KAGRA: 2.5 generation interferometric gravitational wave detector

Akutsu, T.; Ando, Masaki; Arai, K.; Arai, Y.; Araki, S.; Araya, Akito; Aritomi, N.; Asada, Hideki; Aso, Y.; Atsuta, S.; Awai, K.; Bae, S.; Baiotti, Luca; Barton, M. A.; Cannon, K. C.; Capocasa, E.; Cs, Chen; Chiu, T-W.; Cho, K.; Chu, Y-K.; Craig, K.; Creus, W.; Doi, Kunio; Eda, Kazunari; Enomoto, Y.; Flaminio, R.; Fujii, Yoshinori; Fujimoto, Masa–Katsu; Fukunaga, Masataka; Fukushima, Mitsuhiro; Furuhata, T.; Haino, S.; Hasegawa, K.; Hashino, Katsuya; Hayama, K.; Hirobayashi, Shigeki; Hirose, E.; Hsieh, B-H.; Huang, C-Z.; Ikenoue, B.; Inoue, Yuki; Ioka, Kunihito; Itoh, Y.; Izumi, K.; Kaji, T.; Kajita, T.; Kakizaki, Mitsuru; Kamiizumi, M.; Kanbara, Shunsuke; Kanda, Nobuyuki; Kanemura, Shinya; Kaneyama, Masato; Kang, G.; Kasuya, J.; Kataoka, Y.; Kawai, N.; Kawamura, Seiji; Kawasaki, T.; Kim, C.; Kim, J.; Kim, J. C.; Kim, W. S.; Kim, Y.-M.; Kimura, N.; Kinugawa, Tomoya; Kirii, S; Kitaoka, Y.; Kitazawa, H.; Kojima, Yasufumi; Kokeyama, K.; Komori, K.; Kong, Albert; Kotake, Kei; Kozu, R.; Kumar, Rakesh; Kuo, H-S.; Kuroyanagi, Sachiko; Lee, H. K.; Lee, H. M.; Lee, H. W.; Leonardi, M.; Lin, C‐Y.; Lin, F-L.; Liu, G. C.; Liu, Y.; Majorana, E.; Mano, Shuhei; Marchio, M.; Matsui, Toshinori; Matsushima, Fusakazu; Michimura, Yuta; Mio, Norikatsu; Miyakawa, O.; Miyamoto, A.; Miyamoto, Takuya; Miyo, K.; Miyoki, S.; Morii, Wataru; Morisaki, S.; Moriwaki, Y.; Morozumi, Tatsuru; Musha, Mitsuru; Nagano, Koji; Nagano, S.; Nakamura, Kouji; Nakamura, Takashi; Nakano, Hiroyuki; Nakano, Masayuki; Nakao, Ken–ichi; Narikawa, T.; Naticchioni, L.; Quynh, L. Nguyen; Ni, W.-T.; Nishizawa, A.; Obuchi, Yasunari; Ochi, T; Oh, J. J.; Oh, Sang Hoon; Ohashi, M.; Ohishi, N.; Ohkawa, Masashi; Okutomi, K.; Ono, Ken; Oohara, K.; Ooi, C.; Pan, S-S; Park, June; Arellano, F. E. Peña; Pinto, I. M.; Sago, Norichika; Saijo, Motoyuki; Saitou, S.; Saitō, Yoshio; Sakai, Kazuki; Sakai, Y.; Sasai, Masahide; Sasaki, Misao; Sasaki, Y.; Sato, S.; Sato, Nobuaki; Sato, T.; Sekiguchi, Y.; Seto, Naoki; Shibata, Masaru; Shimoda, T.; Shinkai, H.; Shishido, T.; Shoda, A.; Somiya, K.; Son, E. J.; Suemasa, Aru; Suzuki, Toshikazu; Tagoshi, Hideyuki; Tahara, Hiroaki W. H.; Takahashi, Hideya; Takahashi, Ryuichi; Takamori, A.; Takeda, H.; Tanaka, H.; Tanaka, Kazuyuki; Tanaka, Takahiro; Tanioka, S.; Martín, E. N. Tapia San; Tatsumi, Daisuke; Tomaru, T.; Tomura, T.; Travasso, F.; Tsubono, K.; Tsuchida, S.; Uchikata, N.; Uchiyama, Takashi; Uehara, T.; Ueki, Satoshi; Ueno, K.; Uraguchi, Fumihiro; Ushiba, T.; Putten, Maurice H. P. M. van; Vocca, H.; Wada, Sumio; Wakamatsu, Takeshi; Watanabe, Yuko; Xu, W-R.; Yamada, Tomohiro; Yamamoto, A.; Yamamoto, K.; Yamamoto, Shun; Yamamoto, Takahiro; Yokogawa, K.; Yokoyama, Jun′ichi; Yokozawa, T.; Yoon, Tai Hyun; Yoshioka, T.; Yuzurihara, H.; Zeidler, S.; Zhu, Z-H

doi:10.1038/s41550-018-0658-y

Cited by 473 publications

(232 citation statements)

References 27 publications

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“…KAGRA, operated in Japan, has two 3 km orthonormal arms to form an underground GW interferometer. It has a similar designed sensitivity as that of the Advanced LIGO [41]. Moreover, the next-generation ground-based detectors are expected to detect more GW events with larger SNRs, due to their even higher sensitivities.…”

Section: A the Setupmentioning

confidence: 99%

Reduced-order surrogate models for scalar-tensor gravity in the strong field regime and applications to binary pulsars and GW170817

et al. 2019

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We investigate the scalar-tensor gravity of Damour and Esposito-Farèse (DEF), which predicts non-trivial phenomena in the nonperturbative strong-field regime for neutron stars (NSs). Instead of solving the modified Tolman-Oppenheimer-Volkoff equations, we construct reduced-order surrogate models, coded in the pySTGROM package, to predict the relations of a NS radius, mass, and effective scalar coupling to its central density. Our models are accurate at ∼ 1% level and speed up large-scale calculations by two orders of magnitude. As an application, we use pySTGROM and Markov-chain Monte Carlo techniques to constrain parameters in the DEF theory, with five well-timed binary pulsars, the binary NS (BNS) inspiral GW170817, and a hypothetical BNS inspiral in the Advanced LIGO and next-generation GW detectors. In the future, as more binary pulsars and BNS mergers are detected, our surrogate models will be helpful in constraining strong-field gravity with essential speed and accuracy.

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Section: A the Setupmentioning

confidence: 99%

Reduced-order surrogate models for scalar-tensor gravity in the strong field regime and applications to binary pulsars and GW170817

et al. 2019

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“…This approach will also bring new ways to test the theory of gravity on cosmological scales and help to validate our two major frameworks, namely Einstein's theory of General Relativity and the LCDM model of cosmology. mukherje@iap.fr † wandelt@iap.fr ‡ silk@iap.fr With the ongoing ground-based gravitational wave observatories such as Advanced-LIGO (Laser Interferometer Gravitational-Wave Observatory) (Abbott et al 2016c), Virgo (Virgo interferometer) (Acernese et al 2015), and with the upcoming observatories such as KAGRA (Large-scale Cryogenic Gravitational wave Telescope) (Akutsu et al 2019) and LIGO-India (Unnikrishnan 2013), we can measure the gravitational wave signals from binary neutron stars (NS-NS), stellar-mass binary black holes (BH-BH), black hole-neutron star (BH-NS) systems over the frequency range 10 − 1000 Hz and up to a redshift of about one. Along with the ground-based gravitational wave detectors, space-based gravitational wave experiment such as LISA (Laser Interferometer Space Antenna) Klein et al (2016) are going to measure the gravitational wave signal emitted from supermassive binary black holes in the frequency range ∼ 10 −4 −10 −1 Hz.…”

Section: Introductionmentioning

confidence: 99%

Probing the theory of gravity with gravitational lensing of gravitational waves and galaxy surveys

Mukherjee

Wandelt

Silk

2020

Monthly Notices of the Royal Astronomical Society

141

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The cross-correlation of gravitational wave events with upcoming galaxy surveys probe theories of gravity in a fundamentally new way, with the potential to reveal clues as to the nature of dark energy and dark matter. We find that within 10 years, the combination of the Advanced-LIGO and VIRGO detector network with planned galaxy surveys can detect weak gravitational lensing of gravitational waves in the low redshift Universe (z < 0.5). With the next generation gravitational wave experiments such as Voyager, LISA, Cosmic-Explorer and Einstein Telescope, we can extend the range of this probe up to a redshift of z ∼ 20. This new probe will test the theory of gravity using both gravitational wave propagation through spacetime and also the effect of cosmic structures on gravitational waves, opening up a new observational window for cosmology and fundamental physics.

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“…GW will provide important constraints for cosmology via standard sirens (multi-messenger detections of GW and electromagentic signals [11]), as they can test the properties of these dynamical dark energy fields as well as provide independent constraints on cosmological parameters such as the current expansion rate of the universe, H 0 , whose current observational constraints exhibit a 4-6σ tension (see review in [12]). In the upcoming years, detectors such as KAGRA [13], LIGO-India [14], the ET [15] and LISA [16] (and possible proposed detectors such as DECIGO [17]) will come online to measure GW with more precision and over cosmological distances.…”

mentioning

confidence: 99%

Standard Sirens as a Novel Probe of Dark Energy

Wolf

Lagos

2020

Phys. Rev. Lett.

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Cosmological models with a dynamical dark energy field typically lead to a modified propagation of gravitational waves via an effectively time-varying gravitational coupling G(t). The local variation of this coupling between the time of emission and detection can be probed with standard sirens. Here we discuss the role that Lunar Laser Ranging (LLR) and binary pulsar constraints play in the prospects of constraining G(t) with standard sirens. In particular, we argue that LLR constrains the matter-matter gravitational coupling G N (t), whereas binary pulsars and standard sirens constrain the quadratic kinetic gravity self-interaction G gw (t). Generically, these two couplings could be different in alternative cosmological models, in which case LLR constraints are irrelevant for standard sirens. We use the Hulse-Taylor pulsar data and show that observations are highly insensitive to time variations of G gw (t), and we thus conclude that future gravitational waves data will become the best probe to test G gw (t), and will hence provide novel constraints on dynamical dark energy models.Introduction.-Gravitational waves (GW) are a longstanding prediction of Einstein's theory of general relativity (GR) and their recent direct detection by the LIGO/Virgo collaboration [1] has confirmed many aspects of GR [2-4] while future tests will offer exciting opportunities to probe the Universe and its constituents even further. In particular, the unknown nature of dark energy -the component driving the observed late-time accelerated expansion of the Universe [5]has motivated a number of alternative models that promote the cosmological constant of the standard ΛCDM model to be a dynamical dark energy field (see e.g. [6][7][8][9][10]). GW will provide important constraints for cosmology via standard sirens (multi-messenger detections of GW and electromagentic signals [11]), as they can test the properties of these dynamical dark energy fields as well as provide independent constraints on cosmological parameters such as the current expansion rate of the universe, H 0 , whose current observational constraints exhibit a 4-6σ tension (see review in [12]). In the upcoming years, detectors such as KAGRA [13], , the ET [15] and LISA [16] (and possible proposed detectors such as DECIGO [17]) will come online to measure GW with more precision and over cosmological distances.One notable non-trivial signature that can be probed with standard sirens is the possibility of a time-varying gravitational coupling G(t), which typically arises in dynamical dark energy models. In this case, the quadratic action for GW that propagate at the speed of light on a cosmological background is typically given by:

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KAGRA: 2.5 generation interferometric gravitational wave detector

Cited by 473 publications

References 27 publications

Reduced-order surrogate models for scalar-tensor gravity in the strong field regime and applications to binary pulsars and GW170817

Reduced-order surrogate models for scalar-tensor gravity in the strong field regime and applications to binary pulsars and GW170817

Probing the theory of gravity with gravitational lensing of gravitational waves and galaxy surveys

Standard Sirens as a Novel Probe of Dark Energy

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