90 research outputs found
Status of the profession
The number of astronomers has grown by about 40 percent over the past decade. The number of astronomers with jobs in industry, or with long-term, non-tenured, jobs has increased dramatically compared with traditional faculty positions. The increase in the number of astronomers and the declining share of the NSF budget going to astronomy has led to extreme difficulties in the NSF grant program and in support of the National Observatories. In 1989, direct NASA support of astronomers through the grants program exceeds that of NSF, although the total of the NSF grants program over decade far exceeds that of NASA. Access to major new telescopes will be important issue for the 1990s. US astronomers, who once had a monopoly on telescopes larger than 3 meters, will, by the year 2000, have access to just half of the world's optical telescope area
Contamination of health care workersâ coats at the University Teaching Hospital in Lusaka, Zambia: the nosocomial risk
The Respiratory Protection Effectiveness Clinical Trial (ResPECT): a cluster-randomized comparison of respirator and medical mask effectiveness against respiratory infections in healthcare personnel
First Sagittarius A Event Horizon Telescope results. IV. Variability, morphology, and black hole mass
REST OF AUTHORS : Dempsey, Jessica; Desvignes, Gregory; Dexter, Jason; Dhruv, Vedant; Doeleman, Sheperd S.; Dougal, Sean; Dzib, Sergio A.; Eatough, Ralph P.; Emami, Razieh; Falcke, Heino; Farah, Joseph; Fish, Vincent L.; Fomalont, Ed; Ford, H. Alyson; Fraga-Encinas, Raquel; Freeman, William T.; Friberg, Per; Fromm, Christian M.; Fuentes, Antonio; Galison, Peter; Gammie, Charles F.; Garcia, Roberto; Gentaz, Olivier; Georgiev, Boris; Goddi, Ciriaco; Gold, Roman; Gomez-Ruiz, Arturo, I; Gomez, Jose L.; Gu, Minfeng; Gurwell, Mark; Hada, Kazuhiro; Haggard, Daryl; Haworth, Kari; Hecht, Michael H.; Hesper, Ronald; Heumann, Dirk; Ho, Luis C.; Ho, Paul; Honma, Mareki; Huang, Chih-Wei L.; Huang, Lei; Hughes, David H.; Ikeda, Shiro; Impellizzeri, C. M. Violette; Inoue, Makoto; Issaoun, Sara; James, David J.; Jannuzi, Buell T.; Janssen, Michael; Jeter, Britton; Jiang, Wu; Jimenez-Rosales, Alejandra; Johnson, Michael D.; Jorstad, Svetlana; Joshi, Abhishek, V; Jung, Taehyun; Karami, Mansour; Karuppusamy, Ramesh; Kawashima, Tomohisa; Keating, Garrett K.; Kettenis, Mark; Kim, Dong-Jin; Kim, Jae-Young; Kim, Jongsoo; Kim, Junhan; Kino, Motoki; Koay, Jun Yi; Kocherlakota, Prashant; Kofuji, Yutaro; Koch, Patrick M.; Koyama, Shoko; Kramer, Carsten; Kramer, Michael; Krichbaum, Thomas P.; Kuo, Cheng-Yu; La Bella, Noemi; Lauer, Tod R.; Lee, Daeyoung; Lee, Sang-Sung; Leung, Po Kin; Levis, Aviad; Li, Zhiyuan; Lico, Rocco; Lindahl, Greg; Lindqvist, Michael; Lisakov, Mikhail; Liu, Jun; Liu, Kuo; Liuzzo, Elisabetta; Lo, Wen-Ping; Lobanov, Andrei P.; Loinard, Laurent; Lonsdale, Colin J.; Lu, Ru-Sen; Mao, Jirong; Marchili, Nicola; Markoff, Sera; Marrone, Daniel P.; Marscher, Alan P.; Marti-Vidal, Ivan; Matsushita, Satoki; Matthews, Lynn D.; Medeiros, Lia; Menten, Karl M.; Michalik, Daniel; Mizuno, Izumi; Mizuno, Yosuke; Moran, James M.; Moriyama, Kotaro; Moscibrodzka, Monika; Muller, Cornelia; Mus, Alejandro; Musoke, Gibwa; Myserlis, Ioannis; Nadolski, Andrew; Nagai, Hiroshi; Nagar, Neil M.; Nakamura, Masanori; Narayan, Ramesh; Narayanan, Gopal; Natarajan, Iniyan; Nathanail, Antonios; Fuentes, Santiago Navarro; Neilsen, Joey; Neri, Roberto; Ni, Chunchong; Noutsos, Aristeidis; Nowak, Michael A.; Oh, Junghwan; Okino, Hiroki; Olivares, Hector; Ortiz-Leon, Gisela N.; Oyama, Tomoaki; Palumbo, Daniel C. M.; Paraschos, Georgios Filippos; Park, Jongho; Parsons, Harriet; Patel, Nimesh; Pen, Ue-Li; Pesce, Dominic W.; Pietu, Vincent; Plambeck, Richard; PopStefanija, Aleksandar; Porth, Oliver; Potzl, Felix M.; Prather, Ben; Preciado-Lopez, Jorge A.; Pu, Hung-Yi; Ramakrishnan, Venkatessh; Rao, Ramprasad; Rawlings, Mark G.; Raymond, Alexander W.; Rezzolla, Luciano; Ricarte, Angelo; Ripperda, Bart; Roelofs, Freek; Rogers, Alan; Ros, Eduardo; Romero-Canizales, Cristina; Roshanineshat, Arash; Rottmann, Helge; Roy, Alan L.; Ruiz, Ignacio; Ruszczyk, Chet; Rygl, Kazi L. J.; Sanchez, Salvador; Sanchez-Arguelles, David; Sanchez-Portal, Miguel; Sasada, Mahito; Satapathy, Kaushik; Savolainen, Tuomas; Schloerb, F. Peter; Schonfeld, Jonathan; Schuster, Karl-Friedrich; Shao, Lijing; Shen, Zhiqiang; Small, Des; Sohn, Bong Won; SooHoo, Jason; Souccar, Kamal; Sun, He; Tazaki, Fumie; Tetarenko, Alexandra J.; Tiede, Paul; Tilanus, Remo P. J.; Titus, Michael; Torne, Pablo; Traianou, Efthalia; Trent, Tyler; Trippe, Sascha; Turk, Matthew; van Bemmel, Ilse; van Langevelde, Huib Jan; van Rossum, Daniel R.; Vos, Jesse; Wagner, Jan; Ward-Thompson, Derek; Wardle, John; Weintroub, Jonathan; Wex, Norbert; Wharton, Robert; Wielgus, Maciek; Wiik, Kaj; Witzel, Gunther; Wondrak, Michael F.; Wong, George N.; Wu, Qingwen; Yamaguchi, Paul; Yoon, Doosoo; Young, Andre; Young, Ken; Younsi, Ziri; Yuan, Feng; Yuan, Ye-Fei; Zensus, J. Anton; Zhang, Shuo; Zhao, Guang-Yao; Zhao, Shan-Shan; Chang, Dominic O.Please read abstract in the article.We thank an anonymous referee for insightful and
constructive comments that helped improve the quality of this
paper.
The Event Horizon Telescope Collaboration thanks the
following organizations and programs: the Academia Sinica;
the Academy of Finland (projects 274477, 284495, 312496,
315721); the Agencia Nacional de InvestigaciĂłn y Desarrollo
(ANID), Chile via NCN19_058 (TITANs) and Fondecyt
1221421, the Alexander von Humboldt Stiftung; an Alfred P.
Sloan Research Fellowship; Allegro, the European ALMA
Regional Centre node in the Netherlands, the NL astronomy
research network NOVA and the astronomy institutes of the
University of Amsterdam, Leiden University and Radboud
University; the ALMA North America Development Fund; the
Black Hole Initiative, which is funded by grants from the John
Templeton Foundation and the Gordon and Betty Moore
Foundation (although the opinions expressed in this work are
those of the author(s) and do not necessarily reflect the views of
these Foundations); Chandra DD7-18089X and TM6-17006X;
the China Scholarship Council; China Postdoctoral Science Foundation fellowship (2020M671266); Consejo Nacional de
Ciencia y TecnologĂa (CONACYT, Mexico, projects U0004-
246083, U0004-259839, F0003-272050, M0037-279006,
F0003-281692, 104497, 275201, 263356); the ConsejerĂa de
EconomĂa, Conocimiento, Empresas y Universidad of the Junta
de AndalucĂa (grant P18-FR-1769), the Consejo Superior de
Investigaciones CientĂficas (grant 2019AEP112); the Delaney
Family via the Delaney Family John A. Wheeler Chair at
Perimeter Institute; DirecciĂłn General de Asuntos del Personal
Académico-Universidad Nacional Autónoma de México
(DGAPA-UNAM, projects IN112417 and IN112820); the
Dutch Organization for Scientific Research (NWO) VICI
award (grant 639.043.513) and grant OCENW.KLEIN.113;
the Dutch National Supercomputers, Cartesius and Snellius
(NWO Grant 2021.013); the EACOA Fellowship awarded by
the East Asia Core Observatories Association, which consists
of the Academia Sinica Institute of Astronomy and Astrophysics,
the National Astronomical Observatory of Japan,
Center for Astronomical Mega-Science, Chinese Academy of
Sciences, and the Korea Astronomy and Space Science
Institute; the European Research Council (ERC) Synergy
Grant âBlackHoleCam: Imaging the Event Horizon of Black
Holesâ (grant 610058); the European Union Horizon 2020
research and innovation programme under grant agreements
RadioNet (No 730562) and M2FINDERS (No 101018682); the
Generalitat Valenciana postdoctoral grant APOSTD/2018/177
and GenT Program (project CIDEGENT/2018/021); MICINN
Research Project PID2019-108995GB-C22; the European
Research Council for advanced grant âJETSET: Launching,
propagation and emission of relativistic jets from binary
mergers and across mass scalesâ (Grant No. 884631); the
Institute for Advanced Study; the Istituto Nazionale di Fisica Nucleare (INFN) sezione di Napoli, iniziative specifiche
TEONGRAV; the International Max Planck Research School
for Astronomy and Astrophysics at the Universities of Bonn
and Cologne; DFG research grant âJet physics on horizon
scales and beyondâ (Grant No. FR 4069/2-1); Joint Princeton/
Flatiron and Joint Columbia/Flatiron Postdoctoral Fellowships,
research at the Flatiron Institute is supported by the Simons
Foundation; the Japan Ministry of Education, Culture, Sports,
Science and Technology (MEXT; grant JPMXP1020200109);
the Japanese Government (Monbukagakusho: MEXT) Scholarship;
the Japan Society for the Promotion of Science (JSPS)
Grant-in-Aid for JSPS Research Fellowship (JP17J08829); the
Joint Institute for Computational Fundamental Science, Japan;
the Key Research Program of Frontier Sciences, Chinese
Academy of Sciences (CAS, grants QYZDJ-SSW-SLH057,
QYZDJSSW-SYS008, ZDBS-LY-SLH011); the Leverhulme
Trust Early Career Research Fellowship; the Max-Planck-
Gesellschaft (MPG); the Max Planck Partner Group of the
MPG and the CAS; the MEXT/JSPS KAKENHI (grants
18KK0090, JP21H01137, JP18H03721, JP18K13594,
18K03709, JP19K14761, 18H01245, 25120007); the Malaysian
Fundamental Research Grant Scheme (FRGS) FRGS/1/
2019/STG02/UM/02/6; the MIT International Science and
Technology Initiatives (MISTI) Funds; the Ministry of Science
and Technology (MOST) of Taiwan (103-2119-M-001-010-
MY2, 105-2112-M-001-025-MY3, 105-2119-M-001-042, 106-
2112-M-001-011, 106-2119-M-001-013, 106-2119-M-001-
027, 106-2923-M-001-005, 107-2119-M-001-017, 107-2119-
M-001-020, 107-2119-M-001-041, 107-2119-M-110-005, 107-2923-M-001-009, 108-2112-M-001-048, 108-2112-M-
001-051, 108-2923-M-001-002, 109-2112-M-001-025, 109-
2124-M-001-005, 109-2923-M-001-001, 110-2112-M-003-
007-MY2, 110-2112-M-001-033, 110-2124-M-001-007, and
110-2923-M-001-001); the Ministry of Education (MoE) of
Taiwan Yushan Young Scholar Program; the Physics Division,
National Center for Theoretical Sciences of Taiwan; the
National Aeronautics and Space Administration (NASA, Fermi
Guest Investigator grant 80NSSC20K1567, NASA Astrophysics
Theory Program grant 80NSSC20K0527, NASA NuSTAR
award 80NSSC20K0645); NASA Hubble Fellowship grant
HST-HF2-51431.001-A awarded by the Space Telescope
Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under
contract NAS5-26555; the National Institute of Natural
Sciences (NINS) of Japan; the National Key Research and
Development Program of China (grant 2016YFA0400704,
2017YFA0402703, 2016YFA0400702); the National Science
Foundation (NSF, grants AST-0096454, AST-0352953, AST-
0521233, AST-0705062, AST-0905844, AST-0922984, AST-
1126433, AST-1140030, DGE-1144085, AST-1207704, AST-
1207730, AST-1207752, MRI-1228509, OPP-1248097, AST-
1310896, AST-1440254, AST-1555365, AST-1614868, AST-
1615796, AST-1715061, AST-1716327, AST-1716536, OISE-
1743747, AST-1816420, AST-1935980, AST-2034306); NSF
Astronomy and Astrophysics Postdoctoral Fellowship (AST-
1903847); the Natural Science Foundation of China (grants
11650110427, 10625314, 11721303, 11725312, 11873028,
11933007, 11991052, 11991053, 12192220, 12192223); the
Natural Sciences and Engineering Research Council of Canada
(NSERC, including a Discovery Grant and the NSERC Alexander Graham Bell Canada Graduate Scholarships-Doctoral
Program); the National Youth Thousand Talents Program
of China; the National Research Foundation of Korea (the
Global PhD Fellowship Grant: grants NRF-
2015H1A2A1033752, the Korea Research Fellowship Program:
NRF-2015H1D3A1066561, Brain Pool Program:
2019H1D3A1A01102564, Basic Research Support Grant
2019R1F1A1059721, 2021R1A6A3A01086420,
2022R1C1C1005255); Netherlands Research School for
Astronomy (NOVA) Virtual Institute of Accretion (VIA)
postdoctoral fellowships; Onsala Space Observatory (OSO)
national infrastructure, for the provisioning of its facilities/
observational support (OSO receives funding through the
Swedish Research Council under grant 2017-00648); the
Perimeter Institute for Theoretical Physics (research at
Perimeter Institute is supported by the Government of Canada
through the Department of Innovation, Science and Economic
Development and by the Province of Ontario through the
Ministry of Research, Innovation and Science); the Spanish
Ministerio de Ciencia e InnovaciĂłn (grants PGC2018-098915-
B-C21, AYA2016-80889-P, PID2019-108995GB-C21,
PID2020-117404GB-C21); the University of Pretoria for
financial aid in the provision of the new Cluster Server nodes
and SuperMicro (USA) for a SEEDING GRANT approved
towards these nodes in 2020; the Shanghai Pilot Program for
Basic Research, Chinese Academy of Science, Shanghai
Branch (JCYJ-SHFY-2021-013); the State Agency for
Research of the Spanish MCIU through the âCenter of
Excellence Severo Ochoaâ award for the Instituto de AstrofĂsica
de AndalucĂa (SEV-2017- 0709); the Spinoza Prize SPI 78-409; the South African Research Chairs Initiative, through
the South African Radio Astronomy Observatory (SARAO,
grant ID 77948), which is a facility of the National Research
Foundation (NRF), an agency of the Department of Science
and Innovation (DSI) of South Africa; the Toray Science
Foundation; Swedish Research Council (VR); the US Department
of Energy (USDOE) through the Los Alamos National
Laboratory (operated by Triad National Security, LLC, for the
National Nuclear Security Administration of the USDOE
(Contract 89233218CNA000001); and the YCAA Prize
Postdoctoral Fellowship. We thank the staff at the participating observatories,
correlation centers, and institutions for their enthusiastic
support. This paper makes use of the following ALMA data:
ADS/JAO.ALMA#2016.1.01154.V. ALMA is a partnership
of the European Southern Observatory (ESO; Europe,
representing its member states), NSF, and National Institutes
of Natural Sciences of Japan, together with National Research
Council (Canada), Ministry of Science and Technology
(MOST; Taiwan), Academia Sinica Institute of Astronomy
and Astrophysics (ASIAA; Taiwan), and Korea Astronomy and
Space Science Institute (KASI; Republic of Korea), in
cooperation with the Republic of Chile. The Joint ALMA
Observatory is operated by ESO, Associated Universities, Inc.
(AUI)/NRAO, and the National Astronomical Observatory of
Japan (NAOJ). The NRAO is a facility of the NSF operated
under cooperative agreement by AUI. This research used
resources of the Oak Ridge Leadership Computing Facility at
the Oak Ridge National Laboratory, which is supported by the
Office of Science of the U.S. Department of Energy under
Contract No. DE-AC05-00OR22725. We also thank the Center
for Computational Astrophysics, National Astronomical Observatory
of Japan. The computing cluster of Shanghai VLBI
correlator supported by the Special Fund for Astronomy from
the Ministry of Finance in China is acknowledged. APEX is a collaboration between the Max-Planck-Institut fĂŒr
Radioastronomie (Germany), ESO, and the Onsala Space
Observatory (Sweden). The SMA is a joint project between the
SAO and ASIAA and is funded by the Smithsonian Institution
and the Academia Sinica. The JCMT is operated by the East
Asian Observatory on behalf of the NAOJ, ASIAA, and KASI,
as well as the Ministry of Finance of China, Chinese Academy
of Sciences, and the National Key Research and Development
Program (No. 2017YFA0402700) of China and Natural
Science Foundation of China grant 11873028. Additional
funding support for the JCMT is provided by the Science and
Technologies Facility Council (UK) and participating universities
in the UK and Canada. The LMT is a project operated
by the Instituto Nacional de AstrĂłfisica, Ăptica, y ElectrĂłnica
(Mexico) and the University of Massachusetts at Amherst
(USA). The IRAM 30-m telescope on Pico Veleta, Spain is
operated by IRAM and supported by CNRS (Centre National
de la Recherche Scientifique, France), MPG (Max-Planck-
Gesellschaft, Germany) and IGN (Instituto GeogrĂĄfico Nacional,
Spain). The SMT is operated by the Arizona Radio
Observatory, a part of the Steward Observatory of the
University of Arizona, with financial support of operations
from the State of Arizona and financial support for instrumentation
development from the NSF. Support for SPT participation
in the EHT is provided by the National Science Foundation
through award OPP-1852617 to the University of Chicago. Partial support is also provided by the Kavli Institute of
Cosmological Physics at the University of Chicago. The SPT
hydrogen maser was provided on loan from the GLT, courtesy
of ASIAA.
This work used the Extreme Science and Engineering
Discovery Environment (XSEDE), supported by NSF grant
ACI-1548562, and CyVerse, supported by NSF grants DBI-
0735191, DBI-1265383, and DBI-1743442. XSEDE Stampede2
resource at TACC was allocated through TG-AST170024 and
TG-AST080026N. XSEDE JetStream resource at PTI and
TACC was allocated through AST170028. This research is part
of the Frontera computing project at the Texas Advanced
Computing Center through the Frontera Large-Scale Community
Partnerships allocation AST20023. Frontera is made possible by
National Science Foundation award OAC-1818253. This
research was carried out using resources provided by the Open
Science Grid, which is supported by the National Science
Foundation and the U.S. Department of Energy Office of
Science. Additional work used ABACUS2.0, which is part of
the eScience center at Southern Denmark University. Simulations
were also performed on the SuperMUC cluster at the LRZ
in Garching, on the LOEWE cluster in CSC in Frankfurt, on the
HazelHen cluster at the HLRS in Stuttgart, and on the Pi2.0 and
Siyuan Mark-I at Shanghai Jiao Tong University. The computer
resources of the Finnish IT Center for Science (CSC) and the
Finnish Computing Competence Infrastructure (FCCI) project
are acknowledged. This research was enabled in part by support
provided by Compute Ontario (http://computeontario.ca),
Calcul Quebec (http://www.calculquebec.ca) and Compute
Canada (http://www.computecanada.ca).
The EHTC has received generous donations of FPGA chips
from Xilinx Inc., under the Xilinx University Program. The EHTC has benefited from technology shared under open-source
license by the Collaboration for Astronomy Signal Processing and
Electronics Research (CASPER). The EHT project is grateful to
T4Science and Microsemi for their assistance with Hydrogen
Masers. This research has made use of NASAÊŒs Astrophysics
Data System. We gratefully acknowledge the support provided by
the extended staff of the ALMA, both from the inception of the
ALMA Phasing Project through the observational campaigns of
2017 and 2018. We would like to thank A. Deller and W. Brisken
for EHT-specific support with the use of DiFX. We thank Martin
Shepherd for the addition of extra features in the Difmap software
that were used for the CLEAN imaging results presented in this
paper. We acknowledge the significance that Maunakea, where
the SMA and JCMT EHT stations are located, has for the
indigenous Hawaiian people. IMV acknowledges the use of LLuis
Vives HPC resources of the University of Valencia.http://iopscience.iop.org/2041-8205am2023Physic
The development and validation of a scoring tool to predict the operative duration of elective laparoscopic cholecystectomy
Background: The ability to accurately predict operative duration has the potential to optimise theatre efficiency and utilisation, thus reducing costs and increasing staff and patient satisfaction. With laparoscopic cholecystectomy being one of the most commonly performed procedures worldwide, a tool to predict operative duration could be extremely beneficial to healthcare organisations.
Methods: Data collected from the CholeS study on patients undergoing cholecystectomy in UK and Irish hospitals between 04/2014 and 05/2014 were used to study operative duration. A multivariable binary logistic regression model was produced in order to identify significant independent predictors of long (>â90 min) operations. The resulting model was converted to a risk score, which was subsequently validated on second cohort of patients using ROC curves.
Results: After exclusions, data were available for 7227 patients in the derivation (CholeS) cohort. The median operative duration was 60 min (interquartile range 45â85), with 17.7% of operations lasting longer than 90 min. Ten factors were found to be significant independent predictors of operative durations >â90 min, including ASA, age, previous surgical admissions, BMI, gallbladder wall thickness and CBD diameter. A risk score was then produced from these factors, and applied to a cohort of 2405 patients from a tertiary centre for external validation. This returned an area under the ROC curve of 0.708 (SEâ=â0.013, pââ90 min increasing more than eightfold from 5.1 to 41.8% in the extremes of the score.
Conclusion: The scoring tool produced in this study was found to be significantly predictive of long operative durations on validation in an external cohort. As such, the tool may have the potential to enable organisations to better organise theatre lists and deliver greater efficiencies in care
First Sagittarius A Event Horizon Telescope results. VI. Testing the black hole metric
REST OF AUTHORS : Dempsey, Jessica; Desvignes, Gregory; Dexter, Jason; Dhruv, Vedant; Doeleman, Sheperd S.; Dougal, Sean; Dzib, Sergio A.; Eatough, Ralph P.; Emami, Razieh; Falcke, Heino; Farah, Joseph; Fish, Vincent L.; Fomalont, Ed; Ford, H. Alyson; Fraga-Encinas, Raquel; Freeman, William T.; Friberg, Per; Fromm, Christian M.; Fuentes, Antonio; Galison, Peter; Gammie, Charles F.; Garcia, Roberto; Gentaz, Olivier; Georgiev, Boris; Goddi, Ciriaco; Gold, Roman; Gomez-Ruiz, Arturo, I; Gomez, Jose L.; Gu, Minfeng; Gurwell, Mark; Hada, Kazuhiro; Haggard, Daryl; Haworth, Kari; Hecht, Michael H.; Hesper, Ronald; Heumann, Dirk; Ho, Luis C.; Ho, Paul; Honma, Mareki; Huang, Chih-Wei L.; Huang, Lei; Hughes, David H.; Ikeda, Shiro; Impellizzeri, C. M. Violette; Inoue, Makoto; Issaoun, Sara; James, David J.; Jannuzi, Buell T.; Janssen, Michael; Jeter, Britton; Jiang, Wu; Jimenez-Rosales, Alejandra; Johnson, Michael D.; Jorstad, Svetlana; Joshi, Abhishek, V; Jung, Taehyun; Karami, Mansour; Karuppusamy, Ramesh; Kawashima, Tomohisa; Keating, Garrett K.; Kettenis, Mark; Kim, Dong-Jin; Kim, Jae-Young; Kim, Jongsoo; Kim, Junhan; Kino, Motoki; Koay, Jun Yi; Kocherlakota, Prashant; Kofuji, Yutaro; Koch, Patrick M.; Koyama, Shoko; Kramer, Carsten; Kramer, Michael; Krichbaum, Thomas P.; Kuo, Cheng-Yu; La Bella, Noemi; Lauer, Tod R.; Lee, Daeyoung; Lee, Sang-Sung; Leung, Po Kin; Levis, Aviad; Li, Zhiyuan; Lico, Rocco; Lindahl, Greg; Lindqvist, Michael; Lisakov, Mikhail; Liu, Jun; Liu, Kuo; Liuzzo, Elisabetta; Lo, Wen-Ping; Lobanov, Andrei P.; Loinard, Laurent; Lonsdale, Colin J.; Lu, Ru-Sen; Mao, Jirong; Marchili, Nicola; Markoff, Sera; Marrone, Daniel P.; Marscher, Alan P.; Marti-Vidal, Ivan; Matsushita, Satoki; Matthews, Lynn D.; Medeiros, Lia; Menten, Karl M.; Michalik, Daniel; Mizuno, Izumi; Mizuno, Yosuke; Moran, James M.; Moriyama, Kotaro; Moscibrodzka, Monika; Muller, Cornelia; Mus, Alejandro; Musoke, Gibwa; Myserlis, Ioannis; Nadolski, Andrew; Nagai, Hiroshi; Nagar, Neil M.; Nakamura, Masanori; Narayan, Ramesh; Narayanan, Gopal; Natarajan, Iniyan; Nathanail, Antonios; Fuentes, Santiago Navarro; Neilsen, Joey; Neri, Roberto; Ni, Chunchong; Noutsos, Aristeidis; Nowak, Michael A.; Oh, Junghwan; Okino, Hiroki; Olivares, Hector; Ortiz-Leon, Gisela N.; Oyama, Tomoaki; Ozel, Feryal; Palumbo, Daniel C. M.; Paraschos, Georgios Filippos; Park, Jongho; Parsons, Harriet; Patel, Nimesh; Pen, Ue-Li; Pesce, Dominic W.; Pietu, Vincent; Plambeck, Richard; PopStefanija, Aleksandar; Porth, Oliver; Potzl, Felix M.; Prather, Ben; Preciado-Lopez, Jorge A.; Psaltis, Dimitrios; Pu, Hung-Yi; Ramakrishnan, Venkatessh; Rao, Ramprasad; Rawlings, Mark G.; Raymond, Alexander W.; Rezzolla, Luciano; Ricarte, Angelo; Ripperda, Bart; Roelofs, Freek; Rogers, Alan; Ros, Eduardo; Romero-Canizales, Cristina; Roshanineshat, Arash; Rottmann, Helge; Roy, Alan L.; Ruiz, Ignacio; Ruszczyk, Chet; Rygl, Kazi L. J.; Sanchez, Salvador; Sanchez-Arguelles, David; Sanchez-Portal, Miguel; Sasada, Mahito; Satapathy, Kaushik; Savolainen, Tuomas; Schloerb, F. Peter; Schonfeld, Jonathan; Schuster, Karl-Friedrich; Shao, Lijing; Shen, Zhiqiang; Small, Des; Sohn, Bong Won; SooHoo, Jason; Souccar, Kamal; Sun, He; Tazaki, Fumie; Tetarenko, Alexandra J.; Tiede, Paul; Tilanus, Remo P. J.; Titus, Michael; Torne, Pablo; Traianou, Efthalia; Trent, Tyler; Trippe, Sascha; Turk, Matthew; van Bemmel, Ilse; van Langevelde, Huib Jan; van Rossum, Daniel R.; Vos, Jesse; Wagner, Jan; Ward-Thompson, Derek; Wardle, John; Weintroub, Jonathan; Wex, Norbert; Wharton, Robert; Wielgus, Maciek; Wiik, Kaj; Witzel, Gunther; Wondrak, Michael F.; Wong, George N.; Wu, Qingwen; Yamaguchi, Paul; Yoon, Doosoo; Young, Andre; Young, Ken; Younsi, Ziri; Yuan, Feng; Yuan, Ye-Fei; Zensus, J. Anton; Zhang, Shuo; Zhao, Guang-Yao; Zhao, Shan-Shan.Astrophysical black holes are expected to be described by the Kerr metric. This is the only stationary, vacuum,
axisymmetric metric, without electromagnetic charge, that satisfies Einsteinâs equations and does not have
pathologies outside of the event horizon. We present new constraints on potential deviations from the Kerr
prediction based on 2017 EHT observations of Sagittarius A* (Sgr A*). We calibrate the relationship between the
geometrically defined black hole shadow and the observed size of the ring-like images using a library that includes
both Kerr and non-Kerr simulations. We use the exquisite prior constraints on the mass-to-distance ratio for Sgr A*
to show that the observed image size is within âŒ10% of the Kerr predictions. We use these bounds to constrain
metrics that are parametrically different from Kerr, as well as the charges of several known spacetimes. To consider
alternatives to the presence of an event horizon, we explore the possibility that Sgr A* is a compact object with a
surface that either absorbs and thermally reemits incident radiation or partially reflects it. Using the observed image
size and the broadband spectrum of Sgr A*, we conclude that a thermal surface can be ruled out and a fully
reflective one is unlikely. We compare our results to the broader landscape of gravitational tests. Together with the
bounds found for stellar-mass black holes and the M87 black hole, our observations provide further support that
the external spacetimes of all black holes are described by the Kerr metric, independent of their mass.The authors thank the anonymous referee for comments that
improved the manuscript.
The Event Horizon Telescope Collaboration thanks the
following organizations and programs: the Academia Sinica;
the Academy of Finland (projects 274477, 284495, 312496,
315721); the Agencia Nacional de InvestigaciĂłn y Desarrollo
(ANID), Chile via NCN19_058 (TITANs) and Fondecyt
1221421, the Alexander von Humboldt Stiftung; an Alfred P.
Sloan Research Fellowship; Allegro, the European ALMA
Regional Centre node in the Netherlands, the NL astronomy
research network NOVA and the astronomy institutes of the
University of Amsterdam, Leiden University and Radboud
University; the ALMA North America Development Fund; the
Black Hole Initiative, which is funded by grants from the John
Templeton Foundation and the Gordon and Betty Moore
Foundation (although the opinions expressed in this work are
those of the author(s) and do not necessarily reflect the views of
these Foundations); Chandra DD7-18089X and TM6-17006X;
the China Scholarship Council; China Postdoctoral Science
Foundation fellowship (2020M671266); Consejo Nacional de
Ciencia y TecnologĂa (CONACYT, Mexico, projects U0004-
246083, U0004-259839, F0003-272050, M0037-279006,
F0003-281692, 104497, 275201, 263356); the ConsejerĂa de
EconomĂa, Conocimiento, Empresas y Universidad of the Junta
de AndalucĂa (grant P18-FR-1769), the Consejo Superior de Investigaciones CientĂficas (grant 2019AEP112); the Delaney
Family via the Delaney Family John A. Wheeler Chair at
Perimeter Institute; DirecciĂłn General de Asuntos del Personal
Académico-Universidad Nacional Autónoma de México
(DGAPA-UNAM, projects IN112417 and IN112820); the
Dutch Organization for Scientific Research (NWO) VICI
award (grant 639.043.513) and grant OCENW.KLEIN.113;
the Dutch National Supercomputers, Cartesius and Snellius
(NWO Grant 2021.013); the EACOA Fellowship awarded by
the East Asia Core Observatories Association, which consists
of the Academia Sinica Institute of Astronomy and Astrophysics,
the National Astronomical Observatory of Japan,
Center for Astronomical Mega-Science, Chinese Academy of
Sciences, and the Korea Astronomy and Space Science
Institute; the European Research Council (ERC) Synergy
Grant âBlackHoleCam: Imaging the Event Horizon of Black
Holesâ (grant 610058); the European Union Horizon 2020
research and innovation programme under grant agreements
RadioNet (No 730562) and M2FINDERS (No 101018682); the
Generalitat Valenciana postdoctoral grant APOSTD/2018/177
and GenT Program (project CIDEGENT/2018/021); MICINN
Research Project PID2019-108995GB-C22; the European
Research Council for advanced grant âJETSET: Launching,
propagation and emission of relativistic jets from binary
mergers and across mass scalesâ (Grant No. 884631); the
Institute for Advanced Study; the Istituto Nazionale di Fisica
Nucleare (INFN) sezione di Napoli, iniziative specifiche
TEONGRAV; the International Max Planck Research School
for Astronomy and Astrophysics at the Universities of Bonn
and Cologne; DFG research grant âJet physics on horizon
scales and beyondâ (Grant No. FR 4069/2-1); Joint Princeton/
Flatiron and Joint Columbia/Flatiron Postdoctoral Fellowships,
research at the Flatiron Institute is supported by the Simons
Foundation; the Japan Ministry of Education, Culture, Sports,
Science and Technology (MEXT; grant JPMXP1020200109);
the Japanese Government (Monbukagakusho: MEXT) Scholarship;
the Japan Society for the Promotion of Science (JSPS)
Grant-in-Aid for JSPS Research Fellowship (JP17J08829); the
Joint Institute for Computational Fundamental Science, Japan;
the Key Research Program of Frontier Sciences, Chinese
Academy of Sciences (CAS, grants QYZDJ-SSW-SLH057,
QYZDJSSW-SYS008, ZDBS-LY-SLH011); the Leverhulme
Trust Early Career Research Fellowship; the Max-Planck-
Gesellschaft (MPG); the Max Planck Partner Group of the
MPG and the CAS; the MEXT/JSPS KAKENHI (grants
18KK0090, JP21H01137, JP18H03721, JP18K13594,
18K03709, JP19K14761, 18H01245, 25120007); the Malaysian
Fundamental Research Grant Scheme (FRGS) FRGS/1/
2019/STG02/UM/02/6; the MIT International Science and
Technology Initiatives (MISTI) Funds; the Ministry of Science
and Technology (MOST) of Taiwan (103-2119-M-001-010-
MY2, 105-2112-M-001-025-MY3, 105-2119-M-001-042, 106-
2112-M-001-011, 106-2119-M-001-013, 106-2119-M-001-
027, 106-2923-M-001-005, 107-2119-M-001-017, 107-2119-
M-001-020, 107-2119-M-001-041, 107-2119-M-110-005, 107-
2923-M-001-009, 108-2112-M-001-048, 108-2112-M-001-
051, 108-2923-M-001-002, 109-2112-M-001-025, 109-2124-
M-001-005, 109-2923-M-001-001, 110-2112-M-003-007-
MY2, 110-2112-M-001-033, 110-2124-M-001-007, and 110-
2923-M-001-001); the Ministry of Education (MoE) of Taiwan
Yushan Young Scholar Program; the Physics Division,
National Center for Theoretical Sciences of Taiwan; the
National Aeronautics and Space Administration (NASA, Fermi
Guest Investigator grant 80NSSC20K1567, NASA Astrophysics
Theory Program grant 80NSSC20K0527, NASA NuSTAR
award 80NSSC20K0645); NASA Hubble Fellowship grant
HST-HF2-51431.001-A awarded by the Space Telescope
Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under
contract NAS5-26555; the National Institute of Natural
Sciences (NINS) of Japan; the National Key Research and
Development Program of China (grant 2016YFA0400704,
2017YFA0402703, 2016YFA0400702); the National Science
Foundation (NSF, grants AST-0096454, AST-0352953, AST-
0521233, AST-0705062, AST-0905844, AST-0922984, AST-
1126433, AST-1140030, DGE-1144085, AST-1207704, AST-
1207730, AST-1207752, MRI-1228509, OPP-1248097, AST-
1310896, AST-1440254, AST-1555365, AST-1614868, AST-
1615796, AST-1715061, AST-1716327, AST-1716536, OISE-
1743747, AST-1816420, AST-1935980, AST-2034306); NSF
Astronomy and Astrophysics Postdoctoral Fellowship (AST-
1903847); the Natural Science Foundation of China (grants
11650110427, 10625314, 11721303, 11725312, 11873028,
11933007, 11991052, 11991053, 12192220, 12192223); the
Natural Sciences and Engineering Research Council of Canada
(NSERC, including a Discovery Grant and the NSERC Alexander Graham Bell Canada Graduate Scholarships-Doctoral
Program); the National Youth Thousand Talents Program
of China; the National Research Foundation of Korea (the
Global PhD Fellowship Grant: grants NRF-
2015H1A2A1033752, the Korea Research Fellowship Program:
NRF-2015H1D3A1066561, Brain Pool Program:
2019H1D3A1A01102564, Basic Research Support Grant
2019R1F1A1059721, 2021R1A6A3A01086420,
2022R1C1C1005255); Netherlands Research School for
Astronomy (NOVA) Virtual Institute of Accretion (VIA)
postdoctoral fellowships; Onsala Space Observatory (OSO)
national infrastructure, for the provisioning of its facilities/
observational support (OSO receives funding through the
Swedish Research Council under grant 2017-00648); the
Perimeter Institute for Theoretical Physics (research at
Perimeter Institute is supported by the Government of Canada
through the Department of Innovation, Science and Economic
Development and by the Province of Ontario through the
Ministry of Research, Innovation and Science); the Spanish
Ministerio de Ciencia e InnovaciĂłn (grants PGC2018-098915-
B-C21, AYA2016-80889-P, PID2019-108995GB-C21,
PID2020-117404GB-C21); the University of Pretoria for
financial aid in the provision of the new Cluster Server nodes
and SuperMicro (USA) for a SEEDING GRANT approved
towards these nodes in 2020; the Shanghai Pilot Program for
Basic Research, Chinese Academy of Science, Shanghai
Branch (JCYJ-SHFY-2021-013); the State Agency for
Research of the Spanish MCIU through the âCenter of
Excellence Severo Ochoaâ award for the Instituto de AstrofĂsica
de AndalucĂa (SEV-2017-0709); the Spinoza Prize SPI
78-409; the South African Research Chairs Initiative, through
the South African Radio Astronomy Observatory (SARAO,
grant ID 77948), which is a facility of the National Research
Foundation (NRF), an agency of the Department of Science
and Innovation (DSI) of South Africa; the Toray Science
Foundation; Swedish Research Council (VR); the US Department
of Energy (USDOE) through the Los Alamos National
Laboratory (operated by Triad National Security, LLC, for the
National Nuclear Security Administration of the USDOE
(Contract 89233218CNA000001); and the YCAA Prize
Postdoctoral Fellowship.
We thank the staff at the participating observatories,
correlation centers, and institutions for their enthusiastic
support. This paper makes use of the following ALMA data:
ADS/JAO.ALMA#2016.1.01154.V. ALMA is a partnership
of the European Southern Observatory (ESO; Europe,
representing its member states), NSF, and National Institutes
of Natural Sciences of Japan, together with National Research
Council (Canada), Ministry of Science and Technology
(MOST; Taiwan), Academia Sinica Institute of Astronomy
and Astrophysics (ASIAA; Taiwan), and Korea Astronomy and
Space Science Institute (KASI; Republic of Korea), in
cooperation with the Republic of Chile. The Joint ALMA
Observatory is operated by ESO, Associated Universities, Inc.
(AUI)/NRAO, and the National Astronomical Observatory of
Japan (NAOJ). The NRAO is a facility of the NSF operated
under cooperative agreement by AUI. This research used
resources of the Oak Ridge Leadership Computing Facility at
the Oak Ridge National Laboratory, which is supported by the
Office of Science of the U.S. Department of Energy under
Contract No. DE-AC05-00OR22725. We also thank the
Center for Computational Astrophysics, National Astronomical
Observatory of Japan. The computing cluster of Shanghai
VLBI correlator supported by the Special Fund for Astronomy
from the Ministry of Finance in China is acknowledged.
APEX is a collaboration between the Max-Planck-Institut fĂŒr
Radioastronomie (Germany), ESO, and the Onsala Space
Observatory (Sweden). The SMA is a joint project between the
SAO and ASIAA and is funded by the Smithsonian Institution
and the Academia Sinica. The JCMT is operated by the East
Asian Observatory on behalf of the NAOJ, ASIAA, and KASI,
as well as the Ministry of Finance of China, Chinese Academy
of Sciences, and the National Key Research and Development
Program (No. 2017YFA0402700) of China and Natural
Science Foundation of China grant 11873028. Additional
funding support for the JCMT is provided by the Science and
Technologies Facility Council (UK) and participating universities
in the UK and Canada. The LMT is a project operated
by the Instituto Nacional de AstrĂłfisica, Ăptica, y ElectrĂłnica
(Mexico) and the University of Massachusetts at Amherst
(USA). The IRAM 30-m telescope on Pico Veleta, Spain is
operated by IRAM and supported by CNRS (Centre National
de la Recherche Scientifique, France), MPG (Max-Planck-
Gesellschaft, Germany) and IGN (Instituto GeogrĂĄfico Nacional,
Spain). The SMT is operated by the Arizona Radio
Observatory, a part of the Steward Observatory of the University of Arizona, with financial support of operations from the State of
Arizona and financial support for instrumentation development
from the NSF. Support for SPT participation in the EHT is
provided by the National Science Foundation through award
OPP-1852617 to the University of Chicago. Partial support is
also provided by the Kavli Institute of Cosmological Physics at
the University of Chicago. The SPT hydrogen maser was
provided on loan from the GLT, courtesy of ASIAA.
This work used the Extreme Science and Engineering
Discovery Environment (XSEDE), supported by NSF grant
ACI-1548562, and CyVerse, supported by NSF grants DBI-
0735191, DBI-1265383, and DBI-1743442. XSEDE Stampede2
resource at TACC was allocated through TGAST170024
and TG-AST080026N. XSEDE JetStream
resource at PTI and TACC was allocated through
AST170028. This research is part of the Frontera computing
project at the Texas Advanced Computing Center through the
Frontera Large-Scale Community Partnerships allocation
AST20023. Frontera is made possible by National Science
Foundation award OAC-1818253. This research was carried
out using resources provided by the Open Science Grid, which
is supported by the National Science Foundation and the U.S.
Department of Energy Office of Science. Additional work used ABACUS2.0, which is part of the
eScience center at Southern Denmark University. Simulations
were also performed on the SuperMUC cluster at the LRZ in
Garching, on the LOEWE cluster in CSC in Frankfurt, on the
HazelHen cluster at the HLRS in Stuttgart, and on the Pi2.0 and
Siyuan Mark-I at Shanghai Jiao Tong University. The computer
resources of the Finnish IT Center for Science (CSC) and the
Finnish Computing Competence Infrastructure (FCCI) project
are acknowledged. This research was enabled in part by support
provided by Compute Ontario (http://computeontario.ca),
Calcul Quebec (http://www.calculquebec.ca) and Compute
Canada (http://www.computecanada.ca).
The EHTC has received generous donations of FPGA chips
from Xilinx Inc., under the Xilinx University Program. The
EHTC has benefited from technology shared under open-source license by the Collaboration for Astronomy Signal Processing and
Electronics Research (CASPER). The EHT project is grateful to
T4Science and Microsemi for their assistance with Hydrogen
Masers. This research has made use of NASAÊŒs Astrophysics
Data System. We gratefully acknowledge the support provided by
the extended staff of the ALMA, both from the inception of the
ALMA Phasing Project through the observational campaigns of
2017 and 2018. We would like to thank A. Deller and W. Brisken
for EHT-specific support with the use of DiFX. We thank Martin
Shepherd for the addition of extra features in the Difmap software
that were used for the CLEAN imaging results presented in this
paper. We acknowledge the significance that Maunakea, where
the SMA and JCMT EHT stations are located, has for the
indigenous Hawaiian people. IMV acknowledges the use of LLuis
Vives HPC resources of the University of Valencia.http://iopscience.iop.org/2041-8205am2023Physic
Adjunctive rifampicin for Staphylococcus aureus bacteraemia (ARREST): a multicentre, randomised, double-blind, placebo-controlled trial.
BACKGROUND: Staphylococcus aureus bacteraemia is a common cause of severe community-acquired and hospital-acquired infection worldwide. We tested the hypothesis that adjunctive rifampicin would reduce bacteriologically confirmed treatment failure or disease recurrence, or death, by enhancing early S aureus killing, sterilising infected foci and blood faster, and reducing risks of dissemination and metastatic infection. METHODS: In this multicentre, randomised, double-blind, placebo-controlled trial, adults (â„18 years) with S aureus bacteraemia who had received â€96 h of active antibiotic therapy were recruited from 29 UK hospitals. Patients were randomly assigned (1:1) via a computer-generated sequential randomisation list to receive 2 weeks of adjunctive rifampicin (600 mg or 900 mg per day according to weight, oral or intravenous) versus identical placebo, together with standard antibiotic therapy. Randomisation was stratified by centre. Patients, investigators, and those caring for the patients were masked to group allocation. The primary outcome was time to bacteriologically confirmed treatment failure or disease recurrence, or death (all-cause), from randomisation to 12 weeks, adjudicated by an independent review committee masked to the treatment. Analysis was intention to treat. This trial was registered, number ISRCTN37666216, and is closed to new participants. FINDINGS: Between Dec 10, 2012, and Oct 25, 2016, 758 eligible participants were randomly assigned: 370 to rifampicin and 388 to placebo. 485 (64%) participants had community-acquired S aureus infections, and 132 (17%) had nosocomial S aureus infections. 47 (6%) had meticillin-resistant infections. 301 (40%) participants had an initial deep infection focus. Standard antibiotics were given for 29 (IQR 18-45) days; 619 (82%) participants received flucloxacillin. By week 12, 62 (17%) of participants who received rifampicin versus 71 (18%) who received placebo experienced treatment failure or disease recurrence, or died (absolute risk difference -1·4%, 95% CI -7·0 to 4·3; hazard ratio 0·96, 0·68-1·35, p=0·81). From randomisation to 12 weeks, no evidence of differences in serious (p=0·17) or grade 3-4 (p=0·36) adverse events were observed; however, 63 (17%) participants in the rifampicin group versus 39 (10%) in the placebo group had antibiotic or trial drug-modifying adverse events (p=0·004), and 24 (6%) versus six (2%) had drug interactions (p=0·0005). INTERPRETATION: Adjunctive rifampicin provided no overall benefit over standard antibiotic therapy in adults with S aureus bacteraemia. FUNDING: UK National Institute for Health Research Health Technology Assessment
Constraints on black-hole charges with the 2017 EHT observations of M87*
Our understanding of strong gravity near supermassive compact objects has recently improved thanks to the measurements made by the Event Horizon Telescope (EHT). We use here the M87* shadow size to infer constraints on the physical charges of a large variety of nonrotating or rotating black holes. For example, we show that the quality of the measurements is already sufficient to rule out that M87* is a highly charged dilaton black hole. Similarly, when considering black holes with two physical and independent charges, we are able to exclude considerable regions of the space of parameters for the doubly-charged dilaton and the Sen black holes.This paper has made use of the following APEX data: Project ID T-091.F-0006- 2013. APEX is a collaboration between the Max-Planck- Institut fĂŒr Radioastronomie (Germany), ESO, and the Onsala Space Observatory (Sweden).The Academy of Finland; the Alexander von Humboldt Stiftung; Agencia Nacional de InvestigaciĂłn y Desarrollo (ANID), Chile ; an Alfred P. Sloan Research Fellowship; Allegro, the European ALMA Regional Centre node in the Netherlands, the NL astronomy research network NOVA and the astronomy institutes of the University of Amsterdam, Leiden University and Radboud University; the Black Hole Initiative at Harvard University, through a grant from the John Templeton Foundation; the China Scholarship Council; Consejo Nacional de Ciencia y TecnologĂa (CONACYT); the Delaney Family via the Delaney Family John A.Wheeler Chair at Perimeter Institute; DirecciĂłn General de Asuntos del Personal Academico-Universidad Nacional AutĂłnomade Mexico (DGAPA-UNAM); the EACOA Fellowship of the East Asia Core Observatories Association; the European Research Council Synergy Grant âBlackHoleCam: Imaging the Event Horizon of Black Holesâ; the Generalitat Valenciana postdoctoral grant; MICINN Research Project No. PID2019-108995GB-C22; the Gordon and Betty Moore Foundation; the Istituto Nazionale di Fisica Nucleare (INFN) sezione di Napoli, iniziative specifiche TEONGRAV; the International Max Planck Research School for Astronomy and Astrophysics at the Universities of Bonn and Cologne; Joint Princeton/ Flatiron and Joint Columbia/Flatiron Postdoctoral Fellowships, research at the Flatiron Institute is supported by the Simons Foundation; the Japanese Government (Monbukagakusho: MEXT) Scholarship; the Japan Society for the Promotion of Science (JSPS) Grant-in- Aid for JSPS Research Fellowship; the Key Research Program of Frontier Sciences, Chinese Academy of Sciences (CAS); the Lever-hulme Trust Early Career Research Fellowship; the Max-Planck-Gesellschaft (MPG); the Max Planck Partner Group of the MPG and the CAS; the MEXT/JSPS KAKENHI; the Malaysian Fundamental Research Grant Scheme (FRGS); the MIT International Science and Technology Initiatives (MISTI) Funds; the Ministry of Science and Technology (MOST) of Taiwan; the National Aeronautics and Space Administration (NASA); the National Institute of Natural Sciences (NINS) of Japan; the National Key Research and Development Program of China; the National Science Foundation (NSF); the Natural Science Foundation of China); a fellowship of China Postdoctoral Science Foundation; the Natural Sciences and Engineering Research Council of Canada (NSERC, including a Discovery Grant and the NSERC Alexander Graham Bell Canada Graduate Scholarships-Doctoral Program); the National Research Foundation of Korea; the Netherlands Organization for Scientific Research (NWO) VICI award and Spinoza Prize SPI 78-409; the New Scientific Frontiers with Precision Radio Interferometry Fellowship awarded by the South African Radio Astronomy Observatory (SARAO), which is a facility of the National Research Foundation (NRF), an agency of the Department of Science and Innovation (DSI) of South Africa; the South African Research Chairs Initiative of the Department of Science and Innovation and National Research Foundation; the Onsala Space Observatory (OSO) national infrastructure, for the provisioning of its facilities/observational support (OSO receives funding through the Swedish Research Council under Grant No. 2017-00648) the Perimeter Institute for Theoretical Physics (research at Perimeter Institute is supported by the Government of Canada through the Department of Innovation, Science and Economic Development and by the Province of Ontario through the Ministry of Research, Innovation and Science); the Spanish Ministerio de Ciencia e InnovaciĂłn; the State Agency for Research of the Spanish MCIU through the âCenter of Excellence Severo Ochoaâ award for the Instituto de AstrofĂsica de AndalucĂa); the Toray Science Foundation; the ConsejerĂa de EconomĂa, Conocimiento, Empresas y Universidad, Junta de AndalucĂa, the Consejo Superior de Investigaciones CientĂficas; the U.S. Department of Energy (USDOE) through the Los Alamos National Laboratory (operated by Triad National Security, LLC, for the National Nuclear Security Administration of the USDOE (Contract No. 89233218CNA000001); the European Unionâs Horizon 2020 research and innovation program under grant agreement No. 730562 RadioNet; ALMA North America Development Fund; the Academia Sinica; Chandra TM6- 17006X; Chandra award DD7-18089X.https://journals.aps.org/prd/am2023Physic
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