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arXiv 2023年

作者： Wang, Bingjie Leja, Joel Labbé, Ivo Bezanson, Rachel Whitaker, Katherine E. Brammer, Gabriel Furtak, Lukas J. Weaver, John R. Price, Sedona H. Zitrin, Adi Atek, Hakim Coe, Dan Cutler, Sam E. Dayal, Pratika van Dokkum, Pieter Feldmann, Robert Marchesini, Danilo Franx, Marijn Schreiber, Natascha Förster Fujimoto, Seiji Geha, Marla Glazebrook, Karl de Graaff, Anna Greene, Jenny E. Juneau, Stéphanie Kassin, Susan Kriek, Mariska Khullar, Gourav Maseda, Michael Mowla, Lamiya A. Muzzin, Adam Nanayakkara, Themiya Nelson, Erica J. Oesch, Pascal A. Pacifici, Camilla Pan, Richard Papovich, Casey Setton, David J. Shapley, Alice E. Smit, Renske Stefanon, Mauro Suess, Katherine A. Taylor, Edward N. Williams, Christina C. 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 Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Physics & Astronomy and PITT PACC University of Pittsburgh PittsburghPA15260 United States Department of Astronomy University of Massachusetts AmherstMA01003 United States Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Beer-Sheva8410501 Israel Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Space Telescope Science Institute BaltimoreMD21218 United States Association of Universities for Research in Astronomy Inc. for the European Space Agency United States Center for Astrophysical Sciences Department of Physics & Astronomy Johns Hopkins University BaltimoreMD21218 United States Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Department of Astronomy Yale University New HavenCT06511 United States Institute for Computational Science University of Zurich Winterhurerstrasse 190 ZurichCH-8006 Switzerland Department of Physics & Astronomy Tufts University MedfordMA02155 United States Leiden Observatory Leiden University P.O.Box 9513 LeidenNL-2300 AA Netherlands Max-Planck-Institut für extraterrestrische Physik Gießenbachstraße 1 Garching85748 Germany Department of Astronomy The University of Texas at Austin AustinTX78712 United States Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Department of Astrophysical Sciences Princeton University Princ

The recent UNCOVER survey with the James Webb Space Telescope (JWST) exploits the nearby cluster Abell 2744 to create the deepest view of our universe to date by leveraging strong gravitational lensing. In this work, we perform photometric fitting of more than 50,000 robustly detected sources out to z ∼ 15. We show the redshift evolution of stellar ages, star formation rates, and rest-frame colors across the full range of 0.2 z 15. The galaxy properties are inferred using the Prospector Bayesian inference framework using informative Prospector-β priors on masses and star formation histories to produce joint redshift and stellar population posteriors, and additionally lensing magnification is performed on-the-fly to ensure consistency with the scale-dependent priors. We show that this approach produces excellent photometric redshifts with σNMAD ∼ 0.03, of a similar quality to the established photometric redshift code EAzY. In line with the open-source scientific objective of the Treasury survey, we publicly release the stellar population catalog with this paper, derived from the photometric catalog adapting aperture sizes based on source profiles. This release a) includes posterior moments, maximum-likelihood spectra, star-formation histories, and full posterior distributions, offering a rich data set to explore the processes governing galaxy formation and evolution over a parameter space now accessible by JWST. Copyright © 2023, The Authors. All rights reserved.

关键词： Inference engines

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Stable attractors in the three-dimensional general relativistic Poynting-Robertson effect

arXiv

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arXiv 2019年

作者： de Falco, Vittorio Bakala, Pavel Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 OpavaCZ-74601 Czech Republic M. R. Štefánik Observatory Planetarium Sládkovičova 41 Hlohovec920 01

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A new approximation of photon geodesics in Schwarzschild spacetime

arXiv

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arXiv 2019年

作者： la Placa, Riccardo Bakala, Pavel Stella, Luigi Falanga, Maurizio INAF - Osservatorio Astronomico di Roma Monte Porzio Catone Italy Research Centre for Computational Physics and Data Processing Silesian University in Opava Czech Republic M. R. Štefánik Observatory and Planetarium Hlohovec Slovakia Bern Switzerland International Space Science Institute Beijing China

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Mapping Obscured Star Formation in the Host Galaxy of FRB 20201124A

arXiv

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arXiv 2023年

作者： Dong, Yuxin Eftekhari, Tarraneh Fong, Wen-Fai Deller, Adam T. Mannings, Alexandra G. Simha, Sunil Sridhar, Navin Rafelski, Marc Gordon, Alexa C. Bhandari, Shivani Day, Cherie K. Heintz, Kasper E. Hessels, Jason W.T. Leja, Joel James, Clancy W. Kilpatrick, Charles D. Mahony, Elizabeth K. Marcote, Benito Margalit, Ben Nimmo, Kenzie Prochaska, J. Xavier Escorial, Alicia Rouco Ryder, Stuart D. Schroeder, Genevieve Shannon, Ryan M. Tejos, Nicolas Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology John St HawthornVIC3122 Australia Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Department of Astronomy Columbia University New YorkNY10027 United States Group Columbia University New YorkNY10027 United States Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91106 United States Space Telescope Science Institute BaltimoreMD21218 United States Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States CSIRO Space and Astronomy PO Box 76 EppingNSW1710 Australia Department of Physics McGill University MontrealQCH3A 2T8 Canada Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen NDK-2200 Denmark ASTRON Netherlands Institute for Radio Astronomy Oude Hoogeveensedijk 4 Dwingeloo7991 PD Netherlands Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands 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 International Centre for Radio Astronomy Research Curtin University BentleyWA6102 Australia Joint Institute for VLBI ERIC Oude Hoogeveensedijk 4 Dwingeloo7991 PD Netherlands Astronomy Department Theoretical Astrophysics Center University of California Berkeley BerkeleyCA94720 United States MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States 5-1-5 Kashiwanoha Kashiwa277-8583 Japan Division of Scien

We present high-resolution 1.5–6 GHz Karl G. Jansky Very Large Array (VLA) and Hubble Space Telescope (HST) optical and infrared observations of the extremely active repeating fast radio burst (FRB) FRB 20201124A and its barred spiral host galaxy. We constrain the location and morphology of star formation in the host and search for a persistent radio source (PRS) coincident with FRB 20201124A. We resolve the morphology of the radio emission across all frequency bands and measure a star formation rate SFR ≈ 8.9 M☉ yr−1, approximately ≈ 2.5 − 6 times larger than optically-inferred SFRs, demonstrating dust-obscured star formation throughout the host. Compared to a sample of all known FRB hosts with radio emission, the host of FRB 20201124A has the most significantly obscured star formation. While HST observations show the FRB to be offset from the bar or spiral arms, the radio emission extends to the FRB location. We propose that the FRB progenitor could have formed in situ (e.g., a magnetar born from a massive star explosion). It is still plausible, although less likely, that the progenitor of FRB 20201124A migrated from the central bar of the host. We further place a limit on the luminosity of a putative PRS at the FRB position of L6.0 GHz 1.8 ×1027 erg s−1 Hz−1, among the deepest PRS luminosity limits to date. However, this limit is still broadly consistent with both magnetar nebulae and hypernebulae models assuming a constant energy injection rate of the magnetar and an age of 105 yr in each model, respectively. © 2023, CC BY.

关键词： Luminance

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Puffy accretion disks: sub-Eddington, optically thick, and stable

arXiv

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arXiv 2019年

作者： Lančová, Debora Abarca, David Kluźniak, Wlodek Wielgus, Maciek Sadowski, Aleksander Narayan, Ramesh Schee, Jan Török, Gabriel Abramowicz, Marek Research Center for Computational Physics and Data Processing Research Centre of Theoretical Physics and Astrophysics Institute of Physics Silesian University in Opava Czech Republic Black Hole Initiative at Harvard University 20 Garden Street CambridgeMA02138 United States Nicolaus Copernicus Astronomical Centre Polish Academy of Sciences Bartycka 18 Warsaw00-716 Poland Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Akuna Capital 333 South Wabash Av. ChicagoIL60604 United States Department of Physics Göteborg University Sweden

We report on a new class of solutions of black hole accretion disks that we have found through three-dimensional, global, radiative magnetohydrodynamic simulations in general relativity. It combines features of the canonical thin, slim and thick disk models but differs in crucial respects from each of them. We expect these new solutions to provide a more realistic description of black hole disks than the slim disk model. We are presenting a disk solution for a non-spinning black hole at a sub-Eddington mass accretion rate, M = 0.6 M Edd. By the density scale-height measure the disk appears to be thin, having a high density core near the equatorial plane of height hρ ∼ 0.1 r, but most of the inflow occurs through a highly advective, turbulent, optically thick, Keplerian region that sandwiches the core and has a substantial geometrical thickness comparable to the radius, H ∼ r. The accreting fluid is supported above the midplane in large part by the magnetic field, with the gas and radiation to magnetic pressure ratio β ∼ 1, this makes the disk thermally stable, even though the radiation pressure strongly dominates over gas pressure. A significant part of the radiation emerging from the disk is captured by the black hole, so the disk is less luminous than a thin disk would be at the same accretion rate. Copyright © 2019, The Authors. All rights reserved.

关键词： Relativity

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Detection of p-mode Oscillations in HD 35833 with NEID and TESS

arXiv

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arXiv 2022年

作者： Gupta, Arvind F. Luhn, Jacob Wright, Jason T. Mahadevan, Suvrath Ford, Eric B. Stefánsson, Guðmundur Bender, Chad F. Blake, Cullen H. Halverson, Samuel Hearty, Fred Kanodia, Shubham Logsdon, Sarah E. McElwain, Michael W. Ninan, Joe P. Robertson, Paul Roy, Arpita Schwab, Christian Terrien, Ryan C. Department of Astronomy & Astrophysics 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Center for Exoplanets and Habitable Worlds 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Department of Physics & Astronomy The University of California Irvine IrvineCA92697 United States Penn State Extraterrestrial Intelligence Center 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Center for Astrostatistics 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08540 United States Steward Observatory The University of Arizona 933 N. Cherry Ave TucsonAZ85721 United States Department of Physics and Astronomy University of Pennsylvania 209 S 33rd St PhiladelphiaPA19104 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Earth and Planets Laboratory Carnegie Institution for Science 5241 Broad Branch Road NW WashingtonDC20015 United States NSF's National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Exoplanets and Stellar Astrophysics Laboratory NASA Goddard Space Flight Center GreenbeltMD20771 United States Department of Astronomy and Astrophysics Tata Institute of Fundamental Research Homi Bhabha Road Colaba Mumbai400005 India Space Telescope Science Institute 3700 San Martin Dr BaltimoreMD21218 United States Department of Physics and Astronomy Johns Hopkins University 3400 N Charles St BaltimoreMD21218 United States Department of Physics and Astronomy Macquarie University Balaclava Road North RydeNSW2109 Australia Carleton College One North College S

We report the results of observations of p-mode oscillations in the G0 subgiant star HD 35833 in both radial velocities and photometry with NEID and TESS, respectively. We achieve separate, robust detections of the oscillation signal with both instruments (radial velocity amplitude ARV = 1.11 ± 0.09 m s−1, photometric amplitude Aphot = 6.42 ± 0.60 ppm, frequency of maximum power νmax = 595.71 ± 17.28 µHz, and mode spacing ∆ν = 36.65 ± 0.96 µHz) as well as a non-detection in a TESS sector concurrent with the NEID observations. These data shed light on our ability to mitigate the correlated noise impact of oscillations with radial velocities alone, and on the robustness of commonly used asteroseismic scaling relations. The NEID data are used to validate models for the attenuation of oscillation signals for exposure times (Equation presented). and we compare our results to predictions from theoretical scaling relations and find that the observed amplitudes are weaker than expected by > 4σ, hinting at gaps in the underlying physical models. © 2022, CC BY-NC-ND.

关键词： Photometry

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FAIR for AI: An interdisciplinary and international community building perspective

arXiv

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arXiv 2022年

作者： Huerta, E.A. Blaiszik, Ben Brinson, L. Catherine Bouchard, Kristofer E. Diaz, Daniel Doglioni, Caterina Duarte, Javier M. Emani, Murali Foster, Ian Fox, Geoffrey Harris, Philip Heinrich, Lukas Jha, Shantenu Katz, Daniel S. Kindratenko, Volodymyr Kirkpatrick, Christine R. Lassila-Perini, Kati Madduri, Ravi K. Neubauer, Mark S. Psomopoulos, Fotis E. Roy, Avik Rübel, Oliver Zhao, Zhizhen Zhu, Ruike Data Science and Learning Division Argonne National Laboratory LemontIL60439 United States Department of Computer Science University of Chicago ChicagoIL60637 United States Globus University of Chicago ChicagoIL60637 United States Department of Mechanical Engineering and Materials Science Duke University DurhamNC27708 United States Scientific Data Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Biological Systems & Engineering Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Helen Wills Neuroscience Institute University of California Berkeley BerkeleyCA94720 United States Department of Physics University of California La Jolla San DiegoCA92093 United States Lund University Department of Physics Box 118 Lund221 00 Sweden School of Physics & Astronomy The University of Manchester ManchesterM13 9PL United Kingdom Leadership Computing Facility Argonne National Laboratory LemontIL60439 United States Biocomplexity Institute Department of Computer Science University of Virginia CharlottesvilleVA22904 United States Department of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Technical University Munich Arcisstraße 21 München80333 Germany Computational Science Initiative Brookhaven National Laboratory UptonNY11973 United States Electrical and Computer Engineering Rutgers The State University of New Jersey PiscatawayNJ08854 United States National Center for Supercomputing Applications University of Illinois Urbana-Champaign UrbanaIL61801 United States Department of Computer Science University of Illinois at Urbana-Champaign UrbanaIL61801 United States Department of Electrical & Computer Engineering University of Illinois at Urbana-Champaign UrbanaIL61801 United States School of Information Sciences University of Illinois at Urbana-Champaign UrbanaIL61801 United States San Diego Supercomputer Center University of California La Jolla San DiegoCA

A foundational set of findable, accessible, interoperable, and reusable (FAIR) principles were proposed in 2016 as prerequisites for proper data management and stewardship, with the goal of enabling the reusability of scholarly data. The principles were also meant to apply to other digital assets, at a high level, and over time, the FAIR guiding principles have been reinterpreted or extended to include the software, tools, algorithms, and workflows that produce data. FAIR principles are now being adapted in the context of AI models and datasets. Here, we present the perspectives, vision, and experiences of researchers from different countries, disciplines, and backgrounds who are leading the definition and adoption of FAIR principles in their communities of practice, and discuss outcomes that may result from pursuing and incentivizing FAIR AI research. The material for this report builds on the FAIR for AI Workshop held at Argonne National Laboratory on June 7, 2022. Copyright © 2022, The Authors. All rights reserved.

关键词： Information management

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Revisiting the classics: On the evolutionary origin of the "Fe II" and "He/N" spectral classes of novae

arXiv

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arXiv 2023年

作者： Aydi, E. Chomiuk, L. Strader, J. Sokolovsky, K.V. Williams, R.E. Buckley, D.A.H. Ederoclite, A. Izzo, L. Kyer, R. Linford, J.D. Kniazev, A. Metzger, B.D. Mikolajewska, J. Molaro, P. Molina, I. Mukai, K. Munari, U. Orio, M. Panurach, T. Shappee, B.J. Shen, K.J. Sokoloski, J.L. Urquhart, R. Walter, F.M. Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street UrbanaIL61801 United States Sternberg Astronomical Institute Moscow State University Universitetskii pr. 13 Moscow119992 Russia Department of Astronomy & Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA95064 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States South African Astronomical Observatory P.O. Box 9 Observatory7935 South Africa Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa Centro de Estudios de Física del Cosmos de Aragón Plaza San Juan 1 Teruel44001 Spain UK Astronomy Technology Centre Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen Ø2200 Denmark National Radio Astronomy Observatory P.O. Box O SocorroNM87801 United States Southern African Large Telescope Foundation PO Box 9 Observatory7935 South Africa Special Astrophysical Observatory Nizhnij Arkhyz Karachai-Circassia 369167 Russia Department of Physics Columbia Astrophysics Laboratory Columbia University New YorkNY10027 United States Center for Computational Astrophysics Flatiron Institute 162 5th Ave New YorkNY10010 United States Nicolaus Copernicus Astronomical Center Polish Academy of Sciences Bartycka 18 WarsawPL 00-716 Poland INAF-Osservatorio Astronomico di Trieste Via G.B. Tiepolo 11 TriesteI-34143 Italy Institute of Fundamental Physics of the Universe Via Beirut 2 Miramare Trieste Italy CRESST and X-ray Astrophysics Laboratory NASA GSFC GreenbeltMD20771 United States Department of Physics University of Maryland Baltimore County 1000 Hilltop Circle BaltimoreMD21250 United States INAF Astronomical Obs

The optical spectra of novae are characterized by emission lines from the hydrogen Balmer series and either Fe II or He/N, leading to their traditional classification into two spectral classes: "Fe II" and "He/N". For decades, the origins of these spectral features were discussed in the literature in the contexts of different bodies of gas or changes in the opacity of the ejecta, particularly associated with studies by R. E. Williams and S. N. Shore. Here, we revisit these major studies with dedicated, modern data sets, covering the evolution of several novae from early rise to peak all the way to the nebular phase. Our data confirm previous suggestions in the literature that the "Fe II" and "He/N" spectral classes are phases in the spectroscopic evolution of novae driven primarily by changes in the opacity, ionization, and density of the ejecta, and most if not all novae go through at least three spectroscopic phases as their eruptions evolve: an early He/N (phase 1;observed during the early rise to visible peak and characterized by P Cygni lines of He I and N II/III), then an Fe II (phase 2;observed near visible peak and characterized by P Cygni lines of Fe II and O I), and then a later He/N (phase 3;observed during the decline and characterized by emission lines of He I/II, N II/III), before entering the nebular phase. This spectral evolution seems to be ubiquitous across novae, regardless of their speed class;however the duration of each of these phases differs based on the speed class of the nova. © 2023, CC BY-NC-ND.

关键词： Opacity

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The Wide-field Spectroscopic Telescope (WST) Science White Paper

arXiv

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arXiv 2024年

作者： Mainieri, Vincenzo Anderson, Richard I. Brinchmann, Jarle Cimatti, Andrea Ellis, Richard Hill, Vanessa Kneib, Jean-Paul McLeod, Anna Opitom, Cyrielle Roth, Martin M. Sáez, Paula Sánchez Smiljanic, Rodolfo Tolstoy, Eline Bacon, Roland Randich, Sofia Pasquini, Luca Barsanti, Stefania Bryant, Julia Bryson, Ian Casali, Mark Colless, Matthew Couch, Warrick Danielski, Camilla Dierickx, Philippe Driver, Simon Fontana, Adriano Garilli, Bianca de Jong, Roelof S. Lee, David Lehnert, Matt Magrini, Laura Montet, Ben Sanchez-Janssen, Ruben Pandey-Pommier, Mamta Sargent, Mark Schipani, Pietro Steinmetz, Matthias Travouillon, Tony Tresse, Laurence Vernet, Joël Yeche, Christophe Ziegler, Bodo Audard, Marc Arévalo, Patricia Bayo Aran, Amelia M. Bisero, Sofia Bisogni, Susanna Blondin, Stéphane Bonito, Rosaria Branchesi, Marica Catelan, Márcio D'Ammando, Filippo Dainotti, Maria G. De Cia, Annalisa Dhawan, Suhail Dupletsa, Ulyana Hazra, Nandini Ilić, Dragana Ivanov, Valentin D. Izzo, Luca Kovačević, Andjelka B. Kuncarayakti, Hanindyo Kwon, Yuna La Forgia, Fiorangela Lazzarin, Monica Lira, Paulina Loffredo, Eleonora Maguire, Kate Majidi, Fatemeh Z. Marconi, Marcella McGee, Sean Migliorini, Alessandra Minniti, Dante Nicholl, Matt Onori, Francesca Pala, Anna F. Panda, Swayamtrupta Pawlak, Michal Pessi, Priscila J. Popović, Luka Č. Smith, Graham P. Vergani, Susanna D. Vietri, Giustina Ye, Quanzhi Zafar, Tayyaba Matsuno, Tadafumi Kordopatis, Georges Annibali, Francesca Bayo, Amelia Bellazzini, Michele Beltran, Maria Teresa Berni, Leda Bianchi, Simone Biazzo, Katia Bland-Hawthorn, Joss Boffin, Henri M.J. Bono, Giuseppe Bowman, Dominic Braga, Vittorio F. Bragaglia, Angela Brucalassi, Anna Busà, Innocenza Casali, Giada Casasola, Viviana Castro, Norberto Cavallo, Lorenzo Chiappini, Cristina Colzi, Laura Damiani, Francesco da Silva, Ronaldo D'Orazi, Valentina Escorza, Ana Fabrizio, Michele Fiorentino, Giuliana Fontani, Francesco François, Patrick Galindo-Guil, Francisco J. Galli, Daniele Garcia-Rojas, Jorge Guarcello, Mario Giuseppe Helmi, Am European Southern Observatory Karl-Schwarzschild-Strasse 2 Garching bei München85748 Germany Switzerland Instituto de Astrofísica e Ciências do Espaço Universidade do Porto Portugal Dipartimento di Fisica e Astronomia "Augusto Righi" Alma Mater Studiorum Università di Bologna Italy Department of Physics and Astronomy University College London United Kingdom Observatoire de la Côte d'Azur Université Côte d'Azur CNRS Laboratoire Lagrange France Centre for Extragalactic Astronomy Department of Physics Durham University United Kingdom Institute for Computational Cosmology Department of Physics University of Durham United Kingdom Institute for Astronomy University of Edinburgh United Kingdom Germany Nicolaus Copernicus Astronomical Center Polish Academy of Sciences Poland Kapteyn Astronomical Institute University of Groningen Netherlands France INAF - Osservatorio Astrofisico di Arcetri Italy Stockholm University Sweden INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Italy Universidad de Valparaíso Chile University of Geneva Switzerland Research School of Astronomy and Astrophysics Australian National University CanberraACT2611 Australia Australia Instituto de Astrofísica de Canarias Spain Universidad de La Laguna Spain SISSA - Scuola Internazionale Superiore di Studi Avanzati Italy University of Florence Italy INAF - Osservatorio Astronomico di Roma Italy GEPI Observatoire de Paris Universite PSL CNRS France INAF Istituto di Astrofisica Spaziale e Fisica cosmica Milano Italy Sydney Institute for Astronomy School of Physics The University of Sydney Australia Aix Marseille Univ CNRS CNES LAM France INAF - Osservatorio Astronomico di Palermo Italy University of Rome Tor Vergata Italy Newcastle University United Kingdom Italy UK Astronomy Technology Ctr. Royal Observatory Edinburgh United Kingdom INAF OACT Italy Dipartimento di Fisica Università degli Studi di Torino Italy Istituto Nazionale di Fisica Nucleare INFN Sezione di

The WST is proposed as a new facility dedicated to the efficient delivery of spectroscopic surveys and this white paper summarises the initial concept as well as the corresponding science cases. It will provide an end-to-end service from the preparation of surveys to the delivery of high-quality calibrated science data product. Uniquely, it will have the ability to simultaneously deliver fibre-fed multi-object spectroscopy over a large field of view (MOS) and integral field imaging spectroscopy of a central field of 3 × 3 arcmin2 (IFS). WST will fill a crucial gap in the astronomical landscape and will allow full exploitation of major current and upcoming ground and space-based facilities. WST will address outstanding scientific questions in the areas of cosmology;galaxy assembly, evolution, and enrichment, including our own Milky Way;origin of stars and planets;time domain and multi-messenger astrophysics. WST features a 12 meter aperture telescope that covers the UV to the H band and operates in seeing limited conditions. Its field of view (FoV) of 3.1 deg2 will be the largest of any telescope equipped with a MOS. In particular, its FoV is 2.5 times larger than PFS@Subaru and a remarkable 22 times larger than MOONS@VLT. In addition, the WST has a substantial aperture, twice as large (100 square metres) as its 8 meter class competitors. A central circular area with a diameter of 13 arcmin is available for simultaneous IFS observations. Within this area, the IFS with a FoV of 3 × 3 arcmin2 (9 times larger than MUSE@VLT) can be utilised simultaneously with the MOS. In addition, the IFS can be used to mosaic a larger area within the 13 arcmin circle (an area larger than the entire FoV of the ELT) while the MOS positioner can perform multiple configurations. The WST operational model will also implement target of opportunity (ToO) operations at both the telescope and MOS fibre levels to support the time domain science cases. The demand for a facility dedicated to spect

关键词： Telescopes

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Low-latency gravitational wave alert products and their performance at the time of the fourth LIGO-Virgo-KAGRA observing run

arXiv

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arXiv 2023年

作者： Chaudhary, Sushant Sharma Toivonen, Andrew Waratkar, Gaurav Mo, Geoffrey Chatterjee, Deep Antier, Sarah Brockill, Patrick Coughlin, Michael W. Essick, Reed Ghosh, Shaon Morisaki, Soichiro Baral, Pratyusava Baylor, Amanda Adhikari, Naresh Brady, Patrick Davies, Gareth Cabourn Canton, Tito Dal Cavaglia, Marco Creighton, Jolien Choudhary, Sunil Chu, Yu-Kuang Clearwater, Patrick Davis, Luke Dent, Thomas Drago, Marco Ewing, Becca Godwin, Patrick Guo, Weichangfeng Hanna, Chad Huxford, Rachael Harry, Ian Katsavounidis, Erik Kovalam, Manoj Li, Alvin K.Y. Magee, Ryan Marx, Ethan Meacher, Duncan Messick, Cody Morice-Atkinson, Xan Pace, Alexander De Pietri, Roberto Piotrzkowski, Brandon Roy, Soumen Sachdev, Surabhi Singer, Leo P. Singh, Divya Szczepanczyk, Marek Tang, Daniel Trevor, Max Tsukada, Leo Villa-Ortega, Verónica Wen, Linqing Wysocki, Daniel Institute of Multi-messenger Astrophysics and Cosmology Missouri University of Science and Technology Physics Building 1315 N. Pine St. RollaMO65409 United States School of Physics and Astronomy University of Minnesota MinneapolisMN55455 United States Department of Physics IIT Bombay Powai Mumbai400076 India LIGO Laboratory Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 185 Albany Street CambridgeMA02139 United States Artemis Observatoire de la Côte d’Azur Université Côte d’Azur Boulevard de l’Observatoire Nice06304 France Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin-Milwaukee MilwaukeeWI53201 United States Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H8 Canada Department of Physics University of Toronto TorontoONM5S 1A7 Canada David A. Dunlap Department of Astronomy University of Toronto TorontoONM5S 3H4 Canada Montclair State University 1 Normal Ave. MontclairNJ07043 United States Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan University of Portsmouth PortsmouthPO1 3FX United Kingdom Université Paris-Saclay CNRS IN2P3 IJCLab Orsay91405 France University of Wisconsin MilwaukeeWI53211 United States Australia Department of Physics University of Western Australia CrawleyWA6009 Australia IGFAE Universidade de Santiago de Compostela E-15782 Spain Università di Roma La Sapienza RomaI-00133 Italy INFN Sezione di Roma RomaI-00133 Italy Department of Physics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States LIGO Laboratory California Institute of Technology PasadenaCA91125 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States

Multi-messenger searches for binary neutron star (BNS) and neutron star-black hole (NSBH) mergers are currently one of the most exciting areas of astronomy. The search for joint electromagnetic and neutrino counterparts to gravitational wave (GW)s has resumed with Advanced LIGO (aLIGO)’s, Advanced Virgo (AdVirgo)’s and KAGRA’s fourth observing run (O4). To support this effort, public semi-automated data products are sent in near real-time and include localization and source properties to guide complementary observations. In preparation for O4, we have conducted a study using a simulated population of compact binaries and a Mock data Challenge (MDC) in the form of a real-time replay to optimize and profile the software infrastructure and scientific deliverables. End-to-end performance was tested, including data ingestion, running online search pipelines, performing annotations, and issuing alerts to the astrophysics community. We present an overview of the low-latency infrastructure and the performance of the data products that are now being released during O4 based on the MDC. We report the expected median latency for the preliminary alert of full bandwidth searches (29.5 s) and show consistency and accuracy of released data products using the MDC. For the first time, we report the expected median latency for triggers from early warning searches (-3.1 s), which are new in O4 and target neutron star mergers during inspiral phase. This paper provides a performance overview for LVK low-latency alert infrastructure and data products using the MDC and serves as a useful reference for the interpretation of O4 detections. © 2023, CC BY.

关键词： Gravity waves

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