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arXiv 2019年

作者： Emani, Prashant S. Warrell, Jonathan Anticevic, Alan Bekiranov, Stefan Gandal, Michael McConnell, Michael J. Sapiro, Guillermo Aspuru-Guzik, Alán Baker, Justin Bastiani, Matteo McClure, Patrick Murray, John Sotiropoulos, Stamatios N. Taylor, Jacob Senthil, Geetha Lehner, Thomas Gerstein, Mark B. Harrow, Aram W. Program in Computational Biology and Bioinformatics Yale University New HavenCT06520 United States Department of Molecular Biophysics and Biochemistry Yale University New HavenCT06520 United States Yale School of Medicine Department of Psychiatry New HavenCT06511 United States University of Virginia School of Medicine Department of Biochemistry and Molecular Genetics CharlottesvilleVA22903 United States Department of Psychiatry Semel Institute David Geffen School of Medicine University of California–Los Angeles 695 Charles E. Young Drive South Los AngelesCA90095 United States Univ. of Virginia School of Medicine Department of Neuroscience CharlottesvilleVA22903 United States Department of Electrical and Computer Engineering Duke University DurhamNC27708 United States Department of Chemistry University of Toronto 80 St. George Street TorontoONM5S 3H6 Canada TorontoONM5S 1M1 Canada CIFAR Artificial Intelligence Research Chair Vector Institute TorontoONM5S 1M1 Canada Department of Computer Science University of Toronto 40 St. George Street TorontoONM5S 2E4 Canada Schizophrenia and Bipolar Disorder Program McLean Hospital BelmontMA02478 United States Department of Psychiatry Harvard Medical School BostonMA02114 United States Sir Peter Mansfield Imaging Centre School of Medicine University of Nottingham NottinghamNG7 2RD United Kingdom Machine Learning Team National Institute of Mental Health BethesdaMD20892 United States Section on Functional Imaging Methods National Institute of Mental Health BethesdaMD20892 United States Department of Psychiatry Yale University School of Medicine New HavenCT06511 United States Department of Physics Yale University New HavenCT06511 United States Joint Center for Quantum Information and Computer Science University of Maryland College ParkMD20742 United States National Institute of Standards and Technology GaithersburgMD20899 United States Office of Genomics Research Coordination N

The search for meaningful structure in biological data has relied on cutting-edge advances in computational technology and data science methods. However, challenges arise as we push the limits of scale and complexity in biological problems. Innovation in massively parallel, classical computing hardware and algorithms continues to address many of these challenges, but there is a need to simultaneously consider new paradigms to circumvent current barriers to processing speed. Accordingly, we articulate a view towards quantum computation and quantum information science, where algorithms have demonstrated potential polynomial and exponential computational speedups in certain applications, such as machine learning. The maturation of the field of quantum computing, in hardware and algorithm development, also coincides with the growth of several collaborative efforts to address questions across length and time scales, and scientific disciplines. We use this coincidence to explore the potential for quantum computing to aid in one such endeavor: the merging of insights from genetics, genomics, neuroimaging and behavioral phenotyping. By examining joint opportunities for computational innovation across fields, we highlight the need for a common language between biological data analysis and quantum computing. Ultimately, we consider current and future prospects for the employment of quantum computing algorithms in the biological sciences. Copyright © 2019, The Authors. All rights reserved.

关键词： Machine learning

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An unambiguous AGN and a Balmer break in an Ultraluminous Little Red Dot at z=4.47 from Ultradeep UNCOVER and All the Little Things Spectroscopy

arXiv

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arXiv 2024年

作者： Labbe, Ivo Greene, Jenny E. Matthee, Jorryt Treiber, Helena Kokorev, Vasily Miller, Tim B. Kramarenko, Ivan Setton, David J. Ma, Yilun Goulding, Andy D. Bezanson, Rachel Naidu, Rohan P. Williams, Christina C. Atek, Hakim Brammer, Gabriel Cutler, Sam E. Chemerynska, Iryna Cloonan, Aidan P. Dayal, Pratika de Graaff, Anna Fudamoto, Yoshinobu Fujimoto, Seiji Furtak, Lukas J. Glazebrook, Karl Heintz, Kasper E. Leja, Joel Marchesini, Danilo Nanayakkara, Themiya Nelson, Erica J. Oesch, Pascal A. Pan, Richard Price, Sedona H. Shivaei, Irene Sobral, David Suess, Katherine A. van Dokkum, Pieter Wang, Bingjie Weaver, John R. Whitaker, Katherine E. Zitrin, Adi Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Am Campus 1 Klosterneuburg Austria Department of Astronomy The University of Texas at Austin AustinTX78712 United States Northwestern University IL60201 United States Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave. CambridgeMA02139 United States NSF National Optical-Infrared Astronomy Research Laboratory 950 North Cherry Avenue TucsonAZ85719 United States Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Astronomy University of Massachusetts AmherstMA01003 United States Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Center for Frontier Science Chiba University 1-33 Yayoi-cho Inage-ku Chiba263-8522 Japan Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen N2200 Denmark Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 Unite

We present a detailed exploration of the most optically-luminous Little Red Dot (LHα = 1044 erg/s, LV = 1045 erg/s, F444W = 22 AB) discovered by JWST to date. Located in the UNCOVER Abell 2744 field, source A2744−45924 was observed by NIRSpec/PRISM with ultradeep spectroscopy reaching SNR ∼ 100 pix−1, high-resolution 3 − 4 µm NIRCam/Grism spectroscopy from the All the Little Things (ALT) program, and multi-band NIRCam Medium Band imaging from Mega Science. The NIRCam spectra reveal high rest-frame equivalent width WHα,0,broad > 800 Å, broad Hα emission (FWHM ∼ 4500 km/s), on top of narrow, complex Hα absorption. NIRSpec data show exceptionally strong rest-frame ultraviolet (UV) to near-infrared (NIR) Fe II emission (WFeII−UV,0 ∼ 340 Å), UV N IV] λλ1483, 1486 and N III] λ1750, and broad NIR O Iλ8446 emission. The line spectra unambiguously demonstrate a broad-line region (BLR) associated with a possible MBH ∼ 109M supermassive black hole embedded in dense gas, which might explain the non-detection in ultradeep Chandra X-ray data ( 10× underluminous relative to broad LHα). Strong UV Nitrogen lines suggest supersolar N/O ratios due to rapid star formation or intense radiation fields near the AGN. The observed continuum shows a clear Balmer break at rest-frame 3650 Å, which cannot be accounted for by power-law AGN alone. A stellar population model produces an excellent fit with a reddened Balmer break and would imply a massive (M∗ ≈ 8 × 1010 M), old ∼ 500 Myr, compact stellar core, among the densest stellar systems known (ρ ≈ 3 ×106 M/pc2 for Re,optical = 70 ±10 pc), and AGN emission lines with extreme intrinsic equivalent width WHα,0 1000 Å. However, although high M∗ and MBH are supported by evidence of a galaxy overdensity containing 40 galaxies at z = 4.41 − 4.51, deep high-resolution spectroscopy is required to confirm stellar absorption and rule out that the Balmer break is instead caused by dense gas surrounding the AGN. © 2024, CC BY.

关键词： Stars

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The optical light curve of GRB 221009A: the afterglow and the emerging supernova

arXiv

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arXiv 2023年

作者： Fulton, M.D. Smartt, S.J. Rhodes, L. Huber, M.E. Villar, V.A. Moore, T. Srivastav, S. Schultz, A.S.B. Chambers, K.C. Izzo, L. Hjorth, J. Chen, T.-W. Nicholl, M. Foley, R.J. Rest, A. Smith, K.W. Young, D.R. Sim, S.A. Bright, J. Zenati, Y. de Boer, T. Bulger, J. Fairlamb, J. Gao, H. Lin, C.-C. Lowe, T. Magnier, E.A. Smith, I.A. Wainscoat, R. Coulter, D.A. Jones, D.O. Kilpatrick, C.D. McGill, P. Ramirez-Ruiz, E. Lee, K.-S. Narayan, G. Ramakrishnan, V. Ridden-Harper, R. Singh, A. Wang, Q. Kong, A.K.H. Ngeow, C.-C. Pan, Y.-C. Yang, S. Davis, K.W. Piro, A.L. Rojas-Bravo, C. Sommer, J. Yadavalli, S.K. Astrophysics Research Centre School of Mathematics and Physics Queen’s University BelfastBT7 1NN United Kingdom Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive HonoluluHI96822 United States Department of Astronomy and Astrophysics Pennsylvania State University 525 Davey Laboratory University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Technische Universität München TUM School of Natural Sciences Physik-Department James-Franck-Straße 1 Garching85748 Germany Max-Planck-Institut für Astrophysik Karl-Schwarzschild Straße 1 Garching85748 Germany Birmingham Institute for Gravitational Wave Astronomy School of Physics and Astronomy University of Birmingham BirminghamB15 2TT United Kingdom Department of Astronomy and Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA95060 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics and Astronomy The Johns Hopkins University BaltimoreMD21218 United States Institute for Astronomy University of Hawai’i 34 Ohia Ku St. PukalaniHI96768-8288 United States Gemini Observatory NSF’s NOIRLab 670 N. A’ohoku Place HiloHI96720 United States Northwestern University 1800 Sherman Ave EvanstonIL60201 United States Department of Physics and Astronomy Purdue University 525 Northwestern Avenue West LafayetteIN47907 United States Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green St. IL61801 United States Center for Astrophysical Surveys National Center for Super

We present extensive optical photometry of the afterglow of GRB 221009A. Our data cover 0.9 − 59.9 days from the time of Swift and Fermi GRB detections. Photometry in rizy-band filters was collected primarily with Pan-STARRS and supplemented by multiple 1- to 4-meter imaging facilities. We analyzed the Swift X-ray data of the afterglow and found a single decline rate power-law f(t) ∝ t−1.556±0.002 best describes the light curve. In addition to the high foreground Milky Way dust extinction along this line of sight, the data favour additional extinction to consistently model the optical to X-ray flux with optically thin synchrotron emission. We fit the X-ray-derived power-law to the optical light curve and find good agreement with the measured data up to 5 − 6 days. Thereafter we find a flux excess in the riy bands which peaks in the observer frame at ∼ 20 days. This excess shares similar light curve profiles to the type Ic broad-lined supernovae SN 2016jca and SN 2017iuk once corrected for the GRB redshift of z = 0.151 and arbitrarily scaled. This may be representative of a supernova emerging from the declining afterglow. We measure rest-frame absolute peak AB magnitudes of Mg = −19.8 ± 0.6 and Mr = −19.4 ± 0.3 and Mz = −20.1 ± 0.3. If this is an SN component, then Bayesian modelling of the excess flux would imply explosion parameters of Mej = 7.1+2.4−1.7 M, MNi = 1.0+0.6−0.4 M, and vej = 33, 900+5−5,900700 km s−1, for the ejecta mass, nickel mass and ejecta velocity respectively, inferring an explosion energy of Ekin ' 2.6 − 9.0 × 1052 ergs. © 2023, CC BY.

关键词： Photometry

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The UNCOVER Survey: First Release of Ultradeep JWST/NIRSpec PRISM spectra for ∼700 galaxies from z ∼ 0.3 − 13 in Abell 2744

arXiv

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arXiv 2024年

作者： Price, Sedona H. Bezanson, Rachel Labbe, Ivo Furtak, Lukas J. de Graaff, Anna Greene, Jenny E. Kokorev, Vasily Setton, David J. Suess, Katherine A. Brammer, Gabriel Cutler, Sam E. Leja, Joel Pan, Richard Wang, Bingjie Weaver, John R. Whitaker, Katherine E. Atek, Hakim Burgasser, Adam J. Chemerynska, Iryna Dayal, Pratika Feldmann, Robert Förster Schreiber, Natascha M. Fudamoto, Yoshinobu Fujimoto, Seiji Glazebrook, Karl Goulding, Andy D. Khullar, Gourav Kriek, Mariska Marchesini, Danilo Maseda, Michael V. Miller, Tim B. Muzzin, Adam Nanayakkara, Themiya Nelson, Erica Oesch, Pascal A. Shipley, Heath Smit, Renske Taylor, Edward N. van Dokkum, Pieter Williams, Christina C. Zitrin, Adi Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Physics Department Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Astronomy The University of Texas at Austin AustinTX78712 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Astronomy University of Massachusetts AmherstMA01003 United States Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Physics and Astronomy Tufts University 574 Boston Ave. MedfordMA02155 United States Denmark Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Department of Astronomy & Astrophysics UC San Diego La Jolla CA United States Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Department of Astrophysics University of Zurich CH-8057 Switzerland Max-Planck-Institut für extraterrestrische Physik Giessenbachstrasse 1 Garching85748 Germany Center for Frontier Science Chiba University 1-33 Yayoi-cho Inage-ku Chiba263-8522 Japan Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia Leiden Observatory

We present the design and observations of low resolution JWST/NIRSpec PRISM spectroscopy from the Ultradeep NIRSpec and NIRCam ObserVations before the Epoch of Reionization (UNCOVER) Cycle 1 JWST Treasury program. Targets are selected using JWST/NIRCam photometry from UNCOVER and other programs, and cover a wide range of categories and redshifts to ensure the legacy value of the survey. These categories include the first galaxies at z 10, faint galaxies during the Epoch of Reionization (z ∼ 6 − 8), high redshift AGN (z 6), Population III star candidates, distant quiescent and dusty galaxies (1 z 6), and filler galaxies sampling redshift–color–magnitude space from z ∼ 0.1 − 13. Seven NIRSpec MSA masks across the extended Abell 2744 cluster were observed, along with NIRCam parallel imaging in 8 filters (F090W, F115W, F150W, F200W, F277W, F356W, F410M, F444W, F480M) over a total area of ∼26 arcmin2, overlapping existing HST coverage from programs including the Hubble Frontier Fields and BUFFALO. We successfully observed 553 objects down to mF444W ∼ 30AB, and by leveraging mask overlaps, we reach total on-target exposure times ranging from 2.4 − 16.7h. We demonstrate the success rate and distribution of confirmed redshifts, and also highlight the rich information revealed by these ultradeep spectra for a subset of our targets. An updated lens model of Abell 2744 is also presented, including 14 additional spectroscopic redshifts and finding a total cluster mass of MSL = (2.1 ± 0.3) × 1015 M☉. We publicly release reduced 1D and 2D spectra for all objects observed in Summer 2023 along with a spectroscopic redshift catalog and the updated lens model of the cluster (https://***/***). Copyright © 2024, The Authors. All rights reserved.

关键词： Prisms

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Abstracts from Hydrocephalus 2016 Abstracts

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FLUIDS AND BARRIERS OF THE CNS 2017年第SUPPL 1期14卷 1-21页

作者： [Anonymous] Johns Hopkins University Baltimore MD USA. Department of Neurosurgery Johns Hopkins University Baltimore MD USA. Johns Hopkins Biostatistics Center Johns Hopkins Bloomberg School of Public Health Baltimore MD USA. Johns Hopkins Bloomberg School of Public Health Baltimore MD USA. Department of Neurosurgery Johns Hopkins University School of Medicine Baltimore MD USA. Johns Hopkins Aramco Healthcare Dhahran Saudi Arabia. Johns Hopkins Hopkins Aramco Healthcare Dhahran Saudi Arabia. Johns Hopkins Aramco Healthcare Ras Tanura Saudi Arabia. Primary Care Johns Hopkins Aramco Healthcare Ras Tanura Saudi Arabia. Bloomberg School of Public Health Johns Hopkins University Baltimore MD USA. Department of Neurosurgery Rhode Island Hospital Providence RI USA. Department of Epidemiology Johns Hopkins Bloomberg School of Public Health Baltimore MD USA. The Interface Group Institute of PhysiologyUniversity of Zurich Zurich Switzerland. Institute of Physiology University of Zurich Zurich Switzerland. Neuroscience Center Zurich and the Zurich Center for Integrative Human Physiology University of Zurich Zurich Switzerland. BioFlowImage Laboratory University of Picardie Jules Verne Amiens France. Reims Mathematics Laboratory University of Reims Champagne-Ardenne Reims France. Image Processing Laboratory University Hospital of Amiens-Picardie Amiens France. BioFlowImage Laboratory Department of Medical Image Processing University Hospital of Picardie Jules Verne Amiens France. Department of Geriatric University Hospital of Toulouse Toulouse France. Departments of Geriatric University Hospital of Toulouse Toulouse France. Department of Geriatry University Hospital Toulouse Toulouse France. Neurosciences department University of Cambridge Cambridge UK. Brain Physics Lab Academic Neurosurgery University of Cambridge Cambridge UK. Department of Nuclear Medicine University Hospital of Toulouse Toulouse France. Department of Nuclear Medicine University Hospit

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The gravity collective: A search for the electromagnetic counterpart to the neutron star-black hole merger GW190814

arXiv

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arXiv 2021年

作者： Kilpatrick, Charles D. Coulter, David A. Arcavi, Iair Brink, Thomas G. Dimitriadis, Georgios Filippenko, Alexei V. Foley, Ryan J. Howell, D. Andrew Jones, David O. Makler, Martin Piro, Anthony L. Rojas-Bravo, César Sand, David J. Swift, Jonathan J. Tucker, Douglas Zheng, Weikang Allam, Sahar S. Annis, James T. Antilen, Juanita Bachmann, Tristan G. Bloom, Joshua S. Bom, Clecio R. Bostroem, K. Azalee Brout, Dillon Burke, Jamison Butler, Robert E. Butner, Melissa Campillay, Abdo Clever, Karoli E. Conselice, Christopher J. Cooke, Jeff Dage, Kristen C. de Carvalho, Reinaldo R. Jaeger, Thomas D.E. Desai, Shantanu Garcia, Alyssa Garcia-Bellido, Juan Gill, Mandeep S.S. Girish, Nachiket Hallakoun, Na'Ama Herner, Kenneth Hiramatsu, Daichi Holz, Daniel E. Huber, Grace Kawash, Adam M. McCully, Curtis Medallon, Sophia A. Metzger, Brian D. Modak, Shaunak Morgan, Robert Muñoz, Ricardo R. Muñoz-Elgueta, Nahir Murakami, Yukei S. Olivares, Felipe E. Palmese, Antonella Patra, Kishore Pereira, Maria E.S. Pessi, Thallis L. Pineda-Garcia, J. Quirola-Vásquez, Jonathan Ramirez-Ruiz, Enrico Rembold, Sandro Barboza Rest, Armin Rodríguez, Ósmar Santana-Silva, Luidhy Sherman, Nora F. Siebert, Matthew R. Smith, Carli Smith, J. Allyn Soares-Santos, Marcelle Stacey, Holland Stahl, Benjamin E. Strader, Jay Strasburger, Erika Sunseri, James Tinyanont, Samaporn Tucker, Brad E. Ulloa, Natalie Valenti, Stefano Vasylyev, Sergiy Wiesner, Matthew P. Zhang, Keto D. Northwestern University EvanstonIL60208 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel CIFAR Azrieli Global Scholars program CIFAR Toronto Canada Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Las Cumbres Observatory 6740 Cortona Dr Suite 102 GoletaCA93117-5575 United States International Center for Advanced Studies & Instituto de Ciencias Físicas ECyT-UNSAM & CONICET Buenos Aires1650 Argentina Centro Brasileiro de Pesquisas Físicas Rua Dr. Xavier Sigaud 150 Rio de Janeiro RJCEP 22290-180 Brazil The Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States Thacher Observatory Thacher School 5025 Thacher Rd. OjaiCA93023 United States Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Departamento de Astronomía Universidad de Chile Camino El Observatorio 1515 Las Condes Santiago Chile Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Lawrence Berkeley National Laboratory 1 Cyclotron Road MS 50B-4206 BerkeleyCA94720-3411 United States Centro Federal de Educação Tecnológica Celso Suckow da Fonseca Rodovia Mário Covas lote J2 quadra J Itaguaí RJCEP 23810-000 Brazil Department of Physics and Astronomy University of California DavisCA95616 United States Center for Astrophysics Harvard & Smithsonian 60 Garden St CambridgeMA02138 United States Department of Astronomy Indiana University 727 E. Third St. BloomingtonIN47405 United States Dep

We present optical follow-up imaging obtained with the Katzman Automatic Imaging Telescope, Las Cumbres Observatory Global Telescope Network, Nickel Telescope, Swope Telescope, and Thacher Telescope of the LIGO/Virgo gravitational wave (GW) signal from the neutron star–black hole (NSBH) merger GW190814. We searched the GW190814 localization region (19 deg2 for the 90th percentile best localization), covering a total of 51 deg2 and 94.6% of the two-dimensional localization region. Analyzing the properties of 189 transients that we consider as candidate counterparts to the NSBH merger, including their localizations, discovery times from merger, optical spectra, likely host-galaxy redshifts, and photometric evolution, we conclude that none of these objects are likely to be associated with GW190814. Based on this finding, we consider the likely optical properties of an electromagnetic counterpart to GW190814, including possible kilonovae and short gamma-ray burst afterglows. Using the joint limits from our follow-up imaging, we conclude that a counterpart with an rband decline rate of 0.68 mag day−1, similar to the kilonova AT 2017gfo, could peak at an absolute magnitude of at most −17.8 mag (50% confidence). Our data are not constraining for "red" kilonovae and rule out "blue" kilonovae with M > 0.5 M* (30% confidence). We strongly rule out all known types of short gamma-ray burst afterglows with viewing angles ◦ assuming an initial jet opening angle of ∼ 5.2◦ and explosion energies and circumburst densities similar to afterglows explored in the literature. Finally, we explore the possibility that GW190814 merged in the disk of an active galactic nucleus, of which we find four in the localization region, but we do not find any candidate counterparts among these sources. © 2021, CC BY.

关键词： Stars

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Supermassive Black Hole Winds in X-rays - SUBWAYS. I. Ultra-fast outflows in QSOs beyond the local Universe

arXiv

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arXiv 2022年

作者： Matzeu, G.A. Brusa, M. Lanzuisi, G. Dadina, M. Bianchi, S. Kriss, G. Mehdipour, M. Nardini, E. Chartas, G. Middei, R. Piconcelli, E. Gianolli, V. Comastri, A. Longinotti, A.L. Krongold, Y. Ricci, F. Petrucci, P.O. Tombesi, F. Luminari, A. Zappacosta, L. Miniutti, G. Gaspari, M. Behar, E. Bischetti, M. Mathur, S. Perna, M. Giustini, M. Grandi, P. Torresi, E. Vignali, C. Bruni, G. Cappi, M. Costantini, E. Cresci, G. De Marco, B. De Rosa, A. Gilli, R. Guainazzi, M. Kaastra, J. Kraemer, S. La Franca, F. Marconi, A. Panessa, F. Ponti, G. Proga, D. Ursini, F. Fiore, F. King, A.R. Maiolino, R. Matt, G. Merloni, A. University of Bologna Via Gobetti 93/2 BolognaI-40129 Italy INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Gobetti 93/3 BolognaI-40129 Italy Villanueva de la Cañada MadridE-28691 Spain Dipartimento di Matematica e Fisica Universitá degli Studi Roma Tre Via della Vasca Navale 84 RomaI-00146 Italy Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States INAF Osservatorio Astrofisico di Arcetri Largo Enrico Fermi 5 FirenzeI-50125 Italy Department of Physics and Astronomy College of Charleston CharlestonSC29424 United States Space Science Data Center - ASI Via del Politecnico s.n.c. Roma00133 Italy INAF - Osservatorio Astronomico di Roma Via Frascati 33 Monte Porzio Catone Roma00078 Italy Univ. Grenoble Alpes CNRS IPAG Grenoble38000 France Instituto de Astronomía Universidad Nacional Autónoma de México Circuito Exterior Ciudad Universitaria Ciudad de México04510 Mexico Department of Physics University of Rome 'Tor Vergata' Via della Ricerca Scientifica 1 RomeI-00133 Italy Department of Astronomy University of Maryland College ParkMD20742 United States NASA/Goddard Space Flight Center Code 662 GreenbeltMD20771 United States INAF - Istituto di Astrofisica e Planetologia Spaziali Via Fosso del Cavaliere RomaI-00133 Italy Camino Bajo del Castillo s/n Villanueva de la Cañada MadridE-28692 Spain Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544-1001 United States Physics Department The Technion Haifa32000 Israel INAF - Osservatorio Astronomico di Trieste Via G. B. Tiepolo 11 Trieste34143 Italy Department of Astronomy The Ohio State University 140 West 18th Avenue ColumbusOH43210 United States Center for Cosmology and Astroparticle Physics 191 West Woodruff Avenue ColumbusOH43210 United States SRON Netherlands Institute for Space Research Niels Bohrweg 4 Leiden2333 CA Netherlands Departament de Física EEBE Universitat Politè

We present a new X-ray spectroscopic study of 22 luminous (2 × 1045 ≾ Lbol/erg s−1 ≾ 2 × 1046) active galactic nuclei (AGNs) at intermediate-redshift (0.1 ≾ z ≾ 0.4), as part of the SUpermassive Black hole Winds in the x-rAYS (SUBWAYS) sample, mostly composed of quasars (QSOs) and type 1 AGN. Here, 17 targets were observed with XMM-Newton between 2019-2020 and the remaining 5 are from previous observations. The aim of this large campaign (1.45 Ms duration) is to characterise the various manifestations of winds in the X-rays driven from supermassive black holes in AGN. In this paper we focus on the search and characterization of ultra-fast outflows (UFOs), which are typically detected through blueshifted absorption troughs in the Fe K band (E > 7 keV). By following Monte Carlo procedures, we confirm the detection of absorption lines corresponding to highly ionised iron (e.g., Fe xxv Hα, Fe xxvi Lyα) in 7/22 sources at the ≿ 95% confidence level (for each individual line). The global combined probability of such absorption features in the sample is > 99.9%. The SUBWAYS campaign extends at higher luminosity and redshifts than previous local studies on Seyferts, obtained using XMM-Newton and Suzaku observations. We find a UFO detection fraction of ∼ 30% on the total sample that is in agreement with the previous findings. This work independently provides further support for the existence of highly-ionised matter propagating at mildly relativistic speed (≿ 0.1c) in a considerable fraction of AGN over a broad range of luminosities, which is expected to play a key role in the self-regulated AGN feeding-feedback cycle, as also supported by hydrodynamical multiphase simulations. Copyright © 2022, The Authors. All rights reserved.

关键词： Active Galactic Nuclei

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Discovery of Two-dimensional Hexagonal MBene HfBO and Exploration on its Potential for Lithium-Ion Storage

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Angewandte Chemie 2023年第36期135卷

作者： Nanxi Miao Prof. Yutong Gong Huaiyu Zhang Qing Shen Rui Yang Prof. Jianping Zhou Prof. Hideo Hosono Prof. Junjie Wang State Key Laboratory of Solidification Processing School of Materials Science and Engineering Department Northwestern Polytechnical University Xi'an Shaanxi 710072 P. R. China Contribution: Data curation (lead) Formal analysis (equal) Funding acquisition (equal) Software (lead) Writing - original draft (lead) Contribution: Data curation (equal) Formal analysis (equal) Funding acquisition (equal) Validation (equal) Writing - original draft (equal) Writing - review & editing (equal) Contribution: Formal analysis (equal) Software (equal) Contribution: Formal analysis (equal) Investigation (equal) Software (equal) Contribution: Investigation (equal) School of Physics & Information Technology Shaanxi Normal University Xi'an 710119 P. R. China Contribution: Formal analysis (equal) Investigation (equal) MDX Research Center for Element Strategy Tokyo Institute of Technology 4259 Nagatsuta-cho Midori-ku Yokohama Kanagawa 226-8503 Japan Contribution: Funding acquisition (equal) Investigation (equal) Writing - review & editing (equal) Contribution: Conceptualization (lead) Data curation (equal) Formal analysis (equal) Funding acquisition (equal) Supervision (lead) Writing - original draft (lead) Writing - review & editing (lead)

The practical applications of two-dimensional (2D) transition-metal borides (MBenes) have been severely hindered by the lack of accessible MBenes because of the difficulties in the selective etching of traditional ternary MAB phases with orthorhombic symmetry ( ort -MAB). Here, we discover a family of ternary hexagonal MAB ( h -MAB) phases and 2D hexagonal MBenes ( h -MBenes) by ab initio predictions and experiments. Calculations suggest that the ternary h -MAB phases are more suitable precursors for MBenes than the ort -MAB phases. Based on the prediction, we report the experimental synthesis of h -MBene HfBO by selective removal of In from h -MAB Hf 2 InB 2 . The synthesized 2D HfBO delivered a specific capacity of 420 mAh g −1 as an anode material in lithium-ion batteries, demonstrating the potential for energy-storage applications. The discovery of this h -MBene HfBO added a new member to the growing family of 2D materials and provided opportunities for a wide range of novel applications.

关键词： DFT Calculations High-Throughput Screening Lithium-Ion Batteries Two-Dimensional Materials h-MBenes

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Machine Learning for Mini-EUSO Telescope data Analysis

arXiv

引用

arXiv 2023年

作者： Bertaina, Mario Zotov, Mikhail Anzhiganov, Dmitry Barghini, Dario Blaksley, Carl Coretti, Antonio Giulio Kryazhenkov, Aleksandr Montanaro, Antonio Olivi, Leonardo Abe, S. Adams, J.H. Allard, D. Alldredge, P. Aloisio, R. Anchordoqui, L. Anzalone, A. Arnone, E. Bagheri, M. Baret, B. Barghini, D. Battisti, M. Bellotti, R. Belov, A.A. Bertaina, M. Bertone, P.F. Bianciotto, M. Bisconti, F. Blaksley, C. Blin-Bondil, S. Bolmgren, K. Briz, S. Burton, J. Cafagna, F. Cambié, G. Campana, D. Capel, F. Caruso, R. Casolino, M. Cassardo, C. Castellina, A. Černý, K. Christl, M.J. Colalillo, R. Conti, L. Cotto, G. Crawford, H.J. Cremonini, R. Creusot, A. Cummings, A. de Castro Gónzalez, A. de la Taille, C. Diesing, R. Dinaucourt, P. Di Nola, A. Ebisuzaki, T. Eser, J. Fenu, F. Ferrarese, S. Filippatos, G. Finch, W.W. Flaminio, F. Fornaro, C. Fuehne, D. Fuglesang, C. Fukushima, M. Gadamsetty, S. Gardiol, D. Garipov, G.K. Gazda, E. Golzio, A. Guarino, F. Guépin, C. Haungs, A. Heibges, T. Isgrò, F. Judd, E.G. Kajino, F. Kaneko, I. Kim, S.-W. Klimov, P.A. Krizmanic, J.F. Kungel, V. Kuznetsov, E. Martínez, F. López Mandát, D. Manfrin, M. Marcelli, A. Marcelli, L. Marszal, W. Matthews, J.N. Mese, M. Meyer, S.S. Mimouni, J. Miyamoto, H. Mizumoto, Y. Monaco, A. Nagataki, S. Nachtman, J.M. Naumov, D. Neronov, A. Nonaka, T. Ogawa, T. Ogio, S. Ohmori, H. Olinto, A.V. Onel, Y. Osteria, G. Otte, A.N. Pagliaro, A. Panico, B. Parizot, E. Park, I.H. Paul, T. Pech, M. Perfetto, F. Picozza, P. Piotrowski, L.W. Plebaniak, Z. Posligua, J. Potts, M. Prevete, R. Prévôt, G. Przybylak, M. Reali, E. Reardon, P. Reno, M.H. Ricci, M. Matamala, O.F. Romero Romoli, G. Sagawa, H. Sakaki, N. Saprykin, O.A. Sarazin, F. Sato, M. Schovánek, P. Scotti, V. Selmane, S. Sharakin, S.A. Shinozaki, K. Stepanoff, S. Soriano, J.F. Szabelski, J. Tajima, N. Tajima, T. Takahashi, Y. Takeda, M. Takizawa, Y. Thomas, S.B. Tkachev, L.G. Tomida, T. Toscano, S. Dipartimento di Fisica Università di Torino Torino Italy INFN Sezione di Torino Torino Italy Skobeltsyn Institute of Nuclear Physics Lomonosov Moscow State University Moscow Russia Faculty of Computational Mathematics and Cybernetics Lomonosov Moscow State University Moscow Russia INAF Osservatorio astrofisico di Torino Torino Italy RIKEN Wako Japan Department of Electronics and Telecommunications Polytechnic University of Turin Corso Duca degli Abruzzi 24 Turin10129 Italy Algiers Algeria Univ. Constantine I Constantine Algeria Joint Laboratory of Optics Faculty of Science Palacký University Olomouc Czech Republic Institute of Physics of the Czech Academy of Sciences Prague Czech Republic Omega Ecole Polytechnique CNRS IN2P3 Palaiseau France Université de Paris CNRS AstroParticule et Cosmologie ParisF-75013 France France Germany Max Planck Institute for Physics Munich Germany Istituto Nazionale di Fisica Nucleare - Sezione di Bari Italy Università degli Studi di Bari Aldo Moro Italy Dipartimento di Fisica e Astronomia "Ettore Majorana" Università di Catania Italy Istituto Nazionale di Fisica Nucleare - Sezione di Catania Italy Istituto Nazionale di Fisica Nucleare - Laboratori Nazionali di Frascati Italy Istituto Nazionale di Fisica Nucleare - Sezione di Napoli Italy Università di Napoli Federico II Dipartimento di Fisica "Ettore Pancini" Italy INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica Palermo Italy Istituto Nazionale di Fisica Nucleare - Sezione di Roma Tor Vergata Italy Università di Roma Tor Vergata - Dipartimento di Fisica Roma Italy Istituto Nazionale di Fisica Nucleare - Sezione di Torino Italy Dipartimento di Fisica Università di Torino Italy Osservatorio Astrofisico di Torino Istituto Nazionale di Astrofisica Italy Uninettuno University Rome Italy Agenzia Spaziale Italiana Via del Politecnico Roma00133 Italy Gran Sasso Science Institute L’Aquila Italy Institute for Cosmic Ray Research University of Tokyo Kashiwa Ja

Neural networks as well as other methods of machine learning (ML) are known to be highly efficient in different classification tasks, including classification of images and videos. Mini-EUSO is a wide-field-of-view imaging telescope that operates onboard the International Space Station since 2019 collecting data on miscellaneous processes that take place in the atmosphere of Earth in the UV range. Here we briefly present our results on the development of ML-based approaches for recognition and classification of track-like signals in the Mini-EUSO data, among them meteors, space debris and signals the light curves and kinematics of which are similar to those expected from extensive air showers generated by ultra-high-energy cosmic rays. We show that even simple neural networks demonstrate impressive performance in solving these tasks. © 2023, CC BY.

关键词： Machine learning

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COSMOS2020: A panchromatic view of the universe to z ∼ 10 from two complementary catalogs

arXiv

引用

arXiv 2021年

作者： Weaver, John R. Kauffmann, O.B. Ilbert, O. McCracken, H.J. Moneti, A. Toft, S. Brammer, G. Shuntov, M. Davidzon, I. Hsieh, B.C. Laigle, C. Anastasiou, A. Jespersen, C.K. Vinther, J. Capak, P. Casey, C.M. McPartland, C.J.R. Milvang-Jensen, B. Mobasher, B. Sanders, D.B. Zalesky, L. Arnouts, S. Aussel, H. Dunlop, J.S. Faisst, A. Franx, M. Furtak, L.J. Fynbo, J.P.U. Gould, K.M.L. Greve, T.R. Gwyn, S. Kartaltepe, J.S. Kashino, D. Koekemoer, A.M. Kokorev, V. Le Fèvre, O. Lilly, S. Masters, D. Magdis, G. Mehta, V. Peng, Y. Riechers, D.A. Salvato, M. Sawicki, M. Scarlata, C. Scoville, N. Shirley, R. Sneppen, A. Smolčić, V. Steinhardt, C. Stern, D. Tanaka, M. Taniguchi, Y. Teplitz, H.I. Vaccari, M. Wang, W.-H. Zamorani, G. Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Aix Marseille Univ CNRS LAM Laboratoire d’Astrophysique de Marseille Marseille France Institut d’Astrophysique de Paris UMR 7095 CNRS Sorbonne Université 98 bis boulevard Arago Paris75014 France Institute of Astrophysics & Astronomy Academia Sinica Taipei10617 Taiwan The University of Texas at Austin 2515 Speedway Blvd Stop C1400 AustinTX78712 United States Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Department of Physics and Astronomy University of California Riverside 900 University Avenue RiversideCA92521 United States AIM UMR 7158 CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom Infrared Processing and Analysis Center California Institute of Technology 1200 E. California Blvd PasadenaCA91125 United States Leiden Observatory Leiden University P.O.Box 9513 LeidenNL-2300 AA Netherlands DTU-Space Technical University of Denmark Elektrovej 327 Kgs. LyngbyDK2800 Denmark Department of Physics and Astronomy University College London Gower Place LondonWC1E 6BT United Kingdom Herzberg Astronomy and Astrophysics National Research Council of Canada 5071 West Saanich Rd. VictoriaBCV9E 2E7 Canada School of Physics and Astronomy Institute of Technology 84 Lomb Memorial Drive RochesterNY14623 United States Department of Physics ETH Zürich Wolfgang-Pauli-Strasse 27 Zurich8093 Switzerland Institute for Advanced Research Nagoya University Furocho Chikusa Aichi Nagoya464-8602 Japan Space Telescope Science Institute 3700 San Martin Dr. BaltimoreMD21218 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Institute for Astronomy Astrophysics Space Applications and Remo

The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data has been collected in the COSMOS field. This paper describes the collection, processing, and analysis of this new imaging data to produce a new reference photometric redshift catalog. Source detection and multi-wavelength photometry is performed for 1.7 million sources across the 2 deg2 of the COSMOS field, ∼966 000 of which are measured with all available broad-band data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The i © 2021, CC BY.

关键词： Photometry

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