Astronomy University of Cambridge Cambridge United Kingdom

Classifying samples in incomplete datasets is a common aim for machine learning practitioners, but is non-trivial. Missing data is found in most real-world datasets and these missing values are typically imputed using established methods, followed by classification of the now complete, imputed, samples. The focus of the machine learning researcher is then to optimise the downstream classification performance. In this study, we highlight that it is imperative to consider the quality of the imputation. We demonstrate how the commonly used measures for assessing quality are flawed and propose a new class of discrepancy scores which focus on how well the method recreates the overall distribution of the data. To conclude, we highlight the compromised interpretability of classifier models trained using poorly imputed data. All code and data used in this paper are also released publicly at [inserted upon publication]. © 2022, CC BY.

关键词： Classification (of information)

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Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo’s first three observing runs

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Physical Review D 2021年第2期104卷 022005-022005页

作者： R. Abbott T. D. Abbott S. Abraham F. Acernese K. Ackley A. Adams C. Adams R. X. Adhikari V. B. Adya C. Affeldt D. Agarwal M. Agathos K. Agatsuma N. Aggarwal O. D. Aguiar L. Aiello A. Ain P. Ajith T. Akutsu K. M. Aleman G. Allen A. Allocca P. A. Altin A. Amato S. Anand A. Ananyeva S. B. Anderson W. G. Anderson M. Ando S. V. Angelova S. Ansoldi J. M. Antelis S. Antier S. Appert Koya Arai Koji Arai Y. Arai S. Araki A. Araya M. C. Araya J. S. Areeda M. Arène N. Aritomi N. Arnaud S. M. Aronson H. Asada Y. Asali G. Ashton Y. Aso S. M. Aston P. Astone F. Aubin P. Aufmuth K. AultONeal C. Austin S. Babak F. Badaracco M. K. M. Bader S. Bae Y. Bae A. M. Baer S. Bagnasco Y. Bai L. Baiotti J. Baird R. Bajpai M. Ball G. Ballardin S. W. Ballmer M. Bals A. Balsamo G. Baltus S. Banagiri D. Bankar R. S. Bankar J. C. Barayoga C. Barbieri B. C. Barish D. Barker P. Barneo F. Barone B. Barr L. Barsotti M. Barsuglia D. Barta J. Bartlett M. A. Barton I. Bartos R. Bassiri A. Basti M. Bawaj J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale M. Bejger I. Belahcene V. Benedetto D. Beniwal M. G. Benjamin T. F. Bennett J. D. Bentley M. BenYaala F. Bergamin B. K. Berger S. Bernuzzi D. Bersanetti A. Bertolini J. Betzwieser R. Bhandare A. V. Bhandari D. Bhattacharjee S. Bhaumik J. Bidler I. A. Bilenko G. Billingsley R. Birney O. Birnholtz S. Biscans M. Bischi S. Biscoveanu A. Bisht B. Biswas M. Bitossi M.-A. Bizouard J. K. Blackburn J. Blackman C. D. Blair D. G. Blair R. M. Blair F. Bobba N. Bode M. Boer G. Bogaert M. Boldrini F. Bondu E. Bonilla R. Bonnand P. Booker B. A. Boom R. Bork V. Boschi N. Bose S. Bose V. Bossilkov V. Boudart Y. Bouffanais A. Bozzi C. Bradaschia P. R. Brady A. Bramley A. Branch M. Branchesi J. E. Brau M. Breschi T. Briant J. H. Briggs A. Brillet M. Brinkmann P. Brockill A. F. Brooks J. Brooks D. D. Brown S. Brunett G. Bruno R. Bruntz J. Bryant A. Buikema T. Bulik H. J. Bulten A. Buonanno R. Buscicchio D. Buskulic R. L. Byer L. Cadonati M. Caesar G. Cagnoli C. Cahillane H. W. Cain, III J. Calderón Bustillo J. LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Louisiana State University Baton Rouge Louisiana 70803 USA Inter-University Centre for Astronomy and Astrophysics Pune 411007 India Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli Complesso Universitario di Monte S.Angelo I-80126 Napoli Italy OzGrav School of Physics & Astronomy Monash University Clayton 3800 Victoria Australia Christopher Newport University Newport News Virginia 23606 USA LIGO Livingston Observatory Livingston Louisiana 70754 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany University of Cambridge Cambridge CB2 1TN United Kingdom Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany University of Birmingham Birmingham B15 2TT United Kingdom Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA) Northwestern University Evanston Illinois 60208 USA Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Gravity Exploration Institute Cardiff University Cardiff CF24 3AA United Kingdom Gran Sasso Science Institute (GSSI) I-67100 L’Aquila Italy INFN Laboratori Nazionali del Gran Sasso I-67100 Assergi Italy INFN Sezione di Pisa I-56127 Pisa Italy Università di Pisa I-56127 Pisa Italy International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan California State University Fullerton Fullerton California 92831 USA NCSA University of Illinois

We report results from searches for anisotropic stochastic gravitational-wave backgrounds using data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. For the first time, we include Virgo data in our analysis and run our search with a new efficient pipeline called pystoch on data folded over one sidereal day. We use gravitational-wave radiometry (broadband and narrow band) to produce sky maps of stochastic gravitational-wave backgrounds and to search for gravitational waves from point sources. A spherical harmonic decomposition method is employed to look for gravitational-wave emission from spatially-extended sources. Neither technique found evidence of gravitational-wave signals. Hence we derive 95% confidence-level upper limit sky maps on the gravitational-wave energy flux from broadband point sources, ranging from Fα,Θ<(0.013–7.6)×10−8 erg cm−2 s−1 Hz−1, and on the (normalized) gravitational-wave energy density spectrum from extended sources, ranging from Ωα,Θ<(0.57–9.3)×10−9 sr−1, depending on direction (Θ) and spectral index (α). These limits improve upon previous limits by factors of 2.9–3.5. We also set 95% confidence level upper limits on the frequency-dependent strain amplitudes of quasimonochromatic gravitational waves coming from three interesting targets, Scorpius X-1, SN 1987A and the Galactic Center, with best upper limits range from h0<(1.7–2.1)×10−25, a factor of ≥2.0 improvement compared to previous stochastic radiometer searches.

关键词： Experimental studies of gravity General relativity Gravitational waves

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Morpho-kinematic modeling of the expanding ejecta of the extremely slow nova V1280 Scorpii

arXiv

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arXiv 2022年

作者： Naito, Hiroyuki Tajitsu, Akito Ribeiro, Valério A.R.M. Arai, Akira Maehara, Hiroyuki Kouzuma, Shinjirou Iijima, Takashi Okazaki, Atsuo T. Watanabe, Makoto Takagi, Seiko Watanabe, Fumitake Sakon, Itsuki Sadakane, Kozo Nayoro Observatory 157-1 Nisshin Hokkaido Nayoro096-0066 Japan Graduate School of Science Nagoya University Furo-cho Chikusa-ku Aichi Nagoya464-8602 Japan Okayama Astrophysical Observatory National Astronomical Observatory of Japan NINS 3037-5 Honjo Kamogata Asakuchi Okayama719-0232 Japan Instituto de Telecomunicações Campus Universitário de Santiago Aveiro3810-193 Portugal Departamento de Física Universidade de Aveiro Campus Universitário de Santiago Aveiro3810-193 Portugal Department of Astrophysics IMAPP Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa Subaru Telescope National Astronomical Observatory of Japan 650 North A’ohoku Place HiloHI96720 United States Koyama Astronomical Observatory Kyoto Sangyo University Motoyama Kamigamo Kita-ku Kyoto603-8555 Japan Faculty of Liberal Arts and Sciences Chukyo University 101-2 Yagoto-honmachi Showa-ku Aichi Nagoya466-8666 Japan Astronomical Observatory of Padova Asiago Section Osservatorio Astrofisico Asiago Vi 36012 Italy Faculty of Engineering Hokkai-Gakuen University Toyohira-ku Hokkaido Sapporo062-8605 Japan Department of Applied Physics Okayama University of Science Kita-ku Okayama Okayama700-0005 Japan Department of Cosmosciences Hokkaido University Kita 10 Nishi 8 Kita-ku Hokkaido Sapporo060-0810 Japan Department of Astronomy Graduate Schools of Science University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Astronomical Institute Osaka Kyoiku University Asahigaoka Kashiwara Osaka582-8582 Japan

Morphology of nova ejecta is essential for fully understanding the physical processes involved in nova eruptions. We studied the 3D morphology of the expanding ejecta of the extremely slow nova V1280 Sco with a unique light curve. Synthetic line profile spectra were compared to the observed [O III] 4959, 5007 and [N II] 5755 emission line profiles in order to find the best-fit morphology, inclination angle, and maximum expansion velocity of the ejected shell. We derive the best fitting expansion velocity, inclination, and squeeze as Vexp = 2100+100-100 km s-1, i = 80+1-3 deg, and squ = 1.0+0.0-0.1 using [O III] line profiles, and Vexp = 1600+100-100 km s-1, i = 81+2-4 deg, and squ = 1.0+0.0-0.1 using [N II] 5755 line profile. A high inclination angle is consistent with the observational results showing multiple absorption lines originating from clumpy gases which are produced in dense and slow equatorially focused outflows. Based on additional observational features such as optical flares near the maximum light and dust formation on V1280 Sco, a model of internal shock interaction between slow ejecta and fast wind proposed for the γ-ray emission detected in other novae seems to be applicable to this extremely slow and peculiar nova. Increasing the sample size of novae whose morphology is studied will be helpful in addressing long-standing mysteries in novae such as the dominant energy source to power the optical light at the maximum, optical flares near the maximum, clumpiness of the ejecta, and dust formation. Copyright © 2022, The Authors. All rights reserved.

关键词： Morphology

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Lung cancer cells detection by a photoelectrochemical MoS2 biosensing chip

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Biomedical Optics Express 2024年第2期15卷 753-771页

作者： Chun-Liang Lai Riya Karmakar Arvind Mukundan Wei-Chung Chen I-Chen Wu Vladimir E. Fedorov Shih-Wei Feng Ubol Choomjinda Shu-Fang Huang Hsiang-Chen Wang Division of Pulmonology and Critical Care Department of Internal Medicine Dalin Tzu Chi Hospital Buddhist Tzu Chi Medical Foundation No. 2 Minsheng Road Dalin Chiayi 62247 Taiwan School of Medicine Tzu Chi University 701 Zhongyang Rd. Sec. 3 Hualien 97004 Taiwan Department of Mechanical Engineering and Center for Innovative Research on Aging Society (CIRAS) National Chung Cheng Universityhttps://***/0028v3876 168 University Road Min Hsiung Chiayi City 62102 Taiwan Ph.D. Program in Environmental and Occupational Medicine Kaohsiung Medical University Kaohsiung 807 Taiwan Department of Medicine and Graduate Institute of Clinical Medicine College of Medicine Kaohsiung Medical University No. 100 Tzyou 1st Rd. Sanmin Dist. Kaohsiung City 80756 Taiwan Nikolaev Institute of Inorganic Chemistry Siberian Branch of Russian Academy of Sciences Novosibirsk 630090 Russia Department of Natural Sciences Novosibirsk State University 1 Pirogova str. Novosibirsk 630090 Russia Department of Applied Physics National University of Kaohsiung 700 Kaohsiung University Rd. Nanzih District Kaohsiung 81148 Taiwan School of Nursing Shinawatra University 99 Moo 10 Bangtoey Samkhok Pathum Thani 12160 Thailand Division of Chest Medicine Kaohsiung Armed Forces General Hospital 2 Zhongzheng 1st. Rd. Kaohsiung City 80284 Taiwan ryanhuang1128@*** hcwang@ccu.edu.tw (hcwang@ccu.edu.tw)

This research aims to explore the potential application of this approach in the production of biosensor chips. The biosensor chip is utilized for the identification and examination of early-stage lung cancer cells. The findings of the optical microscope were corroborated by the field emission scanning electron microscopy, which provided further evidence that the growth of MoS 2 is uniform and that there is minimal disruption in the electrode, hence minimizing the likelihood of an open circuit creation. Furthermore, the bilayer structure of the produced MoS 2 has been validated through the utilization of Raman spectroscopy. A research investigation was undertaken to measure the photoelectric current generated by three various types of clinical samples containing lung cancer cells, specifically the CL1, NCI-H460, and NCI-H520 cell lines. The findings from the empirical analysis indicate that the coefficient of determination (R-Square) for the linear regression model was approximately 98%. Furthermore, the integration of a double-layer MoS 2 film resulted in a significant improvement of 38% in the photocurrent, as observed in the device's performance.

关键词： Absorption coefficient Chemical vapor deposition Optical absorption Physical vapor deposition Scanning electron microscopy Thin films

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A roadmap for the atmospheric characterization of terrestrial exoplanets with JWST

arXiv

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arXiv 2023年

作者： de Wit, Julien Doyon, René Rackham, Benjamin V. Lim, Olivia Ducrot, Elsa Kreidberg, Laura Benneke, Björn Ribas, Ignasi Berardo, David Niraula, Prajwal Iyer, Aishwarya Shapiro, Alexander Kostogryz, Nadiia Witzke, Veronika Gillon, Michaël Agol, Eric Meadows, Victoria Burgasser, Adam J. Owen, James E. Fortney, Jonathan J. Selsis, Franck Bello-Arufe, Aaron de Beurs, Zoë Bolmont, Emeline Cowan, Nicolas Dong, Chuanfei Drake, Jeremy J. Garcia, Lionel Greene, Thomas Haworth, Thomas Hu, Renyu Kane, Stephen R. Kervella, Pierre Koll, Daniel Krissansen-Totton, Joshua Lagage, Pierre-Olivier Lichtenberg, Tim Lustig-Yaeger, Jacob Lingam, Manasvi Turbet, Martin Seager, Sara Barkaoui, Khalid Bell, Taylor J. Burdanov, Artem Cadieux, Charles Charnay, Benjamin Cloutier, Ryan Cook, Neil J. Correia, Alexandre C.M. Dang, Lisa Daylan, Tansu Delrez, Laetitia Edwards, Billy Fauchez, Thomas J. Flagg, Laura Fraschetti, Federico Haqq-Misra, Jacob Huang, Ziyu Iro, Nicolas Jayawardhana, Ray Jehin, Emmanuel Jin, Meng Kite, Edwin Kitzmann, Daniel Kral, Quentin Lafrenière, David Libert, Anne-Sophie Liu, Beibei Mohanty, Subhanjoy Morris, Brett M. Murray, Catriona A. Piaulet, Caroline Pozuelos, Francisco J. Radica, Michael Ranjan, Sukrit Rathcke, Alexander Roy, Pierre-Alexis Schwieterman, Edward W. Turner, Jake D. Triaud, Amaury Way, Michael J. Department of Earth Atmospheric and Planetary Science Massachusetts Institute of Technology 77 Massachusetts Avenue CambridgeMA02139 United States Department of Physics Université de Montréal MontrealQC Canada Trottier Institute for Research on Exoplanets Université de Montréal MontrealQC Canada Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Paris Region Fellow Marie Sklodowska-Curie Action France AIM CEA CNRS Université Paris-Saclay Université de Paris Gif-sur-YvetteF-91191 France Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Campus UAB c/ Can Magrans s/n Bellaterra Barcelona08193 Spain c/ Gran Capità 2–4 Barcelona08034 Spain School of Earth and Space Exploration Arizona State University 525 E. University Dr. TempeAZ85281 United States Max Planck Institute for Solar System Research Göttingen Germany Astrobiology Research Unit Université de Liège 19C Allée du 6 Août Liège4000 Belgium Department of Astronomy and Astrobiology Program University of Washington Box 351580 SeattleWA98195 United States NASA Nexus for Exoplanet System Science Virtual Planetary Laboratory Team University of Washington Box 351580 SeattleWA98195 United States Center for Astrophysics and Space Sciences UC San Diego UCSD Mail Code 0424 9500 Gilman Drive La Jolla CA92093-0424 United States Astrophysics Group Imperial College London Blackett Laboratory Prince Consort Road LondonSW7 2AZ United Kingdom Department of Astronomy and Astrophysics University of California Santa Cruz Santa CruzCA95064 United States Laboratoire d’astrophysique de Bordeaux Univ. Bordeaux CNRS B18N allée Geoffroy Saint-Hilaire Pessac33615 France Jet Propulsion Laboratory California Institute of Technology PasadenaCA United States Observatoire astronomique de l’université de Genève Chemin Pegasi 51 VersoixCH-1290 Switzerland Centre Vie dans l’Univers Faculté des scien

Ultra-cool dwarf stars are abundant, long-lived, and uniquely suited to enable the atmospheric study of transiting terrestrial companions with JWST. Amongst them, the most prominent is the M8.5V star TRAPPIST-1 and its seven planets. While JWST Cycle 1 observations have started to yield preliminary insights into the planets, they have also revealed that their atmospheric exploration requires a better understanding of their host star. Here, we propose a roadmap to characterize the TRAPPIST-1 system—and others like it—in an efficient and robust manner with JWST. We notably recommend that—although more challenging to schedule—multi-transit windows be prioritized to mitigate the effects of stellar activity and gather up to twice more transits per JWST hour spent. We conclude that, for such systems, planets cannot be studied in isolation by small programs, but rather need large-scale, jointly space- and ground-based initiatives to fully exploit the capabilities of JWST for the exploration of terrestrial planets. © 2023, CC BY.

关键词： Stars

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Systematic studies of elliptic flow measurements in Au+Au collisions at sNN=200 GeV

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Physical Review C 2009年第2期80卷 024909-024909页

作者： S. Afanasiev C. Aidala N. N. Ajitanand Y. Akiba J. Alexander A. Al-Jamel K. Aoki L. Aphecetche R. Armendariz S. H. Aronson R. Averbeck T. C. Awes B. Azmoun V. Babintsev A. Baldisseri K. N. Barish P. D. Barnes B. Bassalleck S. Bathe S. Batsouli V. Baublis F. Bauer A. Bazilevsky S. Belikov R. Bennett Y. Berdnikov M. T. Bjorndal J. G. Boissevain H. Borel K. Boyle M. L. Brooks D. S. Brown D. Bucher H. Buesching V. Bumazhnov G. Bunce J. M. Burward-Hoy S. Butsyk S. Campbell J. -S. Chai S. Chernichenko J. Chiba C. Y. Chi M. Chiu I. J. Choi T. Chujo V. Cianciolo C. R. Cleven Y. Cobigo B. A. Cole M. P. Comets P. Constantin M. Csanád T. Csörgő T. Dahms K. Das G. David H. Delagrange A. Denisov D. d'Enterria A. Deshpande E. J. Desmond O. Dietzsch A. Dion J. L. Drachenberg O. Drapier A. Drees A. K. Dubey A. Durum V. Dzhordzhadze Y. V. Efremenko J. Egdemir A. Enokizono H. En'yo B. Espagnon S. Esumi D. E. Fields F. Fleuret S. L. Fokin B. Forestier Z. Fraenkel J. E. Frantz A. Franz A. D. Frawley Y. Fukao S. -Y. Fung S. Gadrat F. Gastineau M. Germain A. Glenn M. Gonin J. Gosset Y. Goto R. Granier de Cassagnac N. Grau S. V. Greene M. Grosse Perdekamp T. Gunji H. -Å. Gustafsson T. Hachiya A. Hadj Henni J. S. Haggerty M. N. Hagiwara H. Hamagaki H. Harada E. P. Hartouni K. Haruna M. Harvey E. Haslum K. Hasuko R. Hayano M. Heffner T. K. Hemmick J. M. Heuser X. He H. Hiejima J. C. Hill R. Hobbs M. Holmes W. Holzmann K. Homma B. Hong T. Horaguchi M. G. Hur T. Ichihara K. Imai M. Inaba D. Isenhower L. Isenhower M. Ishihara T. Isobe M. Issah A. Isupov B. V. Jacak J. Jia J. Jin O. Jinnouchi B. M. Johnson K. S. Joo D. Jouan F. Kajihara S. Kametani N. Kamihara M. Kaneta J. H. Kang T. Kawagishi A. V. Kazantsev S. Kelly A. Khanzadeev D. J. Kim E. Kim Y. -S. Kim E. Kinney A. Kiss E. Kistenev A. Kiyomichi C. Klein-Boesing L. Kochenda V. Kochetkov B. Komkov M. Konno D. Kotchetkov A. Kozlov P. J. Kroon G. J. Kunde N. Kurihara K. Kurita M. J. Kweon Y. Kwon G. S. Kyle R. Lacey J. G. Lajoie A. Lebedev Y. Le Bornec S. Leckey D. M. Lee M. K. Lee M. J. Joint Institute for Nuclear Research Moscow Region RU-141980 Dubna Russia Columbia University New York New York 10027 and Nevis Laboratories Irvington New York 10533 USA Chemistry Department Stony Brook University SUNY Stony Brook New York 11794 USA RIKEN Nishina Center for Accelerator-Based Science Wako Saitama 351-0198 Japan RIKEN BNL Research Center Brookhaven National Laboratory Upton New York 11973 USA New Mexico State University Las Cruces New Mexico 88003 USA Kyoto University Kyoto 606-8502 Japan SUBATECH (Ecole des Mines de Nantes CNRS-IN2P3 Université de Nantes) BP 20722 F-44307 Nantes France Brookhaven National Laboratory Upton New York 11973-5000 USA Department of Physics and Astronomy Stony Brook University SUNY Stony Brook New York 11794 USA Oak Ridge National Laboratory Oak Ridge Tennessee 37831 USA IHEP Protvino State Research Center of Russian Federation Institute for High Energy Physics Protvino RU-142281 Russia Dapnia CEA Saclay F-91191 Gif-sur-Yvette France University of California–Riverside Riverside California 92521 USA Los Alamos National Laboratory Los Alamos New Mexico 87545 USA University of New Mexico Albuquerque New Mexico 87131 USA PNPI Petersburg Nuclear Physics Institute Gatchina Leningrad region RU-188300 Russia Iowa State University Ames Iowa 50011 USA St. Petersburg State Polytechnic University St. Petersburg Russia Institut für Kernphysik University of Muenster D-48149 Muenster Germany KAERI Cyclotron Application Laboratory Seoul Korea KEK High Energy Accelerator Research Organization Tsukuba Ibaraki 305-0801 Japan Yonsei University IPAP Seoul 120-749 Korea Vanderbilt University Nashville Tennessee 37235 USA Georgia State University Atlanta Georgia 30303 USA IPN-Orsay Universite Paris Sud CNRS-IN2P3 BP1 F-91406 Orsay France ELTE Eötvös Loránd University H-1117 Budapest Pázmány P.s. 1/A Hungary KFKI Research Institute for Particle and Nuclear Physics of the Hungarian Academy of Scienc

We present inclusive charged hadron elliptic flow (v2) measured over the pseudorapidity range |η|6.5) pseudorapidities and (2) the two-particle cumulant method extracted using correlations between particles detected ...

We present inclusive charged hadron elliptic flow (v2) measured over the pseudorapidity range |η|<0.35 in Au+Au collisions at sNN=200 GeV. Results for v2 are presented over a broad range of transverse momentum (pT=0.2−8.0 GeV/c) and centrality (0–60%). To study nonflow effects that are correlations other than collective flow, as well as the fluctuations of v2, we compare two different analysis methods: (1) the event-plane method from two independent subdetectors at forward (|η|=3.1−3.9) and beam (|η|>6.5) pseudorapidities and (2) the two-particle cumulant method extracted using correlations between particles detected at midrapidity. The two event-plane results are consistent within systematic uncertainties over the measured pT and in centrality 0–40%. There is at most a 20% difference in the v2 between the two event-plane methods in peripheral (40–60%) collisions. The comparisons between the two-particle cumulant results and the standard event-plane measurements are discussed.

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High-pT π0 production with respect to the reaction plane in Au+Au collisions at sNN=200 GeV

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Physical Review C 2009年第5期80卷 054907-054907页

作者： S. Afanasiev C. Aidala N. N. Ajitanand Y. Akiba J. Alexander A. Al-Jamel K. Aoki L. Aphecetche R. Armendariz S. H. Aronson R. Averbeck T. C. Awes B. Azmoun V. Babintsev A. Baldisseri K. N. Barish P. D. Barnes B. Bassalleck S. Bathe S. Batsouli V. Baublis F. Bauer A. Bazilevsky S. Belikov R. Bennett Y. Berdnikov M. T. Bjorndal J. G. Boissevain H. Borel K. Boyle M. L. Brooks D. S. Brown D. Bucher H. Buesching V. Bumazhnov G. Bunce J. M. Burward-Hoy S. Butsyk S. Campbell J. -S. Chai S. Chernichenko J. Chiba C. Y. Chi M. Chiu I. J. Choi T. Chujo V. Cianciolo C. R. Cleven Y. Cobigo B. A. Cole M. P. Comets P. Constantin M. Csanád T. Csörgő T. Dahms K. Das G. David H. Delagrange A. Denisov D. d’Enterria A. Deshpande E. J. Desmond O. Dietzsch A. Dion J. L. Drachenberg O. Drapier A. Drees A. K. Dubey A. Durum V. Dzhordzhadze Y. V. Efremenko J. Egdemir A. Enokizono H. En’yo B. Espagnon S. Esumi D. E. Fields F. Fleuret S. L. Fokin B. Forestier Z. Fraenkel J. E. Frantz A. Franz A. D. Frawley Y. Fukao S. -Y. Fung S. Gadrat F. Gastineau M. Germain A. Glenn M. Gonin J. Gosset Y. Goto R. Granier de Cassagnac N. Grau S. V. Greene M. Grosse Perdekamp T. Gunji H. Å. Gustafsson T. Hachiya A. Hadj Henni J. S. Haggerty M. N. Hagiwara H. Hamagaki H. Harada E. P. Hartouni K. Haruna M. Harvey E. Haslum K. Hasuko R. Hayano M. Heffner T. K. Hemmick J. M. Heuser X. He H. Hiejima J. C. Hill R. Hobbs M. Holmes W. Holzmann K. Homma B. Hong T. Horaguchi M. G. Hur T. Ichihara K. Imai M. Inaba D. Isenhower L. Isenhower M. Ishihara T. Isobe M. Issah A. Isupov B. V. Jacak J. Jia J. Jin O. Jinnouchi B. M. Johnson K. S. Joo D. Jouan F. Kajihara S. Kametani N. Kamihara M. Kaneta J. H. Kang T. Kawagishi A. V. Kazantsev S. Kelly A. Khanzadeev D. J. Kim E. Kim Y. -S. Kim E. Kinney Á. Kiss E. Kistenev A. Kiyomichi C. Klein-Boesing L. Kochenda V. Kochetkov B. Komkov M. Konno D. Kotchetkov A. Kozlov P. J. Kroon G. J. Kunde N. Kurihara K. Kurita M. J. Kweon Y. Kwon G. S. Kyle R. Lacey J. G. Lajoie A. Lebedev Y. Le Bornec S. Leckey D. M. Lee M. K. Lee M. J. L Joint Institute for Nuclear Research RU-141980 Dubna Moscow Region Russia Columbia University New York New York 10027 and Nevis Laboratories Irvington New York 10533 USA Chemistry Department Stony Brook University Stony Brook SUNY New York 11794-3400 USA RIKEN Nishina Center for Accelerator-Based Science Wako Saitama 351-0198 Japan RIKEN BNL Research Center Brookhaven National Laboratory Upton New York 11973-5000 USA New Mexico State University Las Cruces New Mexico 88003 USA Kyoto University Kyoto 606-8502 Japan SUBATECH (Ecole des Mines de Nantes CNRS-IN2P3 Université de Nantes) BP 20722-44307 Nantes France Brookhaven National Laboratory Upton New York 11973-5000 USA Department of Physics and Astronomy Stony Brook University SUNY Stony Brook New York 11794 USA Oak Ridge National Laboratory Oak Ridge Tennessee 37831 USA IHEP Protvino State Research Center of Russian Federation Institute for High Energy Physics Protvino RU-142281 Russia Dapnia CEA Saclay F-91191 Gif-sur-Yvette France University of California-Riverside Riverside California 92521 USA Los Alamos National Laboratory Los Alamos New Mexico 87545 USA University of New Mexico Albuquerque New Mexico 87131 USA PNPI Petersburg Nuclear Physics Institute Gatchina Leningrad region RU-188300 Russia Iowa State University Ames Iowa 50011 USA Saint Petersburg State Polytechnic University St. Petersburg Russia Institut für Kernphysik University of Muenster D-48149 Muenster Germany KAERI Cyclotron Application Laboratory Seoul Korea KEK High Energy Accelerator Research Organization Tsukuba Ibaraki 305-0801 Japan Yonsei University IPAP Seoul 120-749 Korea Vanderbilt University Nashville Tennessee 37235 USA Georgia State University Atlanta Georgia 30303 USA IPN-Orsay Universite Paris Sud CNRS-IN2P3 BP1 F-91406 Orsay France ELTE Eötvös Loránd University H-1117 Budapest Pázmány P. s. 1/A Hungary KFKI Research Institute for Particle and Nuclear Physics of the Hungarian Academy

Measurements of the azimuthal anisotropy of high-pT neutral pion (π0) production in Au+Au collisions at sNN=200 GeV by the PHENIX experiment are presented. The data included in this article were collected during the 2004 Relativistic Heavy Ion Collider running period and represent approximately an order of magnitude increase in the number of analyzed events relative to previously published results. Azimuthal angle distributions of π0 mesons detected in the PHENIX electromagnetic calorimeters are measured relative to the reaction plane determined event-by-event using the forward and backward beam-beam counters. Amplitudes of the second Fourier component (v2) of the angular distributions are presented as a function of π0 transverse momentum (pT) for different bins in collision centrality. Measured reaction plane dependent π0 yields are used to determine the azimuthal dependence of the π0 suppression as a function of pT, RAA(Δϕ,pT). A jet-quenching motivated geometric analysis is presented that attempts to simultaneously describe the centrality dependence and reaction plane angle dependence of the π0 suppression in terms of the path lengths of hypothetical parent partons in the medium. This set of results allows for a detailed examination of the influence of geometry in the collision region and of the interplay between collective flow and jet-quenching effects along the azimuthal axis.

关键词： Planing DEPENDENCE Collisions

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Antiaromatic Sapphyrin Isomer: Transformation into Contracted Porphyrinoids with Variable Aromaticity

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Angewandte Chemie 2022年第1期135卷

作者： Dr. Qizhao Li Prof. Dr. Masatoshi Ishida Yunyun Wang Dr. Chengjie Li Dr. Glib Baryshnikov Dr. Bin Zhu Dr. Feng Sha Prof. Dr. Xinyan Wu Prof. Dr. Hans Ågren Prof. Dr. Hiroyuki Furuta Prof. Dr. Yongshu Xie Key Laboratory for Advanced Materials and Joint International Research Laboratory of Precision Chemistry and Molecular Engineering Feringa Nobel Prize Scientist Joint Research Center Frontiers Science Center for Materiobiology and Dynamic Chemistry School of Chemistry and Molecular Engineering East China University of Science & Technology 130 Meilong Road Shanghai 200237 P. R. China Department of Chemistry Graduate School of Science Tokyo Metropolitan University Tokyo 192-0397 Japan Department of Science and Technology Laboratory of Organic Electronics Linköping University 60174 Norrköping Sweden Department of Physics and Astronomy Uppsala University 75120 Uppsala Sweden Department of Applied Chemistry Graduate School of Engineering Kyushu University Fukuoka 819-0395 Japan

Sapphyrin is a pentapyrrolic expanded porphyrin with a 22π aromatic character. Herein, we report the synthesis of a 20π antiaromatic sapphyrin isomer 1 by oxidative cyclization of a pentapyrrane precursor P 5 with a terminal β-linked pyrrole. The resulting isomer 1 , containing a mis-linked bipyrrole unit in the skeleton, exhibits a reactivity for further oxidation due to the distinct antiaromatic electronic structure, affording a fused macrocycle 2 , possessing a spiro-carbon-containing [5.6.5.6]-tetracyclic structure. Subsequent treatment with an acid afforded a weakly aromatic pyrrolone-appended N-confused corrole 3 , and thermal fusion gave a [5.6.5.7]-tetracyclic-ring-embedded 14π aromatic triphyrin(2.1.1) analog 4 . The cyclization at the mis-linked pyrrole moiety of P 5 played a crucial role in synthesizing the antiaromatic porphyrinoid susceptible to facile transformation to novel porphyrinoids with variable aromaticity.

关键词： Antiaromaticity N-Confused Porphyrin Porphyrinoids Sapphyrin Skeletal Rearrangement

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Euclid: Early Release Observations – A preview of the Euclid era through a galaxy cluster magnifying lens

arXiv

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arXiv 2024年

作者： Atek, Hakim Gavazzi, R. Weaver, J.R. Diego, J.M. Schrabback, T. Hatch, N.A. Aghanim, N. Dole, H. Hartley, W.G. Taamoli, S. Congedo, G. Jimenez-Teja, Y. Cuillandre, J.-C. Bañados, E. Belladitta, S. Bowler, R.A.A. Franco, M. Jauzac, M. Mahler, G. Richard, J. Rocci, P.-F. Serjeant, S. Toft, S. Abriola, D. Bergamini, P. Biviano, A. Dimauro, P. Ezziati, M. Golden-Marx, J.B. Grillo, C. Hughes, A.C.N. Kang, Y. Kneib, J.-P. Lombardi, M. Mamon, G.A. McPartland, C.J.R. Meneghetti, M. Miyatake, H. Montes, M. Mortlock, D.J. Oesch, P.A. Okabe, N. Rosati, P. Taylor, A.N. Tarsitano, F. Weller, J. Kluge, M. Laureijs, R. Paltani, S. Saifollahi, T. Schirmer, M. Stone, C. Mora, A. Altieri, B. Amara, A. Andreon, S. Auricchio, N. Baldi, M. Balestra, A. Bardelli, S. Basset, A. Bender, R. Bodendorf, C. Bonino, D. Branchini, E. Brescia, M. Brinchmann, J. Camera, S. Candini, G.P. Capobianco, V. Carbone, C. Cardone, V.F. Carretero, J. Casas, S. Castander, F.J. Castellano, M. Cavuoti, S. Cimatti, A. Conselice, C.J. Conversi, L. Copin, Y. Corcione, L. Courbin, F. Courtois, H.M. Da Silva, A. Degaudenzi, H. Di Giorgio, A.M. Dinis, J. Douspis, M. Dubath, F. Dupac, X. Dusini, S. Ealet, A. Farina, M. Farrens, S. Ferriol, S. Fotopoulou, S. Frailis, M. Franceschi, E. Galeotta, S. Gillard, W. Gillis, B. Giocoli, C. Gómez-Alvarez, P. Grazian, A. Grupp, F. Guzzo, L. Hailey, M. Haugan, S.V.H. Hoar, J. Hoekstra, H. Holliman, M.S. Holmes, W. Hook, I. Hormuth, F. Hornstrup, A. Hudelot, P. Jahnke, K. Jhabvala, M. Keihänen, E. Kermiche, S. Kiessling, A. Kitching, T. Kohley, R. Kubik, B. Kuijken, K. Kümmel, M. Kunz, M. Kurki-Suonio, H. Lahav, O. Le Mignant, D. Ligori, S. Lilje, P.B. Lindholm, V. Lloro, I. Maino, D. Maiorano, E. Mansutti, O. Marggraf, O. Markovic, K. Martinet, N. Marulli, F. Massey, R. Maurogordato, S. McCracken, H.J. Mei, S. Mellier, Y. Merlin, E. Meylan, G. Moresco, M. Moscardini, L. Nakajima, R. Nichol, R.C. Institut d’Astrophysique de Paris UMR 7095 CNRS Sorbonne Université 98 bis boulevard Arago Paris75014 France Aix-Marseille Université CNRS CNES LAM Marseille France Department of Astronomy University of Massachusetts AmherstMA01003 United States Instituto de Física de Cantabria Edificio Juan Jordá Avenida de los Castros Santander39005 Spain Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstr. 25/8 Innsbruck6020 Austria School of Physics and Astronomy University of Nottingham University Park NottinghamNG7 2RD United Kingdom Université Paris-Saclay CNRS Institut d’astrophysique spatiale Orsay91405 France Department of Astronomy University of Geneva ch. d’Ecogia 16 Versoix1290 Switzerland Physics and Astronomy Department University of California 900 University Ave. RiversideCA92521 United States Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía Granada18080 Spain Observatorio Nacional Rua General Jose Cristino 77-Bairro Imperial de Sao Cristovao Rio de Janeiro20921-400 Brazil Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-Yvette91191 France Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 Bologna40129 Italy Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom The University of Texas at Austin AustinTX78712 United States Department of Physics Centre for Extragalactic Astronomy Durham University South Road DH1 3LE United Kingdom Department of Physics Institute for Computational Cosmology Durham University South Road DH1 3LE United Kingdom Astrophysics Research Centre University of KwaZulu-Natal Westville Campus Durban4041 South Africa School of

We present the first analysis of the Euclid Early Release Observations (ERO) program that targets fields around two lensing clusters, Abell 2390 and Abell 2764. We use VIS and NISP imaging to produce photometric catalogs for a total of ∼ 500 000 objects. The imaging data reach a 5 σ typical depth in the range 25.1–25.4 AB in the NISP bands, and 27.1–27.3 AB in the VIS band. Using the Lyman-break method in combination with photometric redshifts, we search for high-redshift galaxies. We identify 30 Lyman-break galaxy (LBG) candidates at z > 6 and 139 extremely red sources (ERSs), most likely at lower redshift. The deeper VIS imaging compared to NISP means we can routinely identify high-redshift Lyman breaks of the order of 3 magnitudes, which reduces contamination by brown dwarf stars and low-redshift galaxies. The difficulty of spatially resolving most of these sources in 0′′ . 3 pix−1 imaging makes the distinction between galaxies and quasars more challenging. Spectroscopic followup campaigns of such bright sources will help constrain both the bright end of the ultraviolet galaxy luminosity function and the quasar luminosity function at z > 6, and constrain the physical nature of these objects. Additionally, we have performed a combined strong lensing and weak lensing analysis of A2390, and demonstrate how Euclid will contribute to better constraining the virial mass of galaxy clusters. From these data, we also identify optical and near-infrared counterparts of known z > 0.6 clusters, which exhibit strong lensing features, establishing the ability of Euclid to characterize high-redshift clusters. Finally, we provide a glimpse of Euclid’s ability to map the intracluster light out to larger radii than current facilities, enabling a better understanding of the cluster assembly history and mapping of the dark matter distribution. This initial dataset illustrates the diverse spectrum of legacy science that will be enabled by the Euclid survey. © 2024, CC BY.

关键词： Galaxies

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