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ALMAGAL I. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. Presentation of the survey and early results

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arXiv 2025年

作者： Molinari, S. Schilke, P. Battersby, C. Ho, P.T.P. Sánchez-Monge, Á. Traficante, A. Jones, B. Beltrán, M.T. Beuther, H. Fuller, G.A. Zhang, Q. Klessen, R.S. Walch, S. Tang, Y.-W. Benedettini, M. Elia, D. Coletta, A. Mininni, C. Schisano, E. Avison, A. Law, C.Y. Nucara, A. Soler, J.D. Stroud, G. Wallace, J. Wells, M.R.A. Ahmadi, A. Brogan, C.L. Hunter, T.R. Liu, S.-Y. Pezzuto, S. Su, Y.-N. Zimmermann, B. Zhang, T. Wyrowski, F. De Angelis, F. Liu, S. Clarke, S.D. Fontani, F. Klaassen, P.D. Koch, P. Johnston, K.G. Lebreuilly, U. Liu, T. Lumsden, S.L. Moeller, T. Moscadelli, L. Kuiper, R. Lis, D. Peretto, N. Pfalzner, S. Rigby, A.J. Sanhueza, P. Rygl, K.L.J. van der Tak, F. Zinnecker, H. Amaral, F. Bally, J. Bronfman, L. Cesaroni, R. Goh, K. Hoare, M.G. Hatchfield, P. Hennebelle, P. Henning, T. Kim, K.T. Kim, W.-J. Maud, L. Merello, M. Nakamura, F. Plume, R. Qin, S.-L. Svoboda, B. Testi, L. Veena, V.S. Walker, D. Istituto di Astrofisica e Planetologia Spaziale Via Fosso del Cavaliere 100 RomaI-00133 Italy Physikalisches Institut der Universität zu Köln Zülpicher Str. 77 KölnD-50937 Germany University of Connecticut United States Institute of Astronomy and Astrophysics Academia Sinica 11F of ASMAB AS/NTU No. 1 Sec. 4 Roosevelt Road Taipei10617 Taiwan Campus UAB Carrer de Can Magrans s/n Bellaterra BarcelonaE-08193 Spain Castelldefels BarcelonaE-08860 Spain Max Planck Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany SKA Observatory Jodrell Bank Lower Withington MacclesfieldSK11 9FT United Kingdom Jodrell Bank Centre for Astrophysics Department of Physics & Astronomy The University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Universität Heidelberg Zentrum für Astronomie Institut für Theoretische Astrophysik Albert-Ueberle-Straße 2 HeidelbergD-69120 Germany Universität Heidelberg Interdisziplinäres Zentrum für Wissenschaftliches Rechnen Im Neuenheimer Feld 205 HeidelbergD-69120 Germany Center for Data and Simulation Science University of Cologne Germany Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Radcliffe Institute for Advanced Studies Harvard University 10 Garden Street CambridgeMA02138 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Dipartimento di Fisica Università di Roma Tor Vergata Via della Ricerca Scientifica 1 RomaI-00133 Italy Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Florence Italy Garching bei München Germany Observatoire de Paris Meudon France UK Astronomy Technology Centre Royal Observatory Edinburgh Blackford Hill EdinburghEH9 3HJ United Kingdom School of Engineering and Physical Sciences Isaac Newton Building Un

Context. A large fraction of stars form in clusters containing high-mass stars, which subsequently influences the local and galaxy-wide environment. Aims. Fundamental questions about the physics responsible for fragmenting molecular parsec-scale clumps into cores of a few thousand astronomical units (au) are still open, that only a statistically significant investigation with ALMA is able to address;for instance: the identification of the dominant agents that determine the core demographics, mass, and spatial distribution as a function of the physical properties of the hosting clumps, their evolutionary stage and the different Galactic environments in which they reside. The extent to which fragmentation is driven by clumps dynamics or mass transport in filaments also remains elusive. Methods. With the ALMAGAL project, we observed the 1.38 mm continuum and lines toward more than 1000 dense clumps in our Galaxy, with M ≥ 500 M☉, Σ ≥ 0.1 g cm−2 and d ≤ 7.5 kiloparsec (kpc). Two different combinations of ALMA Compact Array (ACA) and 12-m array setups were used to deliver a minimum resolution of ∼1000 au over the entire sample distance range. The sample covers all evolutionary stages from infrared dark clouds (IRDCs) to Hii regions from the tip of the Galactic bar to the outskirts of the Galaxy. With a continuum sensitivity of 0.1 mJy, ALMAGAL enables a complete study of the clump-to-core fragmentation process down to M ∼ 0.3 M☉ across the Galaxy. The spectral setup includes several molecular lines to trace the multiscale physics and dynamics of gas, notably CH3CN, H2CO, SiO, CH3OH, DCN, HC3N, and SO, among others. Results. We present an initial overview of the observations and the early science product and results produced in the ALMAGAL Consortium, with a first characterization of the morphological properties of the continuum emission detected above 5σ in our fields. We used "perimeter-versus-area" and convex hull-versus-area metrics to classify the different morpholog

关键词： Giant stars

ALMAGAL II. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy ALMA data processing and pipeline

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arXiv 2025年

作者： Sánchez-Monge, Á. Brogan, C.L. Hunter, T.R. Ahmadi, A. Avison, A. Beltrán, M.T. Beuther, H. Coletta, A. Fuller, G.A. Johnston, K.G. Jones, B. Liu, S.-Y. Mininni, C. Molinari, S. Schilke, P. Schisano, E. Su, Y.-N. Traficante, A. Zhang, Q. Battersby, C. Benedettini, M. Elia, D. Ho, P.T.P. Klaassen, P.D. Klessen, R.S. Law, C.Y. Lis, D.C. Liu, T. Maud, L. Möller, T. Moscadelli, L. Pezzuto, S. Rygl, K.L.J. Sanhueza, P. Soler, J.D. Stroud, G. Tang, Y. van der Tak, F.F.S. Walker, D.L. Wallace, J. Walch, S. Wells, M.R.A. Wyrowski, F. Zhang, T. Allande, J. Bronfman, L. Dann, E. De Angelis, F. Fontani, F. Henning, Th. Kim, W.-J. Kuiper, R. Merello, M. Nakamura, F. Nucara, A. Rigby, A.J. CSIC Campus UAB Carrer de Can Magrans s/n Bellaterra BarcelonaE-08193 Spain Castelldefels BarcelonaE-08860 Spain National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands SKA Observatory Jodrell Bank Lower Withington MacclesfieldSK11 9FT United Kingdom Jodrell Bank Centre for Astrophysics The University of Manchester Oxford Road ManchesterM13 9PL United Kingdom UK ALMA Regional Centre Node M13 9PL United Kingdom INAF-Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 FirenzeI-50125 Italy Max Planck Institute for Astronomy Königstuhl 17 HeidelbergD-69117 Germany INAF-Istituto di Astrofisica e Planetologia Spaziale Via Fosso del Cavaliere 100 RomaI-00133 Italy Dipartimento di Fisica Sapienza Università di Roma Piazzale Aldo Moro 2 RomeI-00185 Italy I. Physikalisches Institut Universität zu Köln Zülpicher Str. 77 KölnD-50937 Germany School of Engineering and Physical Sciences Isaac Newton Building University of Lincoln Brayford Pool LincolnLN6 7TS United Kingdom Institute of Astronomy and Astrophysics Academia Sinica 11F of ASMAB AS/NTU No. 1 Sec. 4 Roosevelt Road Taipei10617 Taiwan Center for Astrophysics Harvard & Smithsonian 60 Garden St CambridgeMA02138 United States University of Connecticut Department of Physics 2152 Hillside Road Unit 3046 StorrsCT06269 United States East Asian Observatory 660 N. A’ohoku Hawaii HiloHI96720 United States UK Astronomy Technology Centre Royal Observatory Edinburgh Blackford Hill EdinburghEH9 3HJ United Kingdom Universität Heidelberg Zentrum für Astronomie Institut für Theoretische Astrophysik Heidelberg Germany Universität Heidelberg Interdisziplinäres Zentrum für Wissenschaftliches Rechnen Heidelberg Germany Radcliffe Institute for Advanced Studies Harvard University 10 Garden Street CambridgeMA02138 United States Jet Propulsion Laboratory California Institute o

Context. Stars form preferentially in clusters embedded inside massive molecular clouds, many of which contain high-mass stars. Thus, a comprehensive understanding of star formation requires a robust and statistically well-constrained characterization of the formation and early evolution of these high-mass star clusters. To achieve this, we designed the ALMAGAL Large Program that observed 1017 high-mass star-forming regions distributed throughout the Galaxy, sampling different evolutionary stages and environmental conditions. Aims. In this work, we present the acquisition and processing of the ALMAGAL data. The main goal is to set up a robust pipeline that generates science-ready products, that is, continuum and spectral cubes for each ALMAGAL field, with a good and uniform quality across the whole sample. Methods. ALMAGAL observations were performed with the Atacama Large Millimeter/submillimeter Array (ALMA). Each field was observed in three different telescope arrays, being sensitive to spatial scales ranging from ≈ 1000 au up to ≈ 0.1 pc. The spectral setup allows sensitive (≈ 0.1 mJy beam−1) imaging of the continuum emission at 219 GHz (or 1.38 mm), and it covers multiple molecular spectral lines observed in four different spectral windows that span about ≈ 4 GHz in frequency coverage. We have designed a Python-based processing workflow to calibrate and image these observational data. This ALMAGAL pipeline includes an improved continuum determination, suited for line-rich sources;an automatic self-calibration process that reduces phase-noise fluctuations and improves the dynamical range by up to a factor ≈ 5 in about 15% of the fields;and the combination of data from different telescope arrays to produce science-ready, fully combined images. Results. The final products are a set of uniformly generated continuum images and spectral cubes for each ALMAGAL field, including individual-array and combined-array products. The fully combined products have spatial resol

关键词： Giant stars

Improvements in miniaturized Hall Thrusters by use of high-temperature SmCo magnets and additive manufacturing techniques

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IOP Conference Series: Materials science and Engineering 2019年第1期576卷

作者： A Olano J Ren G Zhang H Tang T Zhang J Li Key Laboratory of Spacecraft Design Optimization & Dynamic Simulation Technologies of Ministry of Education School of Astronautics Beihang University Beijing 100191 People's Republic of China Key Laboratory of Spacecraft Design Optimization & Dynamic Simulation Technologies of Ministry of Education School of Space and Environment Beihang University Beijing 100191 People's Republic of China School of Materials Science and Engineering Beihang University Beijing 100191 People's Republic of China Science and Technology on Vacuum Technology and Physics Laboratory Lanzhou Institute of Physics Lanzhou 730000 People's Republic of China

This work presents the difficulties associated with the miniaturization of Hall Thruster engines and how state of the art materials and new manufacture techniques can potentially solve these problems. Hall Thrusters are electric propulsion systems that require specific magnetic field topography and uniform propellant distribution for optimal operation which is difficult to achieve with typical materials and by conventional manufacturing methods in miniaturized engines. To keep the optimal magnetic field distribution at small thruster sizes, it is shown that new alloys of SmCo permanent magnets can generate the desired magnetic field distribution and that their high-temperature resistance properties assure its operation temperature will be under the maximum operational temperature. In addition, whereas for the small dimensions required for the anode traditional manufacture methods only allow for simple designs, it is explained how the implementation of 3D-printing techniques can improve the uniformity in the azimuthal distribution of the propellant by allowing complex geometries in the design of the anode that are unattainable with traditional manufacturing.

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Overview of KAGRA : Data transfer and management

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Progress of Theoretical and Experimental Physics 2023年第10期2023卷

作者： Akutsu, T Ando, M Arai, K Arai, Y Araki, S Araya, A Aritomi, N Asada, H Aso, Y Bae, S Bae, Y Baiotti, L Bajpai, R Barton, M A Cannon, K Cao, Z Capocasa, E Chan, M Chen, C Chen, K Chen, Y Chiang, C-Y Chu, H Chu, Y-K Eguchi, S Enomoto, Y Flaminio, R Fujii, Y Fujikawa, Y Fukunaga, M Fukushima, M Gao, D Ge, G Ha, S Hagiwara, A Haino, S Han, W-B Hasegawa, K Hattori, K Hayakawa, H Hayama, K Himemoto, Y Hiranuma, Y Hirata, N Hirose, E Hong, Z Hsieh, B Huang, G-Z Huang, H-Y Huang, P Huang, Y-C Huang, Y Hui, D C Y Ide, S Ikenoue, B Imam, S Inayoshi, K Inoue, Y Ioka, K Ito, K Itoh, Y Izumi, K Jeon, C Jin, H-B Jung, K Jung, P Kaihotsu, K Kajita, T Kakizaki, M Kamiizumi, M Kanda, N Kang, G Kawaguchi, K Kawai, N Kawasaki, T Kim, C Kim, J Kim, J C Kim, W S Kim, Y-M Kimura, N Kita, N Kitazawa, H Kobayashi, Y Kojima, Y Kokeyama, K Komori, K Kong, A K H Kotake, K Kozakai, C Kozu, R Kumar, R Kume, J Kuo, C Kuo, H-S Kuromiya, Y Kuroyanagi, S Kusayanagi, K Kwak, K Lee, H K Lee, H W Lee, R Leonardi, M Li, K L Lin, L C-C Lin, C-Y Lin, F-K Lin, F-L Lin, H L Liu, G C Luo, L-W Majorana, E Marchio, M Michimura, Y Mio, N Miyakawa, O Miyamoto, A Miyazaki, Y Miyo, K Miyoki, S Mori, Y Morisaki, S Moriwaki, Y Nagano, K Nagano, S Nakamura, K Nakano, H Nakano, M Nakashima, R Nakayama, Y Narikawa, T Naticchioni, L Negishi, R Quynh, L Nguyen Ni, W-T Nishizawa, A Nozaki, S Obuchi, Y Ogaki, W Oh, J J Oh, K Oh, S H Ohashi, M Ohashi, T Ohishi, N Ohkawa, M Ohta, H Okutani, Y Okutomi, K Oohara, K Ooi, C Oshino, S Otabe, S Pan, K Pang, H Parisi, A Park, J Arellano, F E Peña Pinto, I Sago, N Saito, S Saito, Y Sakai, K Sakai, Y Sakuno, Y Sasaki, Y Sato, S Sato, T Sawada, T Sekiguchi, T Sekiguchi, Y Shao, L Shibagaki, S Shimizu, R Shimoda, T Shimode, K Shinkai, H Shishido, T Shoda, A Somiya, K Son, E J Sotani, H Sugimoto, R Suresh, J Suzuki, T Tagoshi, H Takahashi, H Takahashi, R Takamori, A Takano, S Takeda, H Takeda, M Tanaka, H Tanaka, K Tanaka, T Tanioka, S Martin, E N Tapia San Telada, S Tomaru, T Tomigami, Y Tomura, T Travasso, F Trozzo, L Tsang, T Ts Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Department of Physics The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan Research Center for the Early Universe (RESCEU) The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan Institute for Cosmic Ray Research (ICRR) KAGRA Observatory The University of Tokyo 5-1-5 Kashiwa-no-Ha Kashiwa City Chiba 277-8582 Japan Accelerator Laboratory High Energy Accelerator Research Organization (KEK) 1-1 Oho Tsukuba City Ibaraki 305-0801 Japan Earthquake Research Institute The University of Tokyo 1-1-1 Yayoi Bunkyo-ku Tokyo 113-0032 Japan Department of Mathematics and Physics Hirosaki University 3 Bunkyo-cho Hirosaki City Aomori 036-8561 Japan Kamioka Branch National Astronomical Observatory of Japan (NAOJ) 238 Higashi-Mozumi Kamioka-cho Hida City Gifu 506-1205 Japan The Graduate University for Advanced Studies (SOKENDAI) 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Korea Institute of Science and Technology Information (KISTI) 245 Daehak-ro Yuseong-gu Daejeon 34141 Korea National Institute for Mathematical Sciences 70 Yuseong-daero 1689 Beon-gil Yuseong-gu Daejeon 34047 Korea International College Osaka University 1-1 Machikaneyama-cho Toyonaka City Osaka 560-0043 Japan School of High Energy Accelerator Science The Graduate University for Advanced Studies (SOKENDAI) 1-1 Oho Tsukuba City Ibaraki 305-0801 Japan Department of Astronomy Beijing Normal University No. 19 Xinjiekou Street Beijing 100875 China Department of Applied Physics Fukuoka University 8-19-1 Nanakuma Jonan Fukuoka City Fukuoka 814-0180 Japan Department of Physics Tamkang University No. 151 Yingzhuan Rd. Danshui Dist. New Taipei City 25137 Taiwan Department of Physics and Institute of Astronomy Nation

KAGRA is a newly built gravitational wave observatory, a laser interferometer with a 3 km arm length, located in Kamioka, Gifu prefecture, Japan. In this article, we describe the KAGRA data management system, i.e., recording of data, transfer from the KAGRA experiment site to computing resources, as well as data distribution to tier sites, including international sites in Taiwan and Korea. The amount of KAGRA data exceeded 1.0 PiB and increased by about 1.5 TB per day during operation in 2020. Our system has succeeded in data management, and has achieved performance that can withstand observations after 2023, that is, a transfer rate of 20 MB s-1or more and file storage of sufficient capacity for petabyte class. We also discuss the sharing of data between the global gravitational-wave detector network with other experiments, namely LIGO and Virgo. The latency, which consists of calculation of calibrated strain data and transfer time within the global network, is very important from the view of multi-messenger astronomy using gravitational waves. Real-time calbrated data delivered from the KAGRA detector site and other detectors to our computing system arrive with about 4–15 seconds of latency. These latencies are sufficiently short compared to the time taken for gravitational wave event search computations. We also established a high-latency exchange of offline calibrated data that was aggregated with a better accuracy compared with real-time data.

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On the origin & thermal stability of Arrokoth’s and Pluto’s ices

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arXiv 2020年

作者： Lisse, Carey M. Young, L.A. Cruikshank, D.P. Sandford, S.A. Schmitt, B. Stern, S.A. Weaver, H.A. Umurhan, O. Pendleton, Y.J. Keane, J.T. Gladstone, G.R. Parker, J.M. Binzel, R.P. Earle, A.M. Horanyi, M. El-Maarry, M. Cheng, A.F. Moore, J.M. McKinnon, W.B. Grundy, W.M. Kavelaars, J.J. Linscott, I.R. Lyra, W. Lewis, B.L. Britt, D.T. Spencer, J.R. Olkin, C.B. McNutt, R.L. Elliott, H.A. Dello-Russo, N. Steckloff, J.K. Neveu, M. Mousis, O. Space Exploration Sector Johns Hopkins University Applied Physics Laboratory 11100 Johns Hopkins Rd LaurelMD20723 United States Southwest Research Institute BoulderCO80302 United States Astrophysics Branch Space Sciences Division NASA/Ames Research Center Moffett FieldCA94035 United States Université Grenoble Alpes CNRS CNES Institut de Planétologie et Astrophysique de Grenoble Grenoble France Solar System Exploration Research Virtual Institute NASA/Ames Research Center Moffett FieldCA94035 United States Astrophysics and Space Sciences Section Jet Propulsion Laboratory/Caltech PasadenaCA91109 United States Southwest Research Institute San AntonioTX28510 United States Dept. of Earth Atmospheric and Planetary Sciences Massachusetts Institute of Technology CambridgeMA02139 United States Laboratory for Atmospheric & Space Physics University of Colorado BoulderCO80303 United States Birkbeck University of London LondonWC12 7HX United Kingdom Department of Earth and Planetary Sciences and McDonnell Center for Space Sciences Washington University One Brookings Drive St. LouisMO63130 United States Lowell Observatory 1400 West Mars Hill Road FlagstaffAZ86001 United States NRC Herzberg Inst of Astrophysics 5071 W Saanich Road Victoria BCBCV9E 2E7 Canada Hansen Experimental Physics Laboratory Stanford University StanfordCA94305-9515 United States Dept. of Astronomy New Mexico State University PO BOX 30001 MSC 4500 Las CrucesNM88003-8001 United States Department of Astronomy Columbia University 550 W. 120th St. New YorkNY10027 United States Division of Astronomy and Astrophysics University of California Los Angeles 475 Portola Plaza Los AngelesCA90025 United States Department of Physics University of Central Florida OrlandoFL32816 United States Physics and Astronomy Department University of Texas at San Antonio San AntonioTX78249 United States Planetary Science Institute TucsonAZ85719 United States Department of Aerospace

In this paper we discuss in a thermodynamic, geologically empirical way the long-term nature of the stable majority ices that could be present in Kuiper Belt object (KBO) 2014 MU69 (also called Arrokoth;hereafter "MU69") after its 4.6 Gyr residence in the Edgeworth-Kuiper belt (EKB) as a cold classical object. We compare the upper bounds for the gas production rate (~1024 molecules/sec) measured by the New Horizons (NH) spacecraft flyby on 01 Jan 2019 to estimates for the outgassing flux rates from a suite of common cometary and KBO ices at the average ~40K sunlit surface temperature of MU69, but do not find the upper limit very constraining except for the most volatile of species (e.g. CO, N2, CH4). More constraining is the stability versus sublimation into vacuum requirement over Myr to Gyr, and from this we find only 3 common ices that are truly refractory: HCN, CH3OH, and H2O (in order of increasing stability), while NH3 and H2CO ices are marginally stable and may be removed by any positive temperature excursions in the EKB, as produced every 108 – 109 yrs by nearby supernovae and passing O/B stars. To date the NH team has reported the presence of abundant CH3OH and H2O on MU69’s surface (Stern et al. 2019, Grundy et al. 2020). NH3 has been searched for, but not found. We predict that future absorption feature detections, if any are ever derived from higher signal-to-noise ratio spectra, will be due to an HCN or poly-H2CO based species. Consideration of the conditions present in the EKB region during the formation era of MU69 lead us to state that it is highly likely that it "formed in the dark", in an optically thick mid-plane, unable to see the nascent, variable, highly luminous Young Stellar Object (YSO)/TTauri Sun, and that KBOs contain HCN and CH3OH ice phases in addition to the H2O ice phases found in their short period (SP) comet descendants. Finally, when we apply our ice thermal stability analysis to bodies/populations related to MU69, we find that meth

关键词： Signal to noise ratio

ACCESS & LRG-BEASTS: A precise new optical transmission spectrum of the ultrahot Jupiter WASP-103b

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arXiv 2021年

作者： Kirk, James Rackham, Benjamin V. MacDonald, Ryan J. López-Morales, Mercedes Espinoza, Néstor Lendl, Monika Wilson, Jamie Osip, David J. Wheatley, Peter J. Skillen, Ian Apai, Dániel Bixel, Alex Gibson, Neale P. Jordán, Andrés Lewis, Nikole K. Louden, Tom McGruder, Chima D. Nikolov, Nikolay Rodler, Florian Weaver, Ian C. Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Earth Atmospheric and Planetary Sciences Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Department of Astronomy Carl Sagan Institute Cornell University 122 Sciences Drive IthacaNY14853 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Observatoire de Genéve University of Geneva Chemin Pegasi 51 Sauverny1290 Switzerland Astrophysics Research Centre School of Mathematics and Physics Queens University Belfast BelfastBT7 1NN United Kingdom Las Campanas Observatory Carnegie Institution of Washington Colina el Pino Casilla 601 La Serena Chile Department of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Centre for Exoplanets and Habitability University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Isaac Newton Group of Telescopes Apartado de Correos 321 Santa Cruz de La PalmaE-38700 Spain Department of Astronomy/Steward Observatory The University of Arizona 933 N. Cherry Avenue TucsonAZ85721 United States Lunar and Planetary Laboratory The University of Arizona 1629 E. Univ. Blvd TucsonAZ85721 United States Earths in Other Solar Systems Team NASA Nexus for Exoplanet System Science School of Physics Trinity College Dublin The University of Dublin Dublin 2 Ireland Facultad de Ingeniería y Ciencias Universidad Adolfo Ibáñez Av. Diagonal las Torres 2640 Peñalolén Santiago Chile Millennium Institute for Astrophysics Santiago Chile European Southern Observatory Alonso de Cordova 3107 Vitacura Santiago de Chile Chile

We present a new ground-based optical transmission spectrum of the ultrahot Jupiter WASP-103b (Teq = 2484 K). Our transmission spectrum is the result of combining five new transits from the ACCESS survey and two new transits from the LRG-BEASTS survey with a reanalysis of three archival Gemini/GMOS transits and one VLT/FORS2 transit. Our combined 11-transit transmission spectrum covers a wavelength range of 3900-9450 Å with a median uncertainty in the transit depth of 148 parts-per-million, which is less than one atmospheric scale height of the planet. In our retrieval analysis of WASP-103b's combined optical and infrared transmission spectrum, we find strong evidence for unocculted bright regions (4.3σ) and weak evidence for H2O (1.9σ), HCN (1.7σ), and TiO (2.1σ), which could be responsible for WASP-103b's observed temperature inversion. Our optical transmission spectrum shows significant structure that is in excellent agreement with the extensively studied ultrahot Jupiter WASP-121b, for which the presence of VO has been inferred. For WASP-103b, we find that VO can only provide a reasonable fit to the data if its abundance is implausibly high and we do not account for stellar activity. Our results highlight the precision that can be achieved by ground-based observations and the impacts that stellar activity from F-type stars can have on the interpretation of exoplanet transmission spectra. © 2021, CC BY.

关键词： Stars

Preventive control for combined heat and power system: A day-ahead security constrained economic dispatch model

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Preventive control for combined heat and power system: A day...

The 11th IET International Conference on Advances in Power system Control, Operation and Management (APSCOM 2018)

作者： Qunli Lin Xinwei Shen Yinliang Xu Yong Sun Zhenyuan Li Qinglai Guo Hongbin Sun Shenzhen Environmental Science and New Energy Technology Engineering Laboratory Tsinghua-Berkeley Shenzhen Institute Tsinghua University Shenzhen China Jilin Power Grid Company State Grid Corp. of China Jilin China State Key Lab of Control and Simulation of Power System and Generation Equipments Department of Electrical Engineering Tsinghua University Beijing China

ISBN: (数字)9781839530043

Integrated Energy system (IES), which plays a vital role in the development of Energy Internet (EI), can improve the efficiency of energy utilization and integration of renewable energy. However, the coupling between multiple energy systems will bring new challenges to the security control of the IES, such as combined heat and power (CHP) system. For IES, the preventive control is the first line of defense to ensure that the system can keep stable operation when contingencies such as the transmission outage or generator outage happen. This paper proposes a preventive control approach for CHP system, in which a day-ahead security constrained economic dispatch (SCED) model of CHP system considering the coupling of heat and electric is formulated. The model aims to minimize the cost of the whole system, while the preventive control of the system can be achieved with the constraints considering the normal states and contingencies states. Case studies based on the IEEE 9-bus system with CHPs are presented to illustrate the approach. The case result shows that the combined electric and heat optimal dispatch is more economical than when two systems are independently optimized and operated. And the proposed preventive control approach of the CHP system can satisfy both the electric and heat demand, and system security is ensured when the N-1 contingencies happened.

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A case-based reasoning approach for task-driven spatial-temporally aware geospatial data discovery through geoportals

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International Journal of Digital Earth 2017年第11期10卷 1146-1165页

作者： Ming Li Wei Guo Lian Duan Xinyan Zhu Institute of Space Science and Technology Nanchang UniversityNanchangPeople’s Republic of China State Key Laboratory of Information Engineering in Surveying Mapping and Remote SensingWuhan UniversityWuhanPeople’s Republic of China Collaborative Innovation Center of Geospatial Technology WuhanPeople’s Republic of China Key Laboratory of Environment Change and Resources Use in Beibu Gulf(Guangxi Teachers Education University) Ministry of EducationGuangxiPeople’s Republic of China Guangxi Key Laboratory of Earth Surface Processes and Intelligent Simulation(Guangxi Teachers Education University) GuangxiPeople’s Republic of China

There is a critical need to develop a means for fast,task-driven discovery of geospatial data found in *** geoportals,however,only provide metadata-based means for discovery,with little support for task-driven discovery,especially when considering spatial–temporal *** address this gap,this paper presents a Case-Based Reasoning-supported Geospatial Data Discovery(CBR-GDD)method and implementation that accesses geospatial data by *** advantages of the CBR-GDD approach is that it builds an analogue reasoning process that provides an internal mechanism bridging tasks and geospatial data with spatial–temporal awareness,thus providing solutions based on past *** CBR-GDD approach includes a set of algorithms that were successfully implemented via three components as an extension of geoportals:ontology-enhanced knowledge base,similarity assessment model,and case retrieval nets.A set of experiments and case studies validate the CBR-GDD approach and application,and demonstrate its efficiency.

关键词： Case-based reasoning geospatial data discovery ontology geoportals spatial–temporal awareness

First study of the two-body scattering involving charm hadrons

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Physical Review D 2022年第5期106卷 052010-052010页

作者： S. Acharya D. Adamová A. Adler J. Adolfsson G. Aglieri Rinella M. Agnello N. Agrawal Z. Ahammed S. Ahmad S. U. Ahn I. Ahuja Z. Akbar A. Akindinov M. Al-Turany S. N. Alam 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 D. Andreou 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 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 I. Belikov A. D. C. Bell Hechavarria F. Bellini 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 P. Bhattacharya L. Bianchi N. Bianchi J. Bielčík J. Bielčíková J. Biernat A. Bilandzic G. Biro S. Biswas J. T. Blair D. Blau M. B. Blidaru C. Blume G. Boca F. Bock 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 E. A. R. Casula 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 S. Cho P. Chochula P. Christakoglou C. H. Christensen P. Christiansen T. Università degli Studi di Foggia Foggia Italy Nuclear Physics Group STFC Daresbury Laboratory Daresbury United Kingdom Jeonbuk National University Jeonju Republic of Korea Lawrence Berkeley National Laboratory Berkeley California USA 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 Joint Institute for Nuclear Research (JINR) Dubna Russia Faculty of Science P.J. Šafárik University Košice Slovakia Indonesian Institute of Sciences Jakarta Indonesia NRC Kurchatov Institute IHEP Protvino Russia Politecnico di Bari and Sezione INFN Bari Italy National Nuclear Research Center Baku Azerbaijan INFN Sezione di Torino Turin Italy Central China Normal University Wuhan China Instituto de Física Universidade Federal do Rio Grande do Sul (UFRGS) Porto Alegre Brazil COMSATS University Islamabad Islamabad Pakistan Dipartimento di Fisica e Astronomia dell’Università and Sezione INFN Bologna Italy Universidade Federal do ABC Santo Andre Brazil Department of Physics and Technology University of Bergen Bergen Norway INFN Sezione di Cagliari Cagliari Italy Institute of Space Science (ISS) Bucharest Romania School of Physics and Astronomy University of Birmingham Birmingham United Kingdom Horia Hulubei National Institute of Physics and Nuclear Engineering Bucharest Romania Niels Bohr Institute University of Copenhagen Copenhagen Denmark Warsaw University of Technology Warsaw Poland Physikalisches Institut Eberhard-Karls-Universität Tübingen Tübingen Germany INFN Sezione di Padova Padova Italy Laboratoire de Physique Subatomique et de Cosmologie Université Grenoble-Alpes CNRS-IN2P3 Grenoble France St. Petersburg State University St. Petersburg Russia Department of Physics University of Oslo Oslo Norway Westfälische Wilhelms-Universität Münster Institut für Kernphysik Münster

This article presents the first measurement of the interaction between charm hadrons and nucleons. The two-particle momentum correlations of pD− and p¯D+ pairs are measured by the ALICE Collaboration in high-multiplicity pp collisions at s=13 TeV. The data are compatible with the Coulomb-only interaction hypothesis within (1.1–1.5)σ. The level of agreement slightly improves if an attractive nucleon (N)D¯ strong interaction is considered, in contrast to most model predictions which suggest an overall repulsive interaction. This measurement allows for the first time an estimation of the 68% confidence level interval for the isospin I=0 inverse scattering length of the ND¯ state f0,I=0−1∈[−0.4,0.9] fm−1, assuming negligible interaction for the isospin I=1 channel.

关键词： Hadron colliders