Characterizing gravitational wave detector networks: from A<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math>to cosmic explorer

Abstract Gravitational-wave observations by the laser interferometer gravitational-wave observatory (LIGO) and Virgo have provided us a new tool to explore the Universe on all scales from nuclear physics to the cosmos and have the massive potential to further impact fundamental physics, astrophysics, and cosmology for decades to come. In this paper we have studied the science capabilities of a network of LIGO detectors when they reach their best possible sensitivity, called A <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math> , given the infrastructure in which they exist and a new generation of observatories that are factor of 10 to 100 times more sensitive (depending on the frequency), in particular a pair of L-shaped cosmic explorer (CE) observatories (one 40 km and one 20 km arm length) in the US and the triangular Einstein telescope with 10 km arms in Europe. We use a set of science metrics derived from the top priorities of several funding agencies to characterize the science capabilities of different networks. The presence of one or two A <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math> observatories in a network containing two or one next generation observatories, respectively, will provide good localization capabilities for facilitating multimessenger astronomy (MMA) and precision measurement of the Hubble parameter. Two CE observatories are indispensable for achieving precise localization of binary neutron star events, facilitating detection of electromagnetic counterparts and transforming MMA. Their combined operation is even more important in the detection and localization of high-redshift sources, such as binary neutron stars, beyond the star-formation peak, and primordial black hole mergers, which may occur roughly 100 million years after the Big Bang. The addition of the Einstein Telescope to a network of two CE observatories is critical for accomplishing all the identified science metrics including the nuclear equation of state, cosmological parameters, the growth of black holes through cosmic history, but also make new discoveries such as the presence of dark matter within or around neutron stars and black holes, continuous gravitational waves from rotating neutron stars, transient signals from supernovae, and the production of stellar-mass black holes in the early Universe. For most metrics the triple network of next generation terrestrial observatories are a factor 100 better than what can be accomplished by a network of three A <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math> observatories.

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Publication Details

Journal
Classical and Quantum Gravity
Published
2024-09-19
DOI
https://doi.org/10.1088/1361-6382/ad7b99
Citations
51
Primary Topic
Pulsars and Gravitational Waves Research
Type
article
Field-Weighted Citation Impact
16.91

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Characterizing gravitational wave detector networks: from A<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math>to cosmic explorer

D. B. Tanner, J. Read, K. G. Arun, Hsin-Yu Chen et al.
51 citations
Classical and Quantum Gravity
Pulsars and Gravitational Waves Research
16.91
article

Characterizing gravitational wave detector networks: from A<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math>to cosmic explorer

D. B. Tanner, J. Read, K. G. Arun, Hsin-Yu Chen, A. L. Miller, Ish Gupta, Anthony Pearce, E. D. Hall, Floor S. Broekgaarden, D. E. McClelland, K. Kuns, Ananya Bandopadhyay, CRISTIANO PALOMBA, Masha Baryakhtar, B. J. Owen, Philippe Landry, Tjonnie G. F. Li, D. H. Shoemaker, A. Nitz, L. Sun, Ssohrab Borhanian, M. Soares-Santos, Geoffrey Lovelace, C. Cahillane, M. E. Zucker, J. R. Smith, Chaitanya Afle, M. Evans, S. Biscoveanu, O. A. Hannuksela, L. Barsotti, S. Vitale, B. S. Sathyaprakash, D. Singh, Sanika Khadkikar, Emanuele Berti, B. J. J. Slagmolen, Keisi Kacanja, P. Fritschel, Rahul Kashyap, C.‐J. Haster, Hiroaki Yamamoto, Arnab Dhani, Joseph D. Romano, Hemantakumar Phurailatpam, Alessandra Corsi
article en
51 citations

Abstract

Abstract Gravitational-wave observations by the laser interferometer gravitational-wave observatory (LIGO) and Virgo have provided us a new tool to explore the Universe on all scales from nuclear physics to the cosmos and have the massive potential to further impact fundamental physics, astrophysics, and cosmology for decades to come. In this paper we have studied the science capabilities of a network of LIGO detectors when they reach their best possible sensitivity, called A <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math> , given the infrastructure in which they exist and a new generation of observatories that are factor of 10 to 100 times more sensitive (depending on the frequency), in particular a pair of L-shaped cosmic explorer (CE) observatories (one 40 km and one 20 km arm length) in the US and the triangular Einstein telescope with 10 km arms in Europe. We use a set of science metrics derived from the top priorities of several funding agencies to characterize the science capabilities of different networks. The presence of one or two A <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math> observatories in a network containing two or one next generation observatories, respectively, will provide good localization capabilities for facilitating multimessenger astronomy (MMA) and precision measurement of the Hubble parameter. Two CE observatories are indispensable for achieving precise localization of binary neutron star events, facilitating detection of electromagnetic counterparts and transforming MMA. Their combined operation is even more important in the detection and localization of high-redshift sources, such as binary neutron stars, beyond the star-formation peak, and primordial black hole mergers, which may occur roughly 100 million years after the Big Bang. The addition of the Einstein Telescope to a network of two CE observatories is critical for accomplishing all the identified science metrics including the nuclear equation of state, cosmological parameters, the growth of black holes through cosmic history, but also make new discoveries such as the presence of dark matter within or around neutron stars and black holes, continuous gravitational waves from rotating neutron stars, transient signals from supernovae, and the production of stellar-mass black holes in the early Universe. For most metrics the triple network of next generation terrestrial observatories are a factor 100 better than what can be accomplished by a network of three A <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"><mml:mrow><mml:msup><mml:mrow/><mml:mo>♯</mml:mo></mml:msup></mml:mrow></mml:math> observatories.

Classical and Quantum GravityVol. 41(24)
Australian National University (AU), California Institute of Technology (US), Texas Tech University (US), Pennsylvania State University (US), University of Nevada, Las Vegas (US), California State University, Fullerton (US), Johns Hopkins University (US), Chinese University of Hong Kong (HK), University of Toronto (CA), Chennai Mathematical Institute (IN), Utrecht University (NL), University of Washington (US), University of Michigan (US), University of Florida (US), National Institute for Subatomic Physics (NL), Canadian Institute for Theoretical Astrophysics (CA), Instituto de Física Teórica (ES), Center for Astrophysics Harvard & Smithsonian (US), ARC Centre of Excellence for Gravitational Wave Discovery (AU), Max Planck Institute for Gravitational Physics (DE), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Massachusetts Institute of Technology (US), Syracuse University (US), Friedrich Schiller University Jena (DE), Cardiff University (GB), The University of Texas at Austin (US), KU Leuven (BE)
National Science Foundation, U.S. Department of Energy, National Aeronautics and Space Administration, Department of Science and Technology, Ministry of Science and Technology, India, Indo-US Science and Technology Forum, Deutsche Forschungsgemeinschaft, KU Leuven, Chinese University of Hong Kong, Ministero degli Affari Esteri e della Cooperazione Internazionale, Vlaamse regering, Istituto Nazionale di Fisica Nucleare, NASA Headquarters, Science and Engineering Research Board, Universitaire Ziekenhuizen Leuven, KU Leuven, Division of Physics, Division of Astronomical Sciences, High Energy Physics
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