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Birrer S, Millon M, Sluse D, Shajib AJ, Courbin F, Erickson S, Koopmans LVE, Suyu SH, Treu T. Time-Delay Cosmography: Measuring the Hubble Constant and Other Cosmological Parameters with Strong Gravitational Lensing. SPACE SCIENCE REVIEWS 2024; 220:48. [PMID: 38899030 PMCID: PMC11182856 DOI: 10.1007/s11214-024-01079-w] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/03/2023] [Accepted: 05/08/2024] [Indexed: 06/21/2024]
Abstract
Multiply lensed images of a same source experience a relative time delay in the arrival of photons due to the path length difference and the different gravitational potentials the photons travel through. This effect can be used to measure absolute distances and the Hubble constant ( H 0 ) and is known as time-delay cosmography. The method is independent of the local distance ladder and early-universe physics and provides a precise and competitive measurement of H 0 . With upcoming observatories, time-delay cosmography can provide a 1% precision measurement of H 0 and can decisively shed light on the current reported 'Hubble tension'. This manuscript details the general methodology developed over the past decades in time-delay cosmography, discusses recent advances and results, and, foremost, provides a foundation and outlook for the next decade in providing accurate and ever more precise measurements with increased sample size and improved observational techniques.
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Affiliation(s)
- S. Birrer
- Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794 USA
- Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, Stanford, CA 94305 USA
| | - M. Millon
- Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, Stanford, CA 94305 USA
- Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland
| | - D. Sluse
- STAR Institute, Quartier Agora - Allée du six Août, 19c B-4000 Liège, Belgium
| | - A. J. Shajib
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 USA
- Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637 USA
| | - F. Courbin
- Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland
- ICC-UB Institut de Ciències del Cosmos, University of Barcelona, Martí Franquès, 1, E-08028 Barcelona, Spain
- ICREA, Pg. Lluís Companys 23, Barcelona, E-08010 Spain
| | - S. Erickson
- Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, Stanford, CA 94305 USA
| | - L. V. E. Koopmans
- Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700AV Groningen, The Netherlands
| | - S. H. Suyu
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
- TUM School of Natural Sciences, Physics Department, Technical University of Munich, James-Franck-Straße 1, 85748 Garching, Germany
- Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), 11F of ASMAB, No.1, Sect. 4, Roosevelt Road, Taipei, 10617 Taiwan
| | - T. Treu
- Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 USA
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2
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Chaudhary SS, Toivonen A, Waratkar G, Mo G, Chatterjee D, Antier S, Brockill P, Coughlin MW, Essick R, Ghosh S, Morisaki S, Baral P, Baylor A, Adhikari N, Brady P, Cabourn Davies G, Dal Canton T, Cavaglia M, Creighton J, Choudhary S, Chu YK, Clearwater P, Davis L, Dent T, Drago M, Ewing B, Godwin P, Guo W, Hanna C, Huxford R, Harry I, Katsavounidis E, Kovalam M, Li AK, Magee R, Marx E, Meacher D, Messick C, Morice-Atkinson X, Pace A, De Pietri R, Piotrzkowski B, Roy S, Sachdev S, Singer LP, Singh D, Szczepanczyk M, Tang D, Trevor M, Tsukada L, Villa-Ortega V, Wen L, Wysocki D. Low-latency gravitational wave alert products and their performance at the time of the fourth LIGO-Virgo-KAGRA observing run. Proc Natl Acad Sci U S A 2024; 121:e2316474121. [PMID: 38652749 PMCID: PMC11067028 DOI: 10.1073/pnas.2316474121] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/25/2023] [Accepted: 03/16/2024] [Indexed: 04/25/2024] Open
Abstract
Multimessenger 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 ALIGO's, AdVirgo's and KAGRA's fourth observing run (O4). To support this effort, public semiautomated 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-toend 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. 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 LIGO-Virgo-KAGRA (LVK) low-latency alert infrastructure and data products using theMDCand serves as a useful reference for the interpretation of O4 detections.
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Affiliation(s)
- Sushant Sharma Chaudhary
- Institute of Multi-messenger Astrophysics and Cosmology, Missouri University of Science and Technology, Rolla, MO65409
| | - Andrew Toivonen
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN55455
| | | | - Geoffrey Mo
- MIT Kavli Institute for Astrophysics, Massachusetts Institute of Technology, Cambridge, MA02139
- MIT Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA02139
| | - Deep Chatterjee
- MIT Kavli Institute for Astrophysics, Massachusetts Institute of Technology, Cambridge, MA02139
- MIT Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA02139
| | - Sarah Antier
- Artemis, Observatoire de la Côte d’Azur, Université Côte d’Azur, Nice06304, France
| | - Patrick Brockill
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Michael W. Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN55455
| | - Reed Essick
- Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ONM5S 3H8, Canada
- Department of Physics, University of Toronto, Toronto, ONM5S 1A7, Canada
- David A. Dunlap Department of Astronomy, University of Toronto, Toronto, ONM5S 3H4, Canada
| | - Shaon Ghosh
- Department of Physics and Astronomy, Montclair State University, NJ07043
| | - Soichiro Morisaki
- Institute for Cosmic Ray Research, The University of Tokyo, Chiba277-8582, Japan
| | - Pratyusava Baral
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Amanda Baylor
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Naresh Adhikari
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Patrick Brady
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | | | - Tito Dal Canton
- Université Paris-Saclay, CNRS/IN2P3, IJCLab, Orsay91405, France
| | - Marco Cavaglia
- Institute of Multi-messenger Astrophysics and Cosmology, Missouri University of Science and Technology, Rolla, MO65409
| | | | - Sunil Choudhary
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Yu-Kuang Chu
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Patrick Clearwater
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Luke Davis
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Thomas Dent
- Instituto Galego de Física de Altas Enerxías, Universidade de Santiago de Compostela, 15705Santiago de Compostela, Spain
| | - Marco Drago
- Universitá di Roma La Sapienza and INFN, Sezione di Roma, RomaI-00133, Italy
| | - Becca Ewing
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | - Patrick Godwin
- Laser Interferometer Gravitational-Wave Observatory (LIGO) Laboratory, California Institute of Technology, Pasadena, CA91125
| | - Weichangfeng Guo
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Chad Hanna
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA16802
- Institute for Computational and Data Sciences, The Pennsylvania State University, University Park, PA16802
| | - Rachael Huxford
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | - Ian Harry
- University of Portsmouth, PortsmouthPO1 3FX, United Kingdom
| | - Erik Katsavounidis
- MIT Kavli Institute for Astrophysics, Massachusetts Institute of Technology, Cambridge, MA02139
- MIT Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA02139
| | - Manoj Kovalam
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Alvin K.Y. Li
- Laser Interferometer Gravitational-Wave Observatory (LIGO) Laboratory, California Institute of Technology, Pasadena, CA91125
| | - Ryan Magee
- Laser Interferometer Gravitational-Wave Observatory (LIGO) Laboratory, California Institute of Technology, Pasadena, CA91125
| | - Ethan Marx
- MIT Kavli Institute for Astrophysics, Massachusetts Institute of Technology, Cambridge, MA02139
- MIT Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA02139
| | - Duncan Meacher
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Cody Messick
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | | | - Alexander Pace
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | - Roberto De Pietri
- Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Universitá di Parma, ParmaI-43124, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Milano Bicocca, Gruppo Collegato di Parma, ParmaI-43124, Italy
| | - Brandon Piotrzkowski
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Soumen Roy
- Nikhef, Amsterdam1098 XG, The Netherlands
- Institute for Gravitational and Subatomic Physics, Utrecht University, Utrecht3584 CC, The Netherlands
| | - Surabhi Sachdev
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
- School of Physics, Georgia Institute of Technology, Atlanta, GW30332
| | - Leo P. Singer
- Astrophysics Science Division, NASA Goddard Space Flight Center, Code 661, Greenbelt, MD20771
- Joint Space-Science Institute, University of Maryland, College Park, MD20742
| | - Divya Singh
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | | | - Daniel Tang
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Max Trevor
- Department of Physics, University of Maryland, College Park, MD20742
| | - Leo Tsukada
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | - Verónica Villa-Ortega
- Instituto Galego de Física de Altas Enerxías, Universidade de Santiago de Compostela, 15705Santiago de Compostela, Spain
| | - Linqing Wen
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Daniel Wysocki
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
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Pang PTH, Dietrich T, Coughlin MW, Bulla M, Tews I, Almualla M, Barna T, Kiendrebeogo RW, Kunert N, Mansingh G, Reed B, Sravan N, Toivonen A, Antier S, VandenBerg RO, Heinzel J, Nedora V, Salehi P, Sharma R, Somasundaram R, Van Den Broeck C. An updated nuclear-physics and multi-messenger astrophysics framework for binary neutron star mergers. Nat Commun 2023; 14:8352. [PMID: 38123551 PMCID: PMC10733434 DOI: 10.1038/s41467-023-43932-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/23/2023] [Accepted: 11/24/2023] [Indexed: 12/23/2023] Open
Abstract
The multi-messenger detection of the gravitational-wave signal GW170817, the corresponding kilonova AT2017gfo and the short gamma-ray burst GRB170817A, as well as the observed afterglow has delivered a scientific breakthrough. For an accurate interpretation of all these different messengers, one requires robust theoretical models that describe the emitted gravitational-wave, the electromagnetic emission, and dense matter reliably. In addition, one needs efficient and accurate computational tools to ensure a correct cross-correlation between the models and the observational data. For this purpose, we have developed the Nuclear-physics and Multi-Messenger Astrophysics framework NMMA. The code allows incorporation of nuclear-physics constraints at low densities as well as X-ray and radio observations of isolated neutron stars. In previous works, the NMMA code has allowed us to constrain the equation of state of supranuclear dense matter, to measure the Hubble constant, and to compare dense-matter physics probed in neutron-star mergers and in heavy-ion collisions, and to classify electromagnetic observations and perform model selection. Here, we show an extension of the NMMA code as a first attempt of analyzing the gravitational-wave signal, the kilonova, and the gamma-ray burst afterglow simultaneously. Incorporating all available information, we estimate the radius of a 1.4M⊙ neutron star to be [Formula: see text] km.
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Affiliation(s)
- Peter T H Pang
- Nikhef, Science Park 105, 1098 XG, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, 3584 CC, Utrecht, The Netherlands
| | - Tim Dietrich
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany.
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam, Germany.
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Mattia Bulla
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91, Stockholm, Sweden
- Department of Physics and Earth Science, University of Ferrara, Via Saragat 1, I-44122, Ferrara, Italy
- INFN, Sezione di Ferrara, Via Saragat 1, I-44122, Ferrara, Italy
- INAF, Osservatorio Astronomico d'Abruzzo, Via Mentore Maggini snc, 64100, Teramo, Italy
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
| | - Mouza Almualla
- Department of Physics, American University of Sharjah, PO Box 26666, Sharjah, UAE
| | - Tyler Barna
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Ramodgwendé Weizmann Kiendrebeogo
- Laboratoire de Physique et de Chimie de l'Environnement, Université Joseph KI-ZERBO, Ouagadougou, Burkina Faso
- Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS, 96 Boulevard de l'Observatoire, F06304, Nice Cedex 4, France
| | - Nina Kunert
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
| | - Gargi Mansingh
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
- Department of Physics, American University, Washington, DC, 20016, USA
| | - Brandon Reed
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
- Department of Physics and Astronomy, University of Minnesota-Duluth, Duluth, MN, 55812, USA
| | - Niharika Sravan
- Department of Physics, Drexel University, Philadelphia, PA, 19104, USA
| | - Andrew Toivonen
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Sarah Antier
- Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS, 96 Boulevard de l'Observatoire, F06304, Nice Cedex 4, France
| | - Robert O VandenBerg
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Jack Heinzel
- Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, MA, 02139, USA
| | - Vsevolod Nedora
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam, Germany
| | - Pouyan Salehi
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
| | - Ritwik Sharma
- Department of Physics, Deshbandhu College, University of Delhi, New Delhi, India
| | - Rahul Somasundaram
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
- Université Lyon, Université Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, F-69622, Villeurbanne, France
- Department of Physics, Syracuse University, Syracuse, NY, 13244, USA
| | - Chris Van Den Broeck
- Nikhef, Science Park 105, 1098 XG, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, 3584 CC, Utrecht, The Netherlands
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4
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Annala E, Gorda T, Hirvonen J, Komoltsev O, Kurkela A, Nättilä J, Vuorinen A. Strongly interacting matter exhibits deconfined behavior in massive neutron stars. Nat Commun 2023; 14:8451. [PMID: 38114461 PMCID: PMC10730725 DOI: 10.1038/s41467-023-44051-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/03/2023] [Accepted: 11/28/2023] [Indexed: 12/21/2023] Open
Abstract
Neutron-star cores contain matter at the highest densities in our Universe. This highly compressed matter may undergo a phase transition where nuclear matter melts into deconfined quark matter, liberating its constituent quarks and gluons. Quark matter exhibits an approximate conformal symmetry, predicting a specific form for its equation of state (EoS), but it is currently unknown whether the transition takes place inside at least some physical neutron stars. Here, we quantify this likelihood by combining information from astrophysical observations and theoretical calculations. Using Bayesian inference, we demonstrate that in the cores of maximally massive stars, the EoS is consistent with quark matter. We do this by establishing approximate conformal symmetry restoration with high credence at the highest densities probed and demonstrating that the number of active degrees of freedom is consistent with deconfined matter. The remaining likelihood is observed to correspond to EoSs exhibiting phase-transition-like behavior, treated as arbitrarily rapid crossovers in our framework.
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Affiliation(s)
- Eemeli Annala
- Department of Physics and Helsinki Institute of Physics, University of Helsinki, P.O. Box 64, FI-00014, University of Helsinki, Finland
| | - Tyler Gorda
- Technische Universität Darmstadt, Department of Physics, 64289, Darmstadt, Germany.
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291, Darmstadt, Germany.
| | - Joonas Hirvonen
- Department of Physics and Helsinki Institute of Physics, University of Helsinki, P.O. Box 64, FI-00014, University of Helsinki, Finland.
| | - Oleg Komoltsev
- Faculty of Science and Technology, University of Stavanger, 4036, Stavanger, Norway.
| | - Aleksi Kurkela
- Faculty of Science and Technology, University of Stavanger, 4036, Stavanger, Norway.
| | - Joonas Nättilä
- Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY, 10010, USA.
- Physics Department and Columbia Astrophysics Laboratory, Columbia University, 538 West 120th Street, New York, NY, 10027, USA.
| | - Aleksi Vuorinen
- Department of Physics and Helsinki Institute of Physics, University of Helsinki, P.O. Box 64, FI-00014, University of Helsinki, Finland.
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5
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Kelly PL, Rodney S, Treu T, Oguri M, Chen W, Zitrin A, Birrer S, Bonvin V, Dessart L, Diego JM, Filippenko AV, Foley RJ, Gilman D, Hjorth J, Jauzac M, Mandel K, Millon M, Pierel J, Sharon K, Thorp S, Williams L, Broadhurst T, Dressler A, Graur O, Jha S, McCully C, Postman M, Schmidt KB, Tucker BE, von der Linden A. Constraints on the Hubble constant from Supernova Refsdal's reappearance. Science 2023:eabh1322. [PMID: 37167351 DOI: 10.1126/science.abh1322] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 05/13/2023]
Abstract
The gravitationally lensed Supernova Refsdal appeared in multiple images, produced through gravitational lensing by a massive foreground galaxy cluster. After the supernova appeared in 2014, lens models of the galaxy cluster predicted an additional image of the supernova would appear in 2015, which was subsequently observed. We use the time delays between the images to perform a blinded measurement of the expansion rate of the Universe, quantified by the Hubble constant (H0). Using eight cluster lens models, we infer [Formula: see text], where Mpc is the megaparsec. Using the two models most consistent with the observations, we find [Formula: see text]. The observations are best reproduced by models that assign dark-matter halos to individual galaxies and the overall cluster.
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Affiliation(s)
- Patrick L Kelly
- Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, MN 55455, USA
| | - Steven Rodney
- Department of Physics and Astronomy, University of South Carolina, Columbia, SC 29208, USA
| | - Tommaso Treu
- Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA
| | - Masamune Oguri
- Center for Frontier Science, Chiba University, Chiba 263-8522, Japan
- Research Center for the Early Universe, University of Tokyo, Tokyo 113-0033, Japan
- Kavli Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Wenlei Chen
- Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, MN 55455, USA
| | - Adi Zitrin
- Physics Department, Ben-Gurion University of the Negev, Beer-Sheva 8410501, Israel
| | - Simon Birrer
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
- Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794, USA
| | - Vivien Bonvin
- Laboratoire d'Astrophysique, Ecole Polytechnique Federale de Lausanne, Observatoire de Sauverny, CH-1290 Versoix, Switzerland
| | - Luc Dessart
- Institut d'Astrophysique de Paris, Centre national de la recherche scientifique-Sorbonne Université, F-75014 Paris, France
| | - Jose M Diego
- Instituto de Física de Cantabria, Consejo Superior de Investigaciones Científicas y la Universidad de Cantabria, 39005 Santander, Spain
| | - Alexei V Filippenko
- Department of Astronomy, University of California, Berkeley, CA 94720, USA
- Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA
| | - Ryan J Foley
- Department of Astronomy and Astrophysics, University of California Observatories/Lick Observatory, University of California, Santa Cruz, CA 95064, USA
| | - Daniel Gilman
- Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA
- Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON, M5S 3H4, Canada
| | - Jens Hjorth
- Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark
| | - Mathilde Jauzac
- Centre for Extragalactic Astronomy, Department of Physics, Durham University, Durham DH1 3LE, UK
- Institute for Computational Cosmology, Durham University, Durham DH1 3LE, UK
- Astrophysics Research Center, University of KwaZulu-Natal, Durban 4041, South Africa
- School of Mathematics, Statistics, and Computer Science, University of KwaZulu-Natal, Durban 4041, South Africa
| | - Kaisey Mandel
- Institute of Astronomy and Kavli Institute for Cosmology, Cambridge CB3 0HA, UK
- Statistical Laboratory, Department of Pure Mathematics and Mathematical Statistics, University of Cambridge, Cambridge CB3 0WB, UK
| | - Martin Millon
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
- Laboratoire d'Astrophysique, Ecole Polytechnique Federale de Lausanne, Observatoire de Sauverny, CH-1290 Versoix, Switzerland
| | - Justin Pierel
- Department of Physics and Astronomy, University of South Carolina, Columbia, SC 29208, USA
- Space Telescope Science Institute, Baltimore, MD 21218, USA
| | - Keren Sharon
- Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA
| | - Stephen Thorp
- Institute of Astronomy and Kavli Institute for Cosmology, Cambridge CB3 0HA, UK
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691, Stockholm, Sweden
| | - Liliya Williams
- Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, MN 55455, USA
| | - Tom Broadhurst
- Ikerbasque Foundation, University of the Basque Country, Donosita International Physics Center, Donostia, Spain
| | - Alan Dressler
- The Observatories of the Carnegie Institution for Science, Pasadena, CA 91101, USA
| | - Or Graur
- Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK
- Department of Astrophysics, American Museum of Natural History, New York, NY 10024, USA
| | - Saurabh Jha
- Department of Physics and Astronomy, Rutgers, The State University of New Jersey, Piscataway, NJ 08854, USA
| | - Curtis McCully
- Las Cumbres Observatory, Goleta, CA 93117, USA
- Department of Physics, University of California, Santa Barbara, CA 93106, USA
| | - Marc Postman
- Space Telescope Science Institute, Baltimore, MD 21218, USA
| | | | - Brad E Tucker
- The Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Australian National University, Canberra, ACT 2611, Australia
- National Centre for the Public Awareness of Science, Australian National University, Canberra, ACT 2611, Australia
- The Australian Research Council Centre of Excellence for All-Sky Astrophysics in 3 Dimensions, ACT 2611, Australia
| | - Anja von der Linden
- Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794, USA
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6
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Han MZ, Huang YJ, Tang SP, Fan YZ. Plausible presence of new state in neutron stars with masses above 0.98M TOV. Sci Bull (Beijing) 2023; 68:913-919. [PMID: 37080849 DOI: 10.1016/j.scib.2023.04.007] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/30/2023] [Revised: 04/03/2023] [Accepted: 04/04/2023] [Indexed: 04/22/2023]
Abstract
We investigate the neutron star (NS) equation of state (EOS) by incorporating multi-messenger data of GW170817, PSR J0030 + 0451, PSR J0740 + 6620, and state-of-the-art theoretical progresses, including the information from chiral effective field theory (χEFT) and perturbative quantum chromodynamics (pQCD) calculation. Taking advantage of the various structures sampling by a single-layer feed-forward neural network model embedded in the Bayesian nonparametric inference, the structure of NS matter's sound speed cs is explored in a model-agnostic way. It is found that a peak structure is common in the cs2 posterior, locating at 2.4-4.8ρsat (nuclear saturation density) and cs2 exceeds c2/3 at 90% credibility. The non-monotonic behavior suggests evidence of the state deviating from the hadronic matter inside the very massive NSs. Assuming the new/exotic state is featured as it is softer than typical hadronic models or even with hyperons, we find that a sizable (⩾10-3M⊙) exotic core, likely made of quark matter, is plausible for the NS with a gravitational mass above about 0.98MTOV, where MTOV represents the maximum gravitational mass of a non-rotating cold NS. The inferred MTOV=2.18-0.13+0.27M⊙ (90% credibility) is well consistent with the value of 2.17-0.12+0.15M⊙ estimated independently with GW170817/GRB 170817A/AT2017gfo assuming a temporary supramassive NS remnant formed after the merger. PSR J0740 + 6620, the most massive NS detected so far, may host a sizable exotic core with a probability of ≈0.36.
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Affiliation(s)
- Ming-Zhe Han
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - Yong-Jia Huang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China; RIKEN Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, Wako 351-0198, Japan
| | - Shao-Peng Tang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Yi-Zhong Fan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China.
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7
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Zeng J, Li Y, Hou Y, Yuan J. Nonideal effect of free electrons on ionization equilibrium and radiative property in dense plasmas. Phys Rev E 2023; 107:L033201. [PMID: 37072979 DOI: 10.1103/physreve.107.l033201] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/28/2022] [Accepted: 02/26/2023] [Indexed: 04/20/2023]
Abstract
The thermodynamic as well as optical properties of strongly coupled plasmas depend crucially on the average degree of ionization and the ionic state composition, which, however, cannot be determined by using the normal Saha equation usually used for the ideal plasmas. Hence, an adequate treatment of the ionization balance and the charge state distribution of strongly coupled plasmas is still a challenge for theory due to the interactions between the electrons and ions and among the electrons themselves. Based on a local density temperature-dependent ion-sphere model, the Saha equation approach is extended to the regime of strongly coupled plasmas by taking into account the free-electron-ion interaction, the free-free-electron interaction, the nonuniform free-electron space distribution, and the free-electron quantum partial degeneracy. All the quantities, including the bound orbitals with ionization potential depression, free-electron distribution, and bound and free-electron partition function contributions, are calculated self-consistently in the theoretical formalism. This study shows that the ionization equilibrium is evidently modified by considering the above nonideal characteristics of the free electrons. Our theoretical formalism is validated by the explanation of a recent experimental measurement of the opacity of dense hydrocarbon.
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Affiliation(s)
- Jiaolong Zeng
- College of Science, Zhejiang University of Technology, Hangzhou Zhejiang 310023, People's Republic of China
- College of Science, National University of Defense Technology, Changsha Hunan 410073, People's Republic of China
| | - Yongjun Li
- College of Science, National University of Defense Technology, Changsha Hunan 410073, People's Republic of China
| | - Yong Hou
- College of Science, National University of Defense Technology, Changsha Hunan 410073, People's Republic of China
| | - Jianmin Yuan
- College of Science, National University of Defense Technology, Changsha Hunan 410073, People's Republic of China
- Graduate School of China Academy of Engineering Physics, Beijing 100193, People's Republic of China
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8
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Keller J, Hebeler K, Schwenk A. Nuclear Equation of State for Arbitrary Proton Fraction and Temperature Based on Chiral Effective Field Theory and a Gaussian Process Emulator. PHYSICAL REVIEW LETTERS 2023; 130:072701. [PMID: 36867798 DOI: 10.1103/physrevlett.130.072701] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/05/2022] [Revised: 12/09/2022] [Accepted: 01/12/2023] [Indexed: 06/18/2023]
Abstract
We calculate the equation of state of asymmetric nuclear matter at finite temperature based on chiral effective field theory interactions to next-to-next-to-next-to-leading order. Our results assess the theoretical uncertainties from the many-body calculation and the chiral expansion. Using a Gaussian process emulator for the free energy, we derive the thermodynamic properties of matter through consistent derivatives and use the Gaussian process to access arbitrary proton fraction and temperature. This enables a first nonparametric calculation of the equation of state in beta equilibrium, and of the speed of sound and the symmetry energy at finite temperature. Moreover, our results show that the thermal part of the pressure decreases with increasing densities.
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Affiliation(s)
- J Keller
- Technische Universität Darmstadt, Department of Physics, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
| | - K Hebeler
- Technische Universität Darmstadt, Department of Physics, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - A Schwenk
- Technische Universität Darmstadt, Department of Physics, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
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9
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Kölsch M, Dietrich T, Ujevic M, Brügmann B. Investigating the mass-ratio dependence of the prompt-collapse threshold with numerical-relativity simulations. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.044026] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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10
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Biswas B, Datta S. Constraining neutron star properties with a new equation of state insensitive approach. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043012] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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11
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Cuoco E, Patricelli B, Iess A, Morawski F. Computational challenges for multimodal astrophysics. NATURE COMPUTATIONAL SCIENCE 2022; 2:479-485. [PMID: 38177801 DOI: 10.1038/s43588-022-00288-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/04/2021] [Accepted: 06/30/2022] [Indexed: 01/06/2024]
Abstract
In the coming decades, we will face major computational challenges, when the improved sensitivity of third-generation gravitational wave detectors will be such that they will be able to detect a high number (of the order of 7 × 104 per year) of multi-messenger events from binary neutron star mergers, similar to GW 170817. In this Perspective, we discuss the application of multimodal artificial intelligence techniques for multi-messenger astrophysics, fusing the information from different signal emissions.
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Affiliation(s)
- Elena Cuoco
- European Gravitational Observatory (EGO), Pisa, Italy.
- Scuola Normale Superiore, Pisa, Italy.
- INFN, Sezione di Pisa, Pisa, Italy.
| | - Barbara Patricelli
- European Gravitational Observatory (EGO), Pisa, Italy
- INFN, Sezione di Pisa, Pisa, Italy
- University of Pisa, Pisa, Italy
| | - Alberto Iess
- Scuola Normale Superiore, Pisa, Italy
- INFN, Sezione di Pisa, Pisa, Italy
| | - Filip Morawski
- Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Warsaw, Poland
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12
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Ujevic M, Rashti A, Gieg H, Tichy W, Dietrich T. High-accuracy high-mass-ratio simulations for binary neutron stars and their comparison to existing waveform models. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.023029] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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13
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Incorporating a Radiative Hydrodynamics Scheme in the Numerical-Relativity Code BAM. UNIVERSE 2022. [DOI: 10.3390/universe8070370] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
To study binary neutron star systems and to interpret observational data such as gravitational-wave and kilonova signals, one needs an accurate description of the processes that take place during the final stages of the coalescence, for example, through numerical-relativity simulations. In this work, we present an updated version of the numerical-relativity code BAM in order to incorporate nuclear-theory-based equations of state and a simple description of neutrino interactions through a neutrino leakage scheme. Different test simulations, for stars undergoing a neutrino-induced gravitational collapse and for binary neutron stars systems, validate our new implementation. For the binary neutron stars systems, we show that we can evolve stably and accurately distinct microphysical models employing the different equations of state: SFHo, DD2, and the hyperonic BHBΛϕ. Overall, our test simulations have good agreement with those reported in the literature.
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14
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Huth S, Pang PTH, Tews I, Dietrich T, Le Fèvre A, Schwenk A, Trautmann W, Agarwal K, Bulla M, Coughlin MW, Van Den Broeck C. Constraining neutron-star matter with microscopic and macroscopic collisions. Nature 2022; 606:276-280. [PMID: 35676430 PMCID: PMC9177417 DOI: 10.1038/s41586-022-04750-w] [Citation(s) in RCA: 11] [Impact Index Per Article: 5.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/13/2021] [Accepted: 04/11/2022] [Indexed: 11/16/2022]
Abstract
Interpreting high-energy, astrophysical phenomena, such as supernova explosions or neutron-star collisions, requires a robust understanding of matter at supranuclear densities. However, our knowledge about dense matter explored in the cores of neutron stars remains limited. Fortunately, dense matter is not probed only in astrophysical observations, but also in terrestrial heavy-ion collision experiments. Here we use Bayesian inference to combine data from astrophysical multi-messenger observations of neutron stars1-9 and from heavy-ion collisions of gold nuclei at relativistic energies10,11 with microscopic nuclear theory calculations12-17 to improve our understanding of dense matter. We find that the inclusion of heavy-ion collision data indicates an increase in the pressure in dense matter relative to previous analyses, shifting neutron-star radii towards larger values, consistent with recent observations by the Neutron Star Interior Composition Explorer mission5-8,18. Our findings show that constraints from heavy-ion collision experiments show a remarkable consistency with multi-messenger observations and provide complementary information on nuclear matter at intermediate densities. This work combines nuclear theory, nuclear experiment and astrophysical observations, and shows how joint analyses can shed light on the properties of neutron-rich supranuclear matter over the density range probed in neutron stars.
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Affiliation(s)
- Sabrina Huth
- Department of Physics, Technische Universität Darmstadt, Darmstadt, Germany.
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany.
| | - Peter T H Pang
- Nikhef, Amsterdam, The Netherlands.
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Utrecht, The Netherlands.
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, USA
| | - Tim Dietrich
- Institut für Physik und Astronomie, Universität Potsdam, Potsdam, Germany
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Potsdam, Germany
| | - Arnaud Le Fèvre
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - Achim Schwenk
- Department of Physics, Technische Universität Darmstadt, Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Max-Planck-Institut für Kernphysik, Heidelberg, Germany
| | | | - Kshitij Agarwal
- Physikalisches Institut, Eberhard Karls Universität Tübingen, Tübingen, Germany
| | - Mattia Bulla
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - Chris Van Den Broeck
- Nikhef, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Utrecht, The Netherlands
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15
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Multi-Messenger Constraints on the Hubble Constant Through Combination of Gravitational Waves, Gamma-Ray Bursts and Kilonovae from Neutron Star Mergers. UNIVERSE 2022. [DOI: 10.3390/universe8050289] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/10/2022]
Abstract
The simultaneous detection of gravitational waves and light from the binary neutron star merger GW170817 led to independent measurements of distance and redshift, providing a direct estimate of the Hubble constant H0 that does not rely on a cosmic distance ladder, nor assumes a specific cosmological model. By using gravitational waves as “standard sirens”, this approach holds promise to arbitrate the existing tension between the H0 value inferred from the cosmic microwave background and those obtained from local measurements. However, the known degeneracy in the gravitational-wave analysis between distance and inclination of the source led to a H0 value from GW170817 that was not precise enough to resolve the existing tension. In this review, we summarize recent works exploiting the viewing-angle dependence of the electromagnetic signal, namely the associated short gamma-ray burst and kilonova, to constrain the system inclination and improve on H0. We outline the key ingredients of the different methods, summarize the results obtained in the aftermath of GW170817 and discuss the possible systematics introduced by each of these methods.
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16
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Komoltsev O, Kurkela A. How Perturbative QCD Constrains the Equation of State at Neutron-Star Densities. PHYSICAL REVIEW LETTERS 2022; 128:202701. [PMID: 35657894 DOI: 10.1103/physrevlett.128.202701] [Citation(s) in RCA: 8] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/22/2021] [Revised: 03/14/2022] [Accepted: 04/25/2022] [Indexed: 06/15/2023]
Abstract
We demonstrate in a general and analytic way how high-density information about the equation of state (EOS) of strongly interacting matter obtained using perturbative quantum chromodynamics constrains the same EOS at densities reachable in physical neutron stars. Our approach is based on utilizing the full information of the thermodynamic potentials at the high-density limit together with thermodynamic stability and causality. This requires considering the pressure as a function of chemical potential p(μ) instead of the commonly used pressure as a function of energy density p(ε). The results can be used to propagate the perturbative quantum chromodynamics calculations reliable around 40n_{s} to lower densities in the most conservative way possible. We constrain the EOS starting from only a few times the nuclear saturation density n≳2.2n_{s}, and at n=5n_{s} we exclude at least 65% of otherwise allowed area in the ε-p plane. This provides information complementary to astrophysical observations that should be taken into account in any complete statistical inference study of the EOS. These purely theoretical results are independent of astrophysical neutron-star input, and hence, they can also be used to test theories of modified gravity and beyond the standard model physics in neutron stars.
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Affiliation(s)
- Oleg Komoltsev
- Faculty of Science and Technology, University of Stavanger, 4036 Stavanger, Norway
| | - Aleksi Kurkela
- Faculty of Science and Technology, University of Stavanger, 4036 Stavanger, Norway
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17
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Shahrbaf M, Blaschke D, Typel S, Farrar G, Alvarez-Castillo D. Sexaquark dilemma in neutron stars and its solution by quark deconfinement. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.103005] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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18
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Breschi M, Bernuzzi S, Godzieba D, Perego A, Radice D. Constraints on the Maximum Densities of Neutron Stars from Postmerger Gravitational Waves with Third-Generation Observations. PHYSICAL REVIEW LETTERS 2022; 128:161102. [PMID: 35522493 DOI: 10.1103/physrevlett.128.161102] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/22/2021] [Revised: 01/31/2022] [Accepted: 03/18/2022] [Indexed: 06/14/2023]
Abstract
Using data from 289 numerical relativity simulations of binary neutron star mergers, we identify, for the first time, a robust quasiuniversal relation connecting the postmerger peak gravitational-wave frequency and the value of the density at the center of the maximum mass nonrotating neutron star. This relation offers a new possibility for precision equation-of-state constraints with next-generation ground-based gravitational-wave interferometers. Mock Einstein Telescope observations of fiducial events indicate that Bayesian inferences can constrain the maximum density to ∼15% (90% credibility level) for a single signal at the minimum sensitivity threshold for a detection. If the postmerger signal is included in a full-spectrum (inspiral-merger-postmerger) analysis of such a signal, the pressure-density function can be tightly constrained up to the maximum density, and the maximum neutron star mass can be measured with an accuracy better than 12% (90% credibility level).
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Affiliation(s)
- Matteo Breschi
- Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, 07743 Jena, Germany
| | - Sebastiano Bernuzzi
- Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, 07743 Jena, Germany
| | - Daniel Godzieba
- Department of Physics, Pennsylvania State University, University Park, Pennsylvania 16802, USA
| | - Albino Perego
- Dipartimento di Fisica, Università di Trento, Via Sommarive 14, 38123 Trento, Italy
- INFN-TIFPA, Trento Institute for Fundamental Physics and Applications, via Sommarive 14, I-38123 Trento, Italy
| | - David Radice
- Department of Physics, Pennsylvania State University, University Park, Pennsylvania 16802, USA
- Institute for Gravitation and the Cosmos, Pennsylvania State University, University Park, Pennsylvania 16802, USA
- Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, Pennsylvania 16802, USA
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19
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Chatziioannou K. Uncertainty limits on neutron star radius measurements with gravitational waves. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.084021] [Citation(s) in RCA: 7] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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20
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Pacilio C, Maselli A, Fasano M, Pani P. Ranking Love Numbers for the Neutron Star Equation of State: The Need for Third-Generation Detectors. PHYSICAL REVIEW LETTERS 2022; 128:101101. [PMID: 35333071 DOI: 10.1103/physrevlett.128.101101] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/26/2021] [Revised: 01/22/2022] [Accepted: 02/10/2022] [Indexed: 06/14/2023]
Abstract
Gravitational-wave measurements of the tidal deformability in neutron-star binary coalescences can be used to infer the still unknown equation of state (EOS) of dense matter above the nuclear saturation density. By employing a Bayesian-ranking test, we quantify the ability of current and future gravitational-wave observations to discriminate among families of nuclear-physics based EOS which differ in particle content and ab initio microscopic calculations. While the constraining power of GW170817 is limited, we show that even twenty coalescences detected by LIGO-Virgo at design sensitivity are not enough to discriminate between EOS with similar softness but distinct microphysics. However, just a single detection with a third-generation detector such as the Einstein Telescope or Cosmic Explorer will rule out several families of EOS with very strong statistical significance and can discriminate among models which feature similar softness, hence, constraining the properties of nuclear matter to unprecedented levels.
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Affiliation(s)
- Costantino Pacilio
- Dipartimento di Fisica, "Sapienza" Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
- INFN, Sezione di Roma, Piazzale Aldo Moro 2, 00185 Roma, Italy
| | - Andrea Maselli
- Gran Sasso Science Institute (GSSI), I-67100 L'Aquila, Italy
- INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy
| | - Margherita Fasano
- Dipartimento di Fisica, "Sapienza" Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
| | - Paolo Pani
- Dipartimento di Fisica, "Sapienza" Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
- INFN, Sezione di Roma, Piazzale Aldo Moro 2, 00185 Roma, Italy
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21
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Abstract
In the frame of Gauss–Bonnet gravity and in the limit of D→4, based on the fact that spherically symmetric solution derived using any of regularization schemes will be the same form as the original theory, we derive a new interior spherically symmetric solution assuming specific forms of the metric potentials that have two constants. Using the junction condition we determine these two constants. By using the data of the star EXO 1785-248, whose mass is M=1.3±0.2M⊙ and radius l=8.849±0.4 km, we calculate the numerical values of these constants, in terms of the dimensionful coupling parameter of the Gauss–Bonnet term, and eventually, we get real values for these constants. In this regard, we show that the components of the energy–momentum tensor have a finite value at the center of the star as well as a smaller value to the surface of the star. Moreover, we show that the equations of the state behave in a non-linear way due to the impact of the Gauss–Bonnet term. Using the Tolman–Oppenheimer–Volkoff equation, the adiabatic index, and stability in the static state we show that the model under consideration is always stable. Finally, the solution of this study is matched with observational data of other pulsars showing satisfactory results.
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22
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Abstract
The neutron lifetime anomaly has been used to motivate the introduction of new physics with hidden-sector particles coupled to baryon number, and on which neutron stars provide powerful constraints. Although the neutron lifetime anomaly may eventually prove to be of mundane origin, we use it as motivation for a broader review of the ways that baryon number violation, be it real or apparent, and dark sectors can intertwine and how neutron star observables, both present and future, can constrain them.
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23
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Boccioli L, Mathews G, O’Connor E. Effect of the Nuclear Equation of State and Relativistic Turbulence on Core-Collapse Supernovae. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202226011025] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The nuclear Equation of State (EoS) is an important component in the evolution and subsequent explosion of core collapse supernovae. We make a survey of various equations of state that can be found in the literature and analyze their effect on the explosion. To simulate the supernovae, we use the general relativistic spherically-symmetric code GR1D, modified to take into account the effects of three-dimensional turbulence through a new mixing length theory approach (STIR). We show that the viability of the explosion is quite EoS dependent and that the strength of explosions correlate best with the central entropy density right after bounce and the onset of turbulent mixing in the proto-neutron star.
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24
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Translating Neutron Star Observations to Nuclear Symmetry Energy via Deep Neural Networks. GALAXIES 2022. [DOI: 10.3390/galaxies10010016] [Citation(s) in RCA: 5] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/04/2023]
Abstract
One of the most significant challenges involved in efforts to understand the equation of state of dense neutron-rich matter is the uncertain density dependence of the nuclear symmetry energy. In particular, the nuclear symmetry energy is still rather poorly constrained, especially at high densities. On the other hand, detailed knowledge of the equation of state is critical for our understanding of many important phenomena in the nuclear terrestrial laboratories and the cosmos. Because of its broad impact, pinning down the density dependence of the nuclear symmetry energy has been a long-standing goal of both nuclear physics and astrophysics. Recent observations of neutron stars, in both electromagnetic and gravitational-wave spectra, have already constrained significantly the nuclear symmetry energy at high densities. The next generation of telescopes and gravitational-wave observatories will provide an unprecedented wealth of detailed observations of neutron stars, which will improve further our knowledge of the density dependence of nuclear symmetry energy, and the underlying equation of state of dense neutron-rich matter. Training deep neural networks to learn a computationally efficient representation of the mapping between astrophysical observables of neutron stars, such as masses, radii, and tidal deformabilities, and the nuclear symmetry energy allows its density dependence to be determined reliably and accurately. In this work, we use a deep learning approach to determine the nuclear symmetry energy as a function of density directly from observational neutron star data. We show, for the first time, that artificial neural networks can precisely reconstruct the nuclear symmetry energy from a set of available neutron star observables, such as masses and radii as measured by, e.g., the NICER mission, or masses and tidal deformabilities as measured by the LIGO/VIRGO/KAGRA gravitational-wave detectors. These results demonstrate the potential of artificial neural networks to reconstruct the symmetry energy and the equation of state directly from neutron star observational data, and emphasize the importance of the deep learning approach in the era of multi-messenger astrophysics.
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25
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Ivanytskyi O, Blaschke D, Fischer T, Bauswein A. Early deconfinement of asymptotically conformal color-superconducting quark matter in neutron stars. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202227407010] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/24/2022] Open
Abstract
We present a relativistic density functional approach to color superconducting quark matter that mimics quark confinement by a fast growth of the quasiparticle selfenergy in the confining region. The approach is shown to be equivalent to a chiral model of quark matter with medium dependent couplings. While the (pseudo)scalar sector of the model is fitted to the vacuum phenomenology of quantum chromodynamics, the strength of interaction in the vector and diquark channels is varied in order to provide the best agreement with the observational constraints on the mass-radius relation and tidal deformability of neutron stars modelled with our approach. In order to recover the conformal behavior of quark matter at asymptotically high densities we introduce a medium dependence of the vector and diquark couplings motivated by the non-perturbative gluon exchange. Our analysis signals that the onset of deconfinement to color superconducting quark matter is likely to occur in neutron stars with masses below 1.0 M⊙.
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Blaschke D, Ayriyan A, Cierniak M, Grunfeld AG, Ivanytskyi O, Shahrbaf M. Special point "trains" in the M-R diagram of hybrid stars. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202227407011] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/24/2022] Open
Abstract
We present a systematic investigation of the possible locations for the special point (SP), a unique feature of hybrid neutron stars in the massradius diagram. The study is performed within the two-phase approach where the high-density (quark matter) phase is described by the covariant nonlocal Nambu–Jona-Lasinio (nlNJL) model equation of state (EOS) which is shown to be equivalent to a constant-sound-speed (CSS) EOS. For the nuclear matter phase around saturation density different relativistic density functional EOSs are used: DD2p00, its excluded-volume modification DD2p40 and the hypernuclear EOS DD2Y-T. In the present contribution we apply the Maxwell construction scheme for the deconfinement transition and demonstrate that a simultaneous variation of the vector and diquark coupling constants results in the occurrence of SP "trains" which are invariant against changing the nuclear matter EOS. We propose that the SP train corresponding to a variation of the diquark coupling at constant vector coupling is special since it serves as a lower bound for the line of maximum masses and accessible radii of massive hybrid stars.
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Mendes RF, Ortiz N, Stergioulas N. Nonlinear dynamics of oscillating neutron stars in scalar-tensor gravity. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.104.104036] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Abstract
Magnetars have already been a potential candidate as gravitational wave sources that could be detected by current and future terrestrial as well as ground-based gravitational wave detectors. In this article, we focus on the gravitational wave emission from the distorted rotating neutron stars. The deformation is assumed to be symmetric around an axis that is perpendicular to the rotation axis. The form is applied in the context of a neutron star whose magnetic field has been deformed on its own. By introducing the effects from all magnetars in the Universe, based on various proposed magnetic field configurations, such as poloidal and toroidal, the stochastic gravitational wave background can be generated. We choose to figure out exactly how the observations of the stochastic gravitational wave background should be used to understand much more about physics correlated with the magnetar behavior, based on the restriction on the ellipticity of the magnetar.
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Yagi K, Stepniczka M. Neutron stars in scalar-tensor theories: Analytic scalar charges and universal relations. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.104.044017] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Abstract
A neutron star was first detected as a pulsar in 1967. It is one of the most mysterious compact objects in the universe, with a radius of the order of 10 km and masses that can reach two solar masses. In fact, neutron stars are star remnants, a kind of stellar zombie (they die, but do not disappear). In the last decades, astronomical observations yielded various contraints for neutron star masses, and finally, in 2017, a gravitational wave was detected (GW170817). Its source was identified as the merger of two neutron stars coming from NGC 4993, a galaxy 140 million light years away from us. The very same event was detected in γ-ray, X-ray, UV, IR, radio frequency and even in the optical region of the electromagnetic spectrum, starting the new era of multi-messenger astronomy. To understand and describe neutron stars, an appropriate equation of state that satisfies bulk nuclear matter properties is necessary. GW170817 detection contributed with extra constraints to determine it. On the other hand, magnetars are the same sort of compact object, but bearing much stronger magnetic fields that can reach up to 1015 G on the surface as compared with the usual 1012 G present in ordinary pulsars. While the description of ordinary pulsars is not completely established, describing magnetars poses extra challenges. In this paper, I give an overview on the history of neutron stars and on the development of nuclear models and show how the description of the tiny world of the nuclear physics can help the understanding of the cosmos, especially of the neutron stars.
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Nuclear Physics and Astrophysics Constraints on the High Density Matter Equation of State. UNIVERSE 2021. [DOI: 10.3390/universe7080257] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
(1) This review has been written in memory of Steven Moszkowski who unexpectedly passed away in December 2020. It has been inspired by our many years of discussions. Steven’s enthusiasm, drive and determination to understand atomic nuclei in simple terms of basic laws of physics was infectious. He sought the fundamental origin of nuclear forces in free space, and their saturation and modification in nuclear medium. His untimely departure left our job unfinished but his legacy lives on. (2) Focusing on the nuclear force acting in nuclear matter of astrophysical interest and its equation of state (EoS), we take several typical snapshots of evolution of the theory of nuclear forces. We start from original ideas in the 1930s moving through to its overwhelming diversity today. The development is supported by modern observational and terrestrial data and their inference in the multimessenger era, as well as by novel mathematical techniques and computer power. (3) We find that, despite the admirable effort both in theory and measurement, we are facing multiple models dependent on a large number of variable correlated parameters which cannot be constrained by data, which are not yet accurate, nor sensitive enough, to identify the theory closest to reality. The role of microphysics in the theories is severely limited or neglected, mostly deemed to be too difficult to tackle. (4) Taking the EoS of high-density matter as an example, we propose to develop models, based, as much as currently possible, on the microphysics of the nuclear force, with a minimal set of parameters, chosen under clear physical guidance. Still somewhat phenomenological, such models could pave the way to realistic predictions, not tracing the measurement, but leading it.
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Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817. UNIVERSE 2021. [DOI: 10.3390/universe7060182] [Citation(s) in RCA: 47] [Impact Index Per Article: 15.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
The density dependence of nuclear symmetry energy is among the most uncertain parts of the Equation of State (EOS) of dense neutron-rich nuclear matter. It is currently poorly known especially at suprasaturation densities partially because of our poor knowledge about isovector nuclear interactions at short distances. Because of its broad impacts on many interesting issues, pinning down the density dependence of nuclear symmetry energy has been a longstanding and shared goal of both astrophysics and nuclear physics. New observational data of neutron stars including their masses, radii, and tidal deformations since GW170817 have helped improve our knowledge about nuclear symmetry energy, especially at high densities. Based on various model analyses of these new data by many people in the nuclear astrophysics community, while our brief review might be incomplete and biased unintentionally, we learned in particular the following: (1) The slope parameter L of nuclear symmetry energy at saturation density ρ0 of nuclear matter from 24 new analyses of neutron star observables was about L≈57.7±19 MeV at a 68% confidence level, consistent with its fiducial value from surveys of over 50 earlier analyses of both terrestrial and astrophysical data within error bars. (2) The curvature Ksym of nuclear symmetry energy at ρ0 from 16 new analyses of neutron star observables was about Ksym≈−107±88 MeV at a 68% confidence level, in very good agreement with the systematics of earlier analyses. (3) The magnitude of nuclear symmetry energy at 2ρ0, i.e., Esym(2ρ0)≈51±13 MeV at a 68% confidence level, was extracted from nine new analyses of neutron star observables, consistent with the results from earlier analyses of heavy-ion reactions and the latest predictions of the state-of-the-art nuclear many-body theories. (4) While the available data from canonical neutron stars did not provide tight constraints on nuclear symmetry energy at densities above about 2ρ0, the lower radius boundary R2.01=12.2 km from NICER’s very recent observation of PSR J0740+6620 of mass 2.08±0.07M⊙ and radius R=12.2–16.3 km at a 68% confidence level set a tight lower limit for nuclear symmetry energy at densities above 2ρ0. (5) Bayesian inferences of nuclear symmetry energy using models encapsulating a first-order hadron–quark phase transition from observables of canonical neutron stars indicated that the phase transition shifted appreciably both L and Ksym to higher values, but with larger uncertainties compared to analyses assuming no such phase transition. (6) The high-density behavior of nuclear symmetry energy significantly affected the minimum frequency necessary to rotationally support GW190814’s secondary component of mass (2.50–2.67) M⊙ as the fastest and most massive pulsar discovered so far. Overall, thanks to the hard work of many people in the astrophysics and nuclear physics community, new data of neutron star observations since the discovery of GW170817 have significantly enriched our knowledge about the symmetry energy of dense neutron-rich nuclear matter.
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Al-Mamun M, Steiner AW, Nättilä J, Lange J, O'Shaughnessy R, Tews I, Gandolfi S, Heinke C, Han S. Combining Electromagnetic and Gravitational-Wave Constraints on Neutron-Star Masses and Radii. PHYSICAL REVIEW LETTERS 2021; 126:061101. [PMID: 33635682 DOI: 10.1103/physrevlett.126.061101] [Citation(s) in RCA: 8] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/04/2020] [Revised: 11/17/2020] [Accepted: 12/17/2020] [Indexed: 06/12/2023]
Abstract
We perform a joint Bayesian inference of neutron-star mass and radius constraints based on GW170817, observations of quiescent low-mass x-ray binaries (QLMXBs), photospheric radius expansion x-ray bursting sources, and x-ray timing observations of J0030+0451. With this dataset, the form of the prior distribution still has an impact on the posterior mass-radius curves and equation of state (EOS), but this impact is smaller than recently obtained when considering QLMXBs alone. We analyze the consistency of the electromagnetic data by including an "intrinsic scattering" contribution to the uncertainties, and find only a slight broadening of the posteriors. This suggests that the gravitational-wave and electromagnetic observations of neutron-star structure are providing a consistent picture of the neutron-star mass-radius curve and the EOS.
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Affiliation(s)
- Mohammad Al-Mamun
- Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
| | - Andrew W Steiner
- Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
- Physics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
| | - Joonas Nättilä
- Physics Department and Columbia Astrophysics Laboratory, Columbia University, 538 West 120th Street, New York, New York 10027, USA
- Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, New York 10010, USA
| | - Jacob Lange
- Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, New York 14623, USA
| | - Richard O'Shaughnessy
- Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, New York 14623, USA
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - Stefano Gandolfi
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - Craig Heinke
- Department of Physics, CCIS 4-183, University of Alberta, Edmonton, Alberta T6G 2E1, Canada
| | - Sophia Han
- Department of Physics, University of California, Berkeley, California 94720, USA
- Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA
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Dietrich T, Coughlin MW, Pang PTH, Bulla M, Heinzel J, Issa L, Tews I, Antier S. Multimessenger constraints on the neutron-star equation of state and the Hubble constant. Science 2020; 370:1450-1453. [PMID: 33335061 DOI: 10.1126/science.abb4317] [Citation(s) in RCA: 32] [Impact Index Per Article: 8.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/24/2020] [Accepted: 10/27/2020] [Indexed: 11/02/2022]
Abstract
Observations of neutron-star mergers with distinct messengers, including gravitational waves and electromagnetic signals, can be used to study the behavior of matter denser than an atomic nucleus and to measure the expansion rate of the Universe as quantified by the Hubble constant. We performed a joint analysis of the gravitational-wave event GW170817 with its electromagnetic counterparts AT2017gfo and GRB170817A, and the gravitational-wave event GW190425, both originating from neutron-star mergers. We combined these with previous measurements of pulsars using x-ray and radio observations, and nuclear-theory computations using chiral effective field theory, to constrain the neutron-star equation of state. We found that the radius of a 1.4-solar mass neutron star is [Formula: see text] km at 90% confidence and the Hubble constant is [Formula: see text] at 1σ uncertainty.
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Affiliation(s)
- Tim Dietrich
- Institut für Physik und Astronomie, Universität Potsdam, 14476 Potsdam, Germany. .,Nikhef, 1098 XG Amsterdam, Netherlands
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA
| | - Peter T H Pang
- Nikhef, 1098 XG Amsterdam, Netherlands.,Department of Physics, Utrecht University, 3584 CC Utrecht, Netherlands
| | - Mattia Bulla
- Nordic Institute for Theoretical Physics (Nordita), 106 91 Stockholm, Sweden
| | - Jack Heinzel
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA.,Department of Physics and Astronomy, Carleton College, Northfield, MN 55057, USA.,Artemis, Université Côte d'Azur, Centre National de la Recherche Scientifique, F-06304 Nice, France
| | - Lina Issa
- Nordic Institute for Theoretical Physics (Nordita), 106 91 Stockholm, Sweden.,École normale supérieure, Université Paris-Saclay, 91190 Gif-sur-Yvette, France
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
| | - Sarah Antier
- Astroparticule et Cosmologie, Université de Paris, Centre National de la Recherche Scientifique, F-75013 Paris, France
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