cometadata/test-preprints-extracted-funding huggingface dataset:
This material is based upon work supported by the Air Force Office of Scientific Research under award number FA9550-21-1-0287. Y.X. acknowledges support from the Dow Discovery Fellowship at UC Santa Barbara. S.C.T. is supported by the Packard Fellowship in Science and Engineering. Acknowledgment is made to the Donors of the American Chemical Society Petroleum Research Fund for partial support of this research. Use was made of computational facilities purchased with funds from the National Science Foundation (OAC-1925717) and administered by the Center for Scientific Computing (MRSEC; NSF DMR 1720256) at UC Santa Barbara.
This work was funded by UKRI under grants MR/T021519/1, EP/V036343/1 and EP/W002302/1, by the Deutsche Forschungsgemeinschaft within the frame of the collaborative research center CRC 1375 (project C5), by the Australian Research Council, the Australian National Fabrication Facility ACT node, as well as China special Grant (134000-E62201ZJ); Zhejiang Provincial Natural Science Foundation of China (Z24F040009), Zhejiang University Education Foundation Qizhen Scholar Foundation (K20240015), and CMOS Special Program of Zhejiang University (04010000-K2A033208).
This work is supported by the Department of Energy through the Fermilab QuantiSED program in the area of 'Intersections of QIS and Theoretical Particle Physics'. Fermilab is operated by Fermi Research Alliance, LLC under contract number DE-AC02-07CH11359 with the United States Department of Energy. Y.-Y. L is supported by the NSF of China through Grant No. 12305107, 12247103. J.S. is supported by Peking University under startup Grant No. 7101302974 and the National Natural Science Foundation of China under Grants No. 12025507, No.12150015; and is supported by the Key Research Program of Frontier Science of the Chinese Academy of Sciences (CAS) under Grants No. ZDBS-LY7003. This work was supported by the Munich Institute for Astro-, Particle and BioPhysics (MIAPbP), which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy-EXC-2094-390783311.
The first author is supported by Grant PAPIIT UNAM IN100723 'Curvas, sistemas lineales en superficies proyectivas y fibrados vectoriales' and CONACyT, Mexico A1-S-9029 'Moduli de curvas y curvatura en A g '. The second author would like to thank Centro de Ciencias Matematicas (CCM), UNAM Campus Morelia, for the wonderful hospitality and financial support through the Programa de Estancias de Investigacion (PREI) de la Direccion General Asuntos del Personal Academico, DGAPA-UNAM. He also likes to thank N. Nitsure (TIFR Mumbai) for his interest and support and U. Stuhler (G¨ ottingen) for introducing him to this exciting circle of ideas.
The authors would like to thank Drs. Gen Chiaki, Sunmyon Chon, Takashi Hosokawa, Ralf Klessen, Masahiro Machida, Hajime Susa and Benoit Commer¸ con for fruitful discussions and useful comments. The numerical simulations were carried out on XC50 Aterui II in Oshu City at the Center for Computational Astrophysics (CfCA) of the National Astronomical Observatory of Japan, the Cray XC40 at Yukawa Institute for Theoretical Physics in Kyoto University, and the computer cluster Draco at Frontier Research Institute for Interdiskiplinary Sciences of Tohoku University. This research is supported by Grants-in-Aid for Scientific Research (KO: 22H00149; KS: 21K20373; TM: 18H05437, 23K03464; KT: 21H04487, 22K0043) from the Japan Society for the Promotion of Science. KES acknowledges financial support from the Graduate Program on Physics for Universe of Tohoku University.
K.W. and T.T. acknowledge support from the JSPS KAKENHI (Grant Numbers 21H05233 and 23H02052) and World Premier International Research Center Initiative (WPI), MEXT, Japan.
This work was supported by the National Science Foundation under Grant No. 2004968. Part of this research was conducted at the Northwest Nanotechnology Infrastructure, a National Nanotechnology Coordinated Infrastructure site at Oregon State University which is supported in part by the National Science Foundation (grant NNCI-2025489) and Oregon State University.
Calculations were performed using the Sulis Tier 2 HPC platform hosted by the Scientific Computing Research Technology Platform at the University of Warwick. Sulis is funded by EPSRC Grant EP/T022108/1 and the HPC Midlands+ consortium. The authors would like to acknowledge the open source projects FlurryPP 2 , HiFiLES 3 , COOLFLUID 4 and PyFR 5 for inspiring the current implementation of the high order flux reconstruction solver. The authors also would like to thank the reviewers for their helpful comments and suggestions in the revision of this manuscript.
This research was supported in part by NSFC under Grant No. 62341201, 62122095, 62072472, 62172445, 62302260, and 62202256, by the National Key R&amp;D Program of China under Grant No. 2022YFF0604502, by CPSF Grant 2023M731956, and by a grant from the Guoqiang Institute, Tsinghua University.
This research is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the Universe from Maunakea, which has the cultural, historical, and natural significance in Hawaii. This work is partly supported by JST SPRING, Japan Grant Number JPMJSP2114, and Graduate Program on Physics for the Universe (GP-PU), Tohoku University. TK acknowledges JSPS KAKENHI Grant Number 18H03717 for financial support. This work is also supported by JSPS KAKENHI Grant Number 22K21349 (International Leading Research). JMPM acknowledges that this project has received funding from the European Union's Horizon research and innovation programme under the Marie Skłodowska-Curie grant agreement No 101106626. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large
The work of Y.-P. Choi is supported by NRF grant no. 2022R1A2C1002820, and the work of C. Pignotti is partially supported by PRIN 2022 (2022238YY5) Optimal control problems: analysis, approximation and applications , by PRIN-PNRR 2022 (P20225SP98) Some mathematical approaches to climate change and its impacts , and by INdAM GNAMPA Project 'Modelli alle derivate parziali per interazioni multiagente non simmetriche' (CUP E53C23001670001).
(ERDF) through project PID2022-136563NB-I00. DNA acknowledges funding support from Fundación Ramón Areces through their international post-doc grant program. AF and PRM thank Spanish MICIN for funding through project PID2019-106235GBI00 and grant PID2022-137980NB-I00 by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/ 10.13039/501100011033 and by 'ERDF A way of making Europe'. AF thanks the European Research Council (ERC) for funding under the Advanced Grant project SUL4LIFE, grant agreement No101096293. This research made use of the IAC HTCondor facility (http://research.cs.wisc.edu/htcondor/), partly financed by the Ministry of Economy and Competitiveness with FEDER funds, code IACA13-3E-2493. This research has made use of NASA's Astrophysics Data System Bibliographic Services. We acknowledge the community effort devoted to the development of the following open-source packages that were used in this work: numpy ( numpy.org , Harris et al. 2020), matplotlib ( matplotlib.org , Hunter 2007), PyTorch ( pytorch.org , Paszke et al. 2019), zarr ( github.com/zarr-developers/zarr-python ) and SHAP (Lundberg &amp; Lee 2017, github.com/shap/shap ).
AAR thanks Carlos Díaz Baso for helpful discussions on the training of NFs. AAR acknowledges support from the Agencia Estatal de Investigación del Ministerio de Ciencia, Innovación y Universidades (MCIU/AEI) and the European Regional Development Fund
This research was supported by the Swiss National Science Foundation (SNSF) under Projects No. PP00P2_170564 and No. 206021_150784. J.S. and M.G. thank the Stiftung für wissenschaftliche Forschung an der UZH for their financial support under grant STWF-21-023. XASand XMCD measurements were performed at SLS X07MA XTreme under proposal 20211683. J.S. and M.G. thank Thomas Greber for granting SQUID access and Michael Stöger-Pollach for performing electron magnetic circular dichroism measurements. Work at LIST was supported by the Luxembourg National Research Fund (FNR) through grants C20/MS/14718071/THERMODIMAT and C21/MS/15799044/FERRODYNAMICS.
This work was supported in part by the National Natural Science Foundation of China under Grant No. 61701197, in part by the National Key Research and Development Program of China under Grant No.2021YFA1000500(4), in part by the National key project 2020YFB1807700, NSFC 62071296, Shanghai Kewei 22JC1404000, in part by the Research Grants Council under the Areas of Excellence scheme grant AoE/E-601/22-R, in part by the 111 Project under Grant No. B12018. (Corresponding authors: Qiong Wu.)
CTD acknowledges support from the Ludwig MaximiliansUniversität in Munich. JHD acknowledges support from an STFC Ernest Rutherford Fellowship (project reference ST/S004858/1). BL acknowledges support from STFC Consolidated Grants ST/I00162X/1, ST/P000541/1 and ST/X001075/1. BG acknowledges support from the UKRI Stephen Hawking Fellowship (grant reference EP/Y017137/1) and a UK STFC Consolidated Grant. CHA acknowledges support from the Excellence Cluster ORIGINS which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy - EXC-2094 - 390783311.
The simulations of this project made use of the DiRAC@Durham facility managed by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). The equipment was funded by BEIS capital funding via STFC capital grants ST/K00042X/1, ST/P002293/1, ST/R002371/1 and ST/S002502/1, Durham University and STFC operations grant ST/R000832/1. DiRAC is part of the National eInfrastructure.
We acknowledge support from (i) JSPS KAKENHI (Grant no. JP 23H03499) to C. S., (ii) China Scholarship Council (Grant no. 202308530309) and Yunnan Provincial Department of Education Science Research Fund Project (Grant no. 2024Y503) to Z.H., and (iii) the grant-in-Aid for Scientific Research from JSPS, Japan, KAKENHI (Grant No. JP 20H02314 and JP 23H03499) awarded to J. T.
Acknoweldgements. We are grateful to M.C. L¨ obl, T. Bell, B. Brown, and S. Chen for fruitful discussions. We are grateful for financial support from Danmarks Grundforskningsfond (DNRF 139, Hy-Q Center for Hybrid Quantum Networks). L.A.P. acknowledges support from Novo Nordisk Foundation (Challenge project 'Solid-Q'). S.P. acknowledges funding from the Marie Skglyph[suppress] lodowskaCurie Fellowship project QSun (nr. 101063763), from the Villum Fonden research grants No.VIL50326 and No.VIL60743, and support from the NNF Quantum Computing Programme.
The work has been supported by Natural Science Foundation of Guangxi Autonomous Region with Grant No. 2022GXNSFDA035068, the National Natural Science Foundation of China (NNSFC) with Grants No. 12075074, No. 12235008, No. 11535002, No. 11705045, Hebei Natural Science Foundation for Distinguished Young Scholars with Grant No. A2022201017, and the youth top-notch talent support program of the Hebei Province.
The Center for High-Performance Buildings (CHPB) at Purdue University supported this work (project CHPB-26-2023). E. Pergantis was also supported by the Onassis Foundation as one of its scholars, as well as the American Society of Heating and Refrigeration Engineers (ASHRAE) through a Grant-in-Aid award. The authors would like to thank the occupants of the DC Nanogrid House for their patience during testing.
This work is supported by: Sweden's Innovation Agency (VINNOVA), grants 2017-02447, 2020-03611, and 202101420, the Swedish Research Council, grants 2017-04385 and 2022-03580, and Cancerfonden projects 22 2353 Pj and 22 2357 Pj. A part of the computations was enabled by resources provided by the National Academic Infrastructure for Supercomputing in Sweden (NAISS) and the Swedish National Infrastructure for Computing (SNIC) at Chalmers Centre for Computational Science and Engineering (C3SE), partially funded by the Swedish Research Council through grants 2022-06725 and 2018-05973. We are grateful to M. Matić for accurate cell location annotations.
R.J.G.E., J.C.R. and S.O. acknowledge support from the Netherlands Organisation for Scientific Research (NWO) and from the European Research Council (ERC Starting Grant 676895 'SPINCAD'). D.B., J.O., T.A., J.H., A.J.H., and Y.B. acknowledge support from the Institute for Basic Science (IBS-R027-D1). Y.B. acknowledges support from Asian Office of Aerospace Research and Development (FA2386-20-1-4052). D.B. acknowledges support from the Alexander von Humboldt Foundation for financial support through a Feodor-Lynen Research Fellowship. F.D. acknowledges support from MCIN/AEI/10.13039/501100011033, and 'FEDER, a way to make Europe', by the European Union (PID2022138269NB-I00).
Acknowledgements. We thank to the anonymous referee for their e ff ort reviewing this work. We also thank to all the authors who have helped us to access their data or who have provided relevant information on the targets: J.M. Almenara, C. Cadieux, D. Dragomir, X. Dumusque, E. González-Álvarez, R. Luque, and M. Mallorquín. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This Project has been funded by grant No.PID2019-107061GB-C61 by the Spanish Ministry of Science and Innovation / State Agency of Research MCIN / AEI / 10.13039 / 501100011033. O. B. R. is supported by INTA grant PRE-MDM-07. J.L.-B. was partly funded by grants LCF / BQ / PI20 / 11760023 (La Caixa), Ramón y Cajal fellowship with code RYC2021-031640-I, and CNS2023-144309. P. F. acknowledges the financial support of the SNSF, the work has been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grant 51NF40_205606. AL acknowledges support from the Swiss NCCR PlanetS and the Swiss National Science Foundation. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40182901 and 51NF40205606. AL acknowledges support of the Swiss National Science Foundation under grant number TMSGI2_211697. Co-funded by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work was supported by FCT - Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalização by these grants: UIDB / 04434 / 2020; UIDP / 04434 / 2020. E.H.C. aknowledges support from grant PRE2020-094770 under project PID2019109522GB-C51 funded by the Spanish Ministry of Science and Innovation / State Agency of Research, MCIN / AEI / 10.13039 / 501100011033, and by 'ERDF, A way of making Europe'.
ACKNOWLEDGMENTS. We are grateful to Moein Darman for providing the one-dimensional code for the FNO. This work is supported by grants from the NSF OAC CSSI program (2005123 and 2004512), Schmidt Sciences, LLC (to P.H. and J.A.), NSF award 2046309 (to P.H.), and the Office of Naval Research (ONR) Young Investigator Award N00014-20-1-2722 (to P.H.). Computational resources are provided by NCAR's CISL (allocation URIC0009) and NSF XSEDE (allocation ATM170020).
The authors would like to thank the referee, Georges Meynet, for his expertise and detailed guidance which was significant in enhancing the content of the manuscript. We acknowledge MESA authors and developers for their continued revisions and public accessibility of the code. JSV and ERH are supported by STFC funding under grant number ST/V000233/1 in the context of the BRIDGCE UK Network. RH acknowledges support from STFC, the World Premier International Research Centre Initiative (WPI Initiative), MEXT, Japan and the IReNA AccelNet Network of Networks (National Science Foundation, Grant No. OISE-1927130). AML acknowledges support from STFC funding under grant number ST/V000233 in the context of the BRIDGCE UK Network. This article is based upon work from the ChETEC COST Action (CA16117) and the European Union's Horizon 2020 research and innovation programme (ChETEC-INFRA,GrantNo.101008324).AACSissupportedbythe Deutsche Forschungsgemeinschaft (DFG - German Research Foundation) in the form of an Emmy Noether Research Group - ProjectID 445674056 (SA4064/1-1, PI Sander) and acknowledges funding from the Federal Ministry of Education and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the Excellence Strategy of the German Federal and State Governments.
Acknowledgements. The author thanks the referee for useful comments and helpful suggestions that improved this manuscript. NC acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG) - CA 2551 / 1-1,2 Our research used Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and APLpy, an open-source plotting
package for Python (Robitaille &amp; Bressert 2012). The Early Release Observations and associated materials were developed, executed, and compiled by the ERO production team. The EROs were also made possible by the foundational e ff orts and support from the JWST instruments, STScI planning and scheduling, Data Management teams, and O ffi ce of Public Outreach. Credits: NASA, ESA, CSA, STScI, Webb ERO Production Team.
Acknowledgements. I thank Natalia Masalaeva for sharing her code and for many helpful discussions, and Thorsten Ackemann for comments on the early version of the manuscript. This work was funded by the Austrian Science Fund (FWF Meitner-Programm, Project No. M3011) and the Austrian Academy of Sciences (ESQ Discovery Programm, Project: 'Using self-organization of ultracold atoms in emerging quantum technologies'). I acknowledge the support of the project KODYN financed by the European Union through the National Recovery and Resilience Plan 2021-2026 (NRPP). In addition, this work was supported by the project Centre for Advanced
Laser Techniques (CALT), co-funded by the European Union through the European Regional Development Fund under the Competitiveness and Cohesion Operational Programme (Grant No. KK.01.1.1.05.0001). The computational results presented here have been achieved using the Vienna Scientific Cluster (VSC). The dynamical evolution equations were solved numerically by using the open-source framework QuantumOptics.jl [69].
The authors are grateful to David Trestini for insightful discussions and cross-checking of some computations. T. J. also thanks Ulrich Sperhake for useful discussions. T. J. and P. R. thank the hospitality and the stimulating environment of the Institut des Hautes Etudes Scientifiques. T. J. is jointly funded by Cambridge Trust, the Department of Applied Mathematics and Theoretical Physics (DAMTP), and the Centre for Doctoral Training, University of Cambridge. P. R. is supported by the Italian Minister of University and Research (MUR) via the PRIN 2020KB33TP, Multimessenger astronomy in the Einstein Telescope Era (METE) . The present research was also partly supported by the ' 2021 Balzan Prize for Gravitation: Physical and Astrophysical Aspects ', awarded to Thibault Damour.
We are thankful to Adam Foster for valuable suggestions related to usage of the AtomDB data in numerical calculations as well as to Riccardo Ferrazzoli who provided us with the synchrotron fraction map for Tycho SNR. This paper employs a list of Chandra datasets, obtained by the Chandra X-ray Observatory, contained in DOI: 10.25574/cdc.259. O.P. acknowledges the OAPa grant number D.D.75/2022 funded by Direzione Scientifica of Istituto Nazionale di Astrofisica, Italy. L.C. is grateful for support from National Science Foundation grants AST-2107070 and AST-2205628. This project has received funding through the MSCA4Ukraine project, which is funded by the European Union. Views and opinions expressed are however those of the authors only and do not necessarily reflect those of the European Union. Neither the European Union nor the MSCA4Ukraine Consortium as a whole nor any individual member institutions of the MSCA4Ukraine Consortium can be held responsible for them. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work made use of the HPC system MEUSA, part of the Sistema Computazionale per l'Astrofisica Numerica (SCAN) of INAF-Osservatorio Astronomico di Palermo, Italy.
Acknowledgements. MBP, AACS, and VR are supported by the German Deutsche Forschungsgemeinschaft, DFG in the form of an Emmy Noether Research Group - Project-ID 445674056 (SA4064 / 1-1, PI Sander). MBP, AACS, and VR are further supported by funding from the Federal Ministry of Education and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the Excellence Strategy of the German Federal and State Governments. JJ acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) Project-ID 496854903 (SA4064 / 2-1, PI Sander) and is a member of the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg (IMPRS-HD). DP acknowledges financial support by the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50 OR 2005. JSV gratefully acknowledges support from STFC via grant ST / V000233 / 1. RK acknowledges financial support via the Heisenberg Research Grant funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under grant no. KU 2849 / 9, project no. 445783058. We thank Danny Lennon and Philip Dufton for providing additional spectra.
DE-SC0020081. The work of Z.T is supported by the U.S. Department of Energy under Award DE-SC0012704 and the Laboratory Directed Research and Development LDRD-23-050 project.
R.V's research is supported by the U.S. Department of Energy, Office of Science, under contract DE-SC0012704 and within the framework of the SURGE Topical Theory Collaboration. He acknowledges partial support from an LDRD at BNL. R.V's work on quantum information science is supported by the U.S. Department of Energy, Office of Science, National Quantum Information Science Research Centers, Co-design Center for Quantum Advantage (C2QA) under contract number DE-SC0012704. He was also supported at Stony Brook by the Simons Foundation as a coPI under Award number 994318 (Simons Collaboration on Confinement and QCD Strings). The work of XZB is supported in part by the U.S. DOE Office of Science under contract Nos. DE-FG02-89ER40531, DE-SC0012704, DE-FG02-10ER41666, and DE-AC02-98CH108. The work of JDB is supported in part by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics, under contract number DE-SC0024189 as part of the Early Career Research Program. H.D is supported by NSF Nuclear Theory grant 2208387, and partially by US-Israel Binational Science Foundation grant 2022132 and the U.S. Department of Energy, Office of Nuclear Physics through contract