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arXiv 2024年

作者： Henderson, Beth A. Casewell, Sarah L. Jordán, Andrés Brahm, Rafael Henning, Thomas Gill, Samuel Mayorga, L.C. Ziegler, Carl Stassun, Keivan G. Goad, Michael R. Acton, Jack Alves, Douglas R. Anderson, David R. Apergis, Ioannis Armstrong, David J. Bayliss, Daniel Burleigh, Matthew R. Dragomir, Diana Gillen, Edward Günther, Maximilian N. Hedges, Christina Hesse, Katharine M. Hobson, Melissa J. Jenkins, James S. Jenkins, Jon M. Kendall, Alicia Lendl, Monika Lund, Michael B. McCormac, James Moyano, Maximiliano Osborn, Ares Pinto, Marcelo Tala Ramsay, Gavin Rapetti, David Saha, Suman Seager, Sara Trifonov, Trifon Udry, Stéphane Vines, Jose I. West, Richard G. Wheatley, Peter J. Winn, Joshua N. Zivave, Tafadzwa School of Physics and Astronomy University of Leicester University Road LeicesterLE1 7RH United Kingdom Facultad de Ingeniería y Ciencias Universidad Adolfo Ibáñez Av. Diagonal las Torres Peñalolén Santiago2640 Chile Millennium Institute of Astrophysics Santiago Chile Data Observatory Foundation Chile Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany Centre for Exoplanets and Habitability University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Dept. of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom The Johns Hopkins University Applied Physics Laboratory 11100 Johns Hopkins Rd LaurelMD20723 United States Department of Physics Engineering and Astronomy Stephen F. Austin State University 1936 North St NacogdochesTX75962 United States Department of Physics and Astronomy Vanderbilt University NashvilleTN37235 United States Departamento de Astronomía Universidad de Chile Casilla 36-D Santiago Chile Instituto de Astronomía Universidad Católica del Norte Angamos 0610 Antofagasta1270709 Chile Department of Physics and Astronomy University of New Mexico 210 Yale Blvd NE AlbuquerqueNM87106 United States Astronomy Unit Queen Mary University of London Mile End Road LondonE1 4NS United Kingdom Keplerlaan 1 Noordwijk2201 AZ Netherlands NASA Goddard Space Flight Center 8800 Greenbelt Rd GreenbeltMD20771 United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Instituto de Estudios Astrofísicos Universidad Diego Portales Av. Ejército 441 Santiago Chile Casilla 36-D Santiago Chile NASA Ames Research Center Moffett FieldCA94035 United States Observatoire de Genève Université de Genève Chemin Pegasi 51 Versoix1290 Switzerland NASA Exoplanet Science Institute IPAC California Institute of Technology PasadenaCA91125 United States Armagh Observatory and Planetarium Col

We report the discovery of the most eccentric transiting brown dwarf in the brown dwarf desert, TOI-2490b. The brown dwarf desert is the lack of brown dwarfs around main sequence stars within ∼ 3 AU and is thought to be caused by differences in formation mechanisms between a star and planet. To date, only ∼ 40 transiting brown dwarfs have been confirmed. TOI-2490b is a (Equation presented) brown dwarf orbiting a (Equation presented) sun-like star on a 60.33 d orbit with an eccentricity of 0.77989 ± 0.00049. The discovery was detected within TESS sectors 5 (30 minute cadence) and 32 (2 minute and 20 second cadence). It was then confirmed with 31 radial velocity measurements with FEROS by the WINE collaboration and photometric observations with the Next Generation Transit Survey. Stellar modelling of the host star estimates an age of ∼ 8 Gyr, which is supported by estimations from kinematics likely placing the object within the thin disc. However, this is not consistent with model brown dwarf isochrones for the system age suggesting an inflated radius. Only one other transiting brown dwarf with an eccentricity higher than 0.6 is currently known in the brown dwarf desert. Demographic studies of brown dwarfs suggestedAuthors such high eccentricity is indicative of stellar formation mechanisms. Copyright © 2024, The Authors. All rights reserved.

关键词： Stars

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Personalized radiotherapy design for glioblastoma: Integrating mathematical tumor models, multimodal scans and Bayesian inference

arXiv

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arXiv 2018年

作者： Lipková, Jana Angelikopoulos, Panagiotis Wu, Stephen Alberts, Esther Wiestler, Benedikt Diehl, Christian Preibisch, Christine Pyka, Thomas Combs, Stephanie Hadjidoukas, Panagiotis van Leemput, Koen Koumoutsakos, Petros Lowengrub, John Menze, Bjoern Germany Dept. of Neuroradiolog Klinikum Rechts der Isar TUM Germany D.E. Shaw Research L.L.C United States Institute of Statistical Mathematics Tokyo Japan Dept. of Diagnostic and Interventional Neuroradiology & Neuroimaging Center & Clinic for Neurology Klinikum Rechts der Isar TUM Germany Dept. of Nuclear Medicine Klinikum Rechts der Isar TUM Germany Dept. of Radiation Oncology Klinikum Rechts der Isar TUM Institute of Innovative Radiotherapy Helmholtz Zentrum Munich & Deutsches Konsortium für Translationale Krebsforschung Germany IBM Research - Zurich Switzerland Harvard Medical School Boston United States Dept. of Applied Mathematics and Computer Science TU Denmark Denmark Computational Science and Engineering Lab ETH Zürich Switzerland Dept. of Mathematics Biomedical Engineering Chemical Engineering and Materials Science Center for Complex Biological Systems Chao Family Comprehensive Cancer Center UC Irvine United States Institute for Advanced Study TUM Germany

Glioblastoma is a highly invasive brain tumor, whose cells infiltrate surrounding normal brain tissue beyond the lesion outlines visible in the current medical scans. These infiltrative cells are treated mainly by radiotherapy. Existing radiotherapy plans for brain tumors derive from population studies and scarcely account for patient-specific conditions. Here we provide a Bayesian machine learning framework for the rational design of improved, personalized radiotherapy plans using mathematical modeling and patient multimodal medical scans. Our method, for the first time, integrates complementary information from high resolution MRI scans and highly specific FET-PET metabolic maps to infer tumor cell density in glioblastoma patients. The Bayesian framework quantifies imaging and modeling uncertainties and predicts patient-specific tumor cell density with credible intervals. The proposed methodology relies only on data acquired at a single time point and thus is applicable to standard clinical settings. An initial clinical population study shows that the radiotherapy plans generated from the inferred tumor cell infiltration maps spare more healthy tissue thereby reducing radiation toxicity while yielding comparable accuracy with standard radiotherapy protocols. Moreover, the inferred regions of high tumor cell densities coincide with the tumor radioresistant areas, providing guidance for personalized dose-escalation. The proposed integration of multimodal scans and mathematical modeling provides a robust, non-invasive tool to assist personalized radiotherapy design. Copyright © 2018, The Authors. All rights reserved.

关键词： Radiotherapy

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Recovery of Compactly Supported Functions from Spectrogram Measurements via Lifting

Recovery of Compactly Supported Functions from Spectrogram M...

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International Conference on Sampling Theory and Applications

作者： Sami Merhi Aditya Viswanathan Mark Iwen Department of Mathematics Michigan State University Dept. of Mathematics and Dept. of Computational Mathematics Science and Engineering (CMSE) Michigan State University

ISBN: (纸本)9781538615669

A novel phase retrieval method, motivated by pty-chographic imaging, is proposed for the approximate recovery of a compactly supported specimen function f : R → C from its continuous short time Fourier transform (STFT) spectrogram measurements. The method, partially inspired by the well known Phase Lift [1] algorithm, is based on a lifted formulation of the infinite dimensional problem which is then later truncated for the sake of computation. Numerical experiments demonstrate the promise of the proposed approach.

关键词： lift STFT Spectrogram Sake lifts one-dimensional problem phase method

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Spinning up a Daze: TESS Uncovers a Hot Jupiter orbiting the Rapid-Rotator TOI-778

arXiv

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arXiv 2022年

作者： Clark, Jake T. Addison, Brett C. Okumura, Jack Vach, Sydney Errico, Adriana Heitzmann, Alexis Rodriguez, Joseph E. Wright, Duncan J. Clerté, Mathieu Brown, Carolyn J. Fetherolf, Tara Wittenmyer, Robert A. Plavchan, Peter Kane, Stephen R. Horner, Jonathan Kielkopf, John F. Shporer, Avi Tinney, C.G. Hui-Gen, Liu Ballard, Sarah Bowler, Brendan P. Mengel, Matthew W. Zhou, George Lee, Annette S. David, Avelyn Heim, Jessica Lee, Michele E. Sevilla, Verónica Zafar, Naqsh E. Hinkel, Natalie R. Allen, Bridgette E. Bayliss, Daniel Berberyan, Arthur Berlind, Perry Bieryla, Allyson Bouchy, François Brahm, Rafael Bryant, Edward M. Christiansen, Jessie L. Ciardi, David R. Ciardi, Krys N. Collins, Karen A. Dallant, Jules Davis, Allen B. Díaz, Matías R. Dressing, Courtney D. Esquerdo, Gilbert A. Harre, Jan-Vincent Howell, Steve B. Jenkins, Jon M. Jensen, Eric L.N. Jones, Matías I. Jordán, Andrés Latham, David W. Lund, Michael B. McCormac, James Nielsen, Louise D. Otegi, Jon Quinn, Samuel N. Radford, Don J. Ricker, George R. Schwarz, Richard P. Seager, Sara Smith, Alexis M.S. Stockdale, Chris Tan, Thiam-Guan Udry, Stéphane Vanderspek, Roland Günther, Maximilian N. Wang, Songhu Wingham, Geof Winn, Joshua N. University of Southern Queensland Centre for Astrophysics USQ Toowoomba West Street QLD4350 Australia Swinburne University of Technology Centre for Astrophysics and Supercomputing John Street HawthornVIC3122 Australia Center for Astrophysics Harvard & Smithsonian 60 Garden St CambridgeMA02138 United States Astronomy Unit Queen Mary University of London Mile End Road LondonE1 4NS United Kingdom Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Earth and Planetary Sciences University of California Riverside 900 University Avenue RiversideCA92521 United States Department of Physics & Astronomy George Mason University 4400 University Drive MS 3F3 FairfaxVA22030 United States Department of Earth and Planetary Sciences University of California RiversideCA92521 United States Department of Physics and Astronomy University of Louisville LouisvilleKY40292 United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Exoplanetary Science UNSW School of Physics UNSW Sydney NSW2052 Australia School of Astronomy and Space Science Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education Nanjing University Jiangsu Nanjing210046 China Department of Astronomy University of Florida 211 Bryant Space Science Center GainesvilleFL32611 United States Department of Astronomy The University of Texas AustinTX78712 United States The Native Skywatchers Initiative MN United States Department of Physics and Astronomy St. Cloud University MN United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Jeremiah Horrocks Institute University of Central Lancashire PrestonPR1 2HE United Kingdom Space Science and Engineering Division Southwest Research Institute San AntonioTX78238 United States NASA Exoplanet Science Institute - Ca

NASA’s Transiting Exoplanet Survey Satellite (TESS) mission, has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating (v sin (i) = 35.1 ± 1.0 km s−1) early F3V-dwarf, HD 115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS’s initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva-Australis, TRES, CORALIE and CHIRON to confirm and characterise TOI-778 b. A joint analysis of the light curves and the radial velocity measurements yield a mass, radius, and orbital period for TOI-778 b of 2.76+0−0.2423 MJ, 1.370 ± 0.043 RJ, and ∼ 4.63 days, respectively. The planet orbits a bright (V = 9.1 mag) F3-dwarf with M = 1.40 ± 0.05 M, R = 1.70 ± 0.05 R, and log g = 4.05 ± 0.17. We observed a spectroscopic transit of TOI-778 b, which allowed us to derive a sky-projected spin-orbit angle of 18◦ ± 11◦, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller aperture telescopes such as Minerva-Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars. © 2022, CC BY.

关键词： Satellites

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SN 2022acko: the First Early Far-Ultraviolet Spectra of a Type IIP Supernova

arXiv

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arXiv 2023年

作者： Bostroem, K. Azalee Dessart, Luc Hillier, D. John Lundquist, Michael Andrews, Jennifer E. Sand, David J. Dong, Yize Valenti, Stefano Haislip, Joshua Hoang, Emily T. Hosseinzadeh, Griffin Janzen, Daryl Jencson, Jacob E. Jha, Saurabh W. Kouprianov, Vladimir Pearson, Jeniveve Meza Retamal, Nicolas E. Reichart, Daniel E. Shrestha, Manisha Ashall, Christopher Baron, E. Brown, Peter J. DerKacy, James M. Farah, Joseph Galbany, Lluís Hernández, J.I. González Green, Elizabeth Hoeflich, Peter Howell, D. Andrew Kwok, Lindsey A. McCully, Curtis Müller-Bravo, Tomás E. Newsome, Megan Gonzalez, Estefania Padilla Pellegrino, Craig Rho, Jeonghee Rowe, Micalyn Schwab, Michaela Shahbandeh, Melissa Smith, Nathan Strader, Jay Terreran, Giacomo Van Dyk, Schuyler D. Wyatt, Samuel Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States Institut d’Astrophysique de Paris CNRS-Sorbonne Université 98 bis boulevard Arago Paris75014 France University of Pittsburgh 3941 O’Hara Street PittsburghPA15260 United States W. M. Keck Observatory 65-1120 Māmalahoa Highway KamuelaHI96743-8431 United States Gemini Observatory 670 North A‘ohoku Place HiloHI96720-2700 United States Department of Physics and Astronomy University of California Davis 1 Shields Avenue DavisCA95616-5270 United States Department of Physics and Astronomy University of North Carolina 120 East Cameron Avenue Chapel HillNC27599 United States Department of Physics and Engineering Physics University of Saskatchewan 116 Science Place SaskatoonSKS7N 5E2 Canada Department of Physics and Astronomy The Johns Hopkins University 3400 North Charles Street BaltimoreMD21218 United States Department of Physics and Astronomy Rutgers the State University of New Jersey 136 Frelinghuysen Road PiscatawayNJ08854-8019 United States Department of Physics Virginia Tech BlacksburgVA24061 United States Planetary Science Institute 1700 East Fort Lowell Suite 106 TucsonAZ85719-2395 United States Hamburger Sternwarte Gojenbergsweg 112 HamburgD-21029 Germany Homer L. Dodge Department of Physics and Astronomy University of Oklahoma 440 W. Brooks Rm 100 NormanOK73019-2061 United States Department of Physics and Astronomy Texas A&M University 4242 TAMU College StationTX77843 United States Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain Institut d’Estudis Espacials de Catalunya Gran Capità 2-4 Edifici Nexus Desp. 201 BarcelonaE-08034 Spain Instituto de Astrofísica de Canarias La Laguna TenerifeE-38205 Spain Universidad de La Lag

We present five far- and near-ultraviolet spectra of the Type II plateau supernova, SN 2022acko, obtained 5, 6, 7, 19, and 21 days after explosion, all observed with the Hubble Space Telescope/Space Telescope Imaging Spectrograph. The first three epochs are earlier than any Type II plateau supernova has been observed in the far-ultraviolet revealing unprecedented characteristics. These three spectra are dominated by strong lines, primarily from metals, which contrasts with the featureless early optical spectra. The flux decreases over the initial time series as the ejecta cool and line-blanketing takes effect. We model this unique dataset with the non-local thermodynamic equilibrium radiation transport code CMFGEN, finding a good match to the explosion of a low-mass red supergiant with energy Ekin = 6 × 1050 erg. With these models we identify, for the first time, the ions that dominate the early ultraviolet spectra. We present optical photometry and spectroscopy, showing that SN 2022acko has a peak absolute magnitude of V = −15.4 mag and plateau length of ∼ 115d. The spectra closely resemble those of SN 2005cs and SN 2012A. Using the combined optical and ultraviolet spectra, we report the fraction of flux as a function of bluest wavelength on days 5, 7, and 19. We create a spectral time-series of Type II supernovae in the ultraviolet, demonstrating the rapid decline of flux over the first few weeks of evolution. Future observations of Type II supernovae are required to map out the landscape of exploding red supergiants, with and without circumstellar material, which is best revealed in high-quality ultraviolet spectra. © 2023, CC BY.

关键词： Supernovae

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MAGIC and H.E.S.S. detect VHE gamma rays from the blazar OT 081 for the first time: a deep multiwavelength study 37

MAGIC and H.E.S.S. detect VHE gamma rays from the blazar OT ...

引用

37th International Cosmic Ray Conference, ICRC 2021

作者： Seglar-Arroyo, M. Sanchez, D. Esteban Gutierrez, A. Agudo, I. Ciprini, S. Filippenko, A.V. Hovatta, T. Jermak, H. Kopatskaya, E.N. Lähteenmäki, A. Larionov, V.M. Larionova, L.V. Morozova, D.A. Pahljina, M. Tornikoski, M. Troitsky, I. Verrecchia, F. Xiao, H.B. Zheng, W. Acciari, V.A. Ansoldi, S. Antonelli, L.A. Arbet Engels, A. Artero, M. Asano, K. Baack, D. Babić, A. Baquero, A. Barres de Almeida, U. Barrio, J.A. Batković, I. Becerra González, J. Bednarek, W. Bellizzi, L. Bernardini, E. Bernardos, M. Berti, A. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Biland, A. Blanch, O. Bökenkamp, H. Bonnoli, G. Bošnjak, Ž. Busetto, G. Carosi, R. Ceribella, G. Cerruti, M. Chai, Y. Chilingarian, A. Cikota, S. Colak, S.M. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. D'Amico, G. D'Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. Delfino, M. Delgado, J. Delgado Mendez, C. Depaoli, D. Di Pierro, F. Di Venere, L. Do Souto Espiñeira, E. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsaesser, D. Fallah Ramazani, V. Fattorini, A. Fonseca, M.V. Font, L. Fruck, C. Fukami, S. Fukazawa, Y. García López, R.J. Garczarczyk, M. Gasparyan, S. Gaug, M. Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Green, J.G. Green, D. Hadasch, D. Hahn, A. Heckmann, L. Herrera, J. Hoang, J. Hrupec, D. Hütten, M. Inada, T. Ishio, K. Iwamura, Y. Jiménez Martínez, I. Jormanainen, J. Jouvin, L. Karjalainen, M. Kerszberg, D. Kobayashi, Y. Kubo, H. Kushida, J. Lamastra, A. Lelas, D. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, A. Loporchio, S. Machado de Oliveira Fraga, B. Maggio, C. Majumdar, P. Makariev, M. Mallamaci, M. Maneva, G. Manganaro, M. Mannheim, K. Maraschi, L. Mariotti, M. Martínez, M. Mazin, D. Menchiari, S. Mender, S. Mićanović, S. Miceli, D. Miener, T. Miranda, J.M. Mirzoyan, R. Molina, E. Moralejo, A. Morcuende, D. Moreno, V. Moretti, E. Nakamori, T. Nava, L. Neustroev, V. University of Rijeka Department of Physics Radmile Matejčić 2 Rijeka Croatia IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France CNRS LAPP France CSIC Granada Spain Roma Tor Vergata Section RomeI-00133 Italy ASI Space Science Data Center RomeI-00133 Italy Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Aalto University Tuorla observatory Finland Liverpool John Moores University United Kingdom St. Petersburg State University Russia Aalto University Finland INAF Osservatorio Astronomico di Roma via Frascati 33 Monte Porzio CatoneI-00078 Italy Guangzhou University China Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain Università di Udine INFN Trieste UdineI-33100 Italy RomeI-00136 Italy ETH Zürich ZürichCH-8093 Switzerland E-08193 Spain The University of Tokyo Chiba Kashiwa277-8582 Japan Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil Università di Padova INFN PadovaI-35131 Italy University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Università di Siena INFN Pisa SienaI-53100 Italy ZeuthenD-15738 Germany Max-Planck-Institut für Physik MünchenD-80805 Germany Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Armenian MAGIC Group A. Alikhanyan National Science Laboratory Yerevan0036 Armenia Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain INFN MAGIC Group INFN Sezione di Torino Università d

OT 081 is a luminous blazar well known for its variability in many energy bands. The very-high-energy (VHE;E > 100 GeV) gamma-ray emission from the source was discovered by MAGIC and H.E.S.S. during flaring activity in July 2016, after a trigger from the Large Area Telescope (LAT) onboard the Fermi satellite. By analysing the multiwavelength light curves and the broadband spectral energy distribution (SED), we study the activity of the source and investigate four individual states of activity in the window from MJD 57575 to 57602. The intrinsic gamma-ray spectrum can be described by a power law with spectral indices of 3.27 ± 0.44 (MAGIC) and 3.39 ± 0.58 (H.E.S.S.) over energy ranges 60-300 GeV and 120-500 GeV, respectively. The combined contemporaneous high-energy (HE;E > 100 MeV) through VHE SED shows curvature and can be described by a log-parabola shape. A simple one-zone synchrotron self-Compton (SSC) model is not sufficient to describe the broadband SED. The presence of broad emission lines in the optical spectrum of the source challenges the categorisation of OT 081 as a BL Lac and, together with the emission scenarios tested, points to the possibility that the source is transitional in nature between a BL Lac and a flat-spectrum radio quasar. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Germanium alloys

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The PLATO mission

引用

Experimental Astronomy 2025年第3期59卷 1-111页

作者： Rauer, Heike Aerts, Conny Cabrera, Juan Deleuil, Magali Erikson, Anders Gizon, Laurent Goupil, Mariejo Heras, Ana Walloschek, Thomas Lorenzo-Alvarez, Jose Marliani, Filippo Martin-Garcia, César Mas-Hesse, J. Miguel O’Rourke, Laurence Osborn, Hugh Pagano, Isabella Piotto, Giampaolo Pollacco, Don Ragazzoni, Roberto Ramsay, Gavin Udry, Stéphane Appourchaux, Thierry Benz, Willy Brandeker, Alexis Güdel, Manuel Janot-Pacheco, Eduardo Kabath, Petr Kjeldsen, Hans Min, Michiel Santos, Nuno Smith, Alexis Suarez, Juan-Carlos Werner, Stephanie C. Aboudan, Alessio Abreu, Manuel Acuña, Lorena Adams, Moritz Adibekyan, Vardan Affer, Laura Agneray, François Agnor, Craig Aguirre Børsen-Koch, Victor Ahmed, Saad Aigrain, Suzanne Al-Bahlawan, Ashraf Alcacera Gil, Ma de los Angeles Alei, Eleonora Alencar, Silvia Alexander, Richard Alfonso-Garzón, Julia Alibert, Yann Allende Prieto, Carlos Almeida, Leonardo Alonso Sobrino, Roi Altavilla, Giuseppe Althaus, Christian Alvarez Trujillo, Luis Alonso Amarsi, Anish Ammler-von Eiff, Matthias Amôres, Eduardo Andrade, Laerte Antoniadis-Karnavas, Alexandros António, Carlos Aparicio del Moral, Beatriz Appolloni, Matteo Arena, Claudio Armstrong, David Aroca Aliaga, Jose Asplund, Martin Audenaert, Jeroen Auricchio, Natalia Avelino, Pedro Baeke, Ann Baillié, Kevin Balado, Ana Ballber Balagueró, Pau Balestra, Andrea Ball, Warrick Ballans, Herve Ballot, Jerome Barban, Caroline Barbary, Gaële Barbieri, Mauro Barceló Forteza, Sebastià Barker, Adrian Barklem, Paul Barnes, Sydney Barrado Navascues, David Barragan, Oscar Baruteau, Clément Basu, Sarbani Baudin, Frederic Baumeister, Philipp Bayliss, Daniel Bazot, Michael Beck, Paul G. Belkacem, Kevin Bellinger, Earl Benatti, Serena Benomar, Othman Bérard, Diane Bergemann, Maria Bergomi, Maria Bernardo, Pierre Biazzo, Katia Bignamini, Andrea Bigot, Lionel Billot, Nicolas Binet, Martin Biondi, David Biondi, Federico Birch, Aaron C. Bitsch, Bertram Bluhm Ceballos, Paz Victoria Bódi, Attila Bognár, Zsófia Boisse, Isabelle Bolmont, Emeline Bonanno, Alfio Bonavita, Institut für Planetenforschung Deutsches Zentrum für Luft- und Raumfahrt DLR Rutherfordstrasse 2 Berlin 12489 Germany Fachbereich Geowissenschaften Institut für Geologische Freie Universität Berlin Malteserstr. 74-100 Berlin 12249 Germany Institute of Astronomy KU Leuven Leuven Belgium CNRS CNES LAM Aix Marseille University Marseille France Max Planck Institute for Solar System Research Göttingen Germany LESIA Paris Observatory PSL University Sorbonne University Paris Cité University CNRS Meudon France ESTEC European Space Agency Noordwijk Netherlands ESAC European Space Agency Madrid Spain Centro de Astrobiología CSIC-INTA Campus ESAC Madrid Spain Center for Space and Habitability University of Bern Bern Switzerland INAF - Osservatorio Astrofisico di Catania Catania Italy Department of Physics and Astronomy University of Padua Padua Italy Department of Physics University of Warwick Coventry United Kingdom Astronomical Observatory of Padova INAF - Italian National Institute for Astrophysics Padua Italy Armagh Observatory and Planetarium College Hill Armagh United Kingdom Geneve Observatory University of Geneve Geneve Switzerland IAS University of Paris-Saclay Orsay France AlbaNove University Centre Stockholm University Stockholm Sweden Department of Astrophysics University of Vienna Vienna Austria Department of Astronomy University of Sao Paulo Sao Paulo Brazil Astronomical Institute of the Czech Academy of Sciences Ondřejov Czech Republic Department of Physics and Astronomy Aarhus University Aarhus Denmark Institute for Space Research SRON Leiden Netherlands Instituto de Astrofísica e Ciências do Espaço CAUP Universidade do Porto Porto Portugal Departamento de Física e Astronomia Faculdade da Ci ncias Universidade do Porto Porto Portugal Mullard Space Science Laboratory University College London Holmbury Saint Mary United Kingdom Dept. Theoretical Physics and the Cosmos University of Granada Granada Spain Centre for Plan

PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2REarth) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases. © The Author(s) 2025.

关键词： Asteroseismology Exoplanets PLATO mission

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Follow-up observations of GW170817 with the MAGIC telescopes 37

Follow-up observations of GW170817 with the MAGIC telescopes

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37th International Cosmic Ray Conference, ICRC 2021

作者： Stamerra, A. Salafia, O.S. Berti, A. Covino, S. D'Elia, V. Miceli, D. Nava, L. Patricelli, B. Righi, C. Inoue, S. Antonelli, L.A. Ansoldi, S. De Lotto, B. Longo, F. Tavecchio, F. Acciari, V.A. Arbet Engels, A. Artero, M. Asano, K. Baack, D. Babić, A. Baquero, A. Barres de Almeida, U. Barrio, J.A. Batković, I. Becerra González, J. Bednarek, W. Bellizzi, L. Bernardini, E. Bernardos, M. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Biland, A. Blanch, O. Bökenkamp, H. Bonnoli, G. Bošnjak, Ž. Busetto, G. Carosi, R. Ceribella, G. Cerruti, M. Chai, Y. Chilingarian, A. Cikota, S. Colak, S.M. Colombo, E. Contreras, J.L. Cortina, J. D'Amico, G. Da Vela, P. Dazzi, F. De Angelis, A. Delfino, M. Delgado, J. Delgado Mendez, C. Depaoli, D. Di Pierro, F. Di Venere, L. Do Souto Espiñeira, E. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsaesser, D. Fallah Ramazani, V. Fattorini, A. Fonseca, M.V. Font, L. Fruck, C. Fukami, S. Fukazawa, Y. García López, R.J. Garczarczyk, M. Gasparyan, S. Gaug, M. Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Green, J.G. Green, D. Hadasch, D. Hahn, A. Heckmann, L. Herrera, J. Hoang, J. Hrupec, D. Hütten, M. Inada, T. Ishio, K. Iwamura, Y. Jiménez Martínez, I. Jormanainen, J. Jouvin, L. Karjalainen, M. Kerszberg, D. Kobayashi, Y. Kubo, H. Kushida, J. Lamastra, A. Lelas, D. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. López-Coto, R. López-Moya, M. López-Oramas, A. Loporchio, S. Machado de Oliveira Fraga, B. Maggio, C. Majumdar, P. Makariev, M. Mallamaci, M. Maneva, G. Manganaro, M. Mannheim, K. Maraschi, L. Mariotti, M. Martínez, M. Mazin, D. Menchiari, S. Mender, S. Mićanović, S. Miener, T. Miranda, J.M. Mirzoyan, R. Molina, E. Moralejo, A. Morcuende, D. Moreno, V. Moretti, E. Nakamori, T. Neustroev, V. Nigro, C. Nilsson, K. Nishijima, K. Noda, K. Nozaki, S. Ohtani, Y. Oka, T. Otero-Santos, J. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J.M. INAF - Osservatorio Astronomico di Roma Rome Italy INAF - Osservatorio Astronomico di Brera Merate Italy Rome Italy Max-Planck-Institut für Physik München Germany Space Science Data Center - Agenzia Spaziale Italiana Rome Italy European Gravitational Observatory Pisa Italy RIKEN Saitama Wako Japan Università di Udine INFN Trieste Udine Italy Dipartimento di Fisica Università di Trieste Trieste Italy Scuola Normale Superiore Pisa Italy Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain Università di Udine INFN Trieste UdineI-33100 Italy RomeI-00136 Italy ETH Zürich ZürichCH-8093 Switzerland E-08193 Spain The University of Tokyo Chiba Kashiwa277-8582 Japan Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil Università di Padova INFN PadovaI-35131 Italy University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Università di Siena INFN Pisa SienaI-53100 Italy ZeuthenD-15738 Germany Max-Planck-Institut für Physik MünchenD-80805 Germany Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Armenian MAGIC Group A. Alikhanyan National Science Laboratory Yerevan0036 Armenia Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica Università e del Politecnico di Bari BariI-70125 Italy Croatian MAGIC Group University of Rijeka Department of Physics Rijeka51000 Croatia Universität Würzburg WürzburgD-

The discovery of the electromagnetic counterpart AT2017gfo and the GRB 170817A, associated to the binary neutron star merger GW170817, was one of the major advances in the study of gamma-ray bursts (GRBs) and the hallmark of the multi-messenger astronomy with gravitational waves. Another breakthrough in GRB physics is represented by the discovery of the highly energetic, teraelectronvolt (TeV) component in the GRB 190114C, possibly an universal component in all GRBs. This conclusion is also suggested by the hint of TeV emission in the short GRB 160821B and a few more events reported in the literature. The missing observational piece is the joint detection of TeV emission and gravitational waves from a short GRB and its progenitor. MAGIC observed the counterpart AT2017gfo as soon as the visibility conditions allowed it, namely from January to June 2018. These observations correspond to the maximum flux level observed in the radio and X-ray bands. The upper limits derived from TeV observations are compared with the modelling of the late non-thermal emission using the multi-frequency SED. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)

关键词： Gravity waves

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Inferring Human Activities Using Robust Privileged Probabilistic Learning

Inferring Human Activities Using Robust Privileged Probabili...

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International Conference on Computer Vision Workshops (ICCV Workshops)

作者： Michalis Vrigkas Evangelos Kazakos Christophoros Nikou Ioannis A. Kakadiaris Computational Biomedicine Lab University of Houston Houston TX USA Dept. Computer Science & Engineering University of Ioannina Ioannina Greece

Classification models may often suffer from "structure imbalance" between training and testing data that may occur due to the deficient data collection process. This imbalance can be represented by the learning using privileged information (LUPI) paradigm. In this paper, we present a supervised probabilistic classification approach that integrates LUPI into a hidden conditional random field (HCRF) model. The proposed model is called LUPI-HCRF and is able to cope with additional information that is only available during training. Moreover, the proposed method employes Student's t-distribution to provide robustness to outliers by modeling the conditional distribution of the privileged information. Experimental results in three publicly available datasets demonstrate the effectiveness of the proposed approach and improve the state-of-the-art in the LUPI framework for recognizing human activities.

关键词： Training Robustness Videos Testing Probabilistic logic Visualization Activity recognition

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Fault tolerant variants of the fine-grained parallel incomplete LU factorization 25

Fault tolerant variants of the fine-grained parallel incompl...

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25th High Performance Computing Symposium, HPC 2017, Part of the 2017 Spring Simulation Multi-Conference, SpringSim 2017

作者： Coleman, Evan Sosonkina, Masha Chow, Edmond Naval Surface Warfare Center Dahlgren Division 17320 Dahlgren Rd DahlgrenVA United States Dept. of Modeling Simulation and Visualization Engineering Old Dominion University 5115 Hampton Blvd NorfolkVA United States School of Computational Science and Engineering Georgia Institute of Technology 266 Ferst Drive AtlantaGA United States

ISBN: (纸本)9781510838222

This paper presents an investigation into fault tolerance for the fine-grained parallel algorithm for computing an incomplete LU factorization. Results concerning the convergence of the algorithm with respect to the occurrence of faults, and the impact of any sub-optimality in the produced incomplete factors in Krylov subspace solvers are given. Numerical tests show that the simple algorithmic changes suggested here can ensure convergence of the fine-grained parallel incomplete factorization, and improve the performance of the use of the resulting factors as preconditioners in Krylov subspace solvers if faults do occur. ©2017 Society for Modeling & Simulation International (SCS).

关键词： Fault tolerance

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