Overview of KAGRA: Detector design and construction history

Akutsu, T.; Ando, M.; Arai, K.; Arai, Y.; Araki, S.; Araya, A.; Aritomi, N.; Aso, Y.; Bae, S. -W.; Bae, Y. -B.; Baiotti, L.; Bajpai, R.; Barton, M. A.; Cannon, K.; Capocasa, E.; Chan, M. -L.; Chen, C. -S.; Chen, K. -H.; Chen, Y. -R.; Chu, H. -Y.; Chu, Y-K.; Eguchi, S.; Enomoto, Y.; Flaminio, R.; Fujii, Y.; Fukunaga, M.; Fukushima, M.; Ge, G. -G.; Hagiwara, A.; Haino, S.; Hasegawa, K.; Hayakawa, H.; Hayama, K.; Himemoto, Y.; Hiranuma, Y.; Hirata, N.; Hirose, E.; Hong, Z.; Hsieh, B. -H.; Huang, G. -Z.; -W., Huang, P.; Huang, Y. -J.; Ikenoue, B.; Imam, S.; Inayoshi, K.; Inoue, Y.; Ioka, K.; Itoh, Y.; Izumi, K.; Jung, K.; Jung, P.; Kajita, T.; Kamiizumi, M.; Kanda, N.; Kang, G. -W.; Kawaguchi, K.; Kawai, N.; Kawasaki, T.; Kim, C.; Kim, J.; Kim, W.; Kim, Y. -M.; Kimura, N.; Kita, N.; Kitazawa, H.; Kojima, Y.; Kokeyama, K.; Komori, K.; Kong, A. K. H.; Kotake, K.; Kozakai, C.; Kozu, R.; Kumar, R.; Kume, J.; Kuo, C. -M.; Kuo, H. -S.; Kuroyanagi, S.; Kusayanagi, K.; Kwak, K.; Lee, H. -K.; Lee, H. -W.; -K., Lee, R.; Leonardi, M.; Lin, C. -Y.; Lin, F. -L.; Lin, L. C. -C.; Liu, G. -C.; Luo, L. -W.; Marchio, M.; Michimura, Y.; Mio, N.; Miyakawa, O.; Miyamoto, A.; Miyazaki, Y.; Miyo, K.; Miyoki, S.; Morisaki, S.; Moriwaki, Y.; Nagano, K.; Nagano, S.; Nakamura, K.; Nakano, H.; Nakano, M.; Nakashima, R.; Narikawa, T.; Negishi, R.; Ni, W. -T.; Nishizawa, A.; Obuchi, Y.; Ogaki, W.; Oh, J. J.; Oh, S. -H.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, K.; Oohara, K.; Ooi, C. -P.; Oshino, S.; Pan, K. -C.; Pang, H. -F.; Park, J.; Arellano, F. E. Peña; Pinto, I.; Sago, N.; Saito, S.; Saito, Y.; Sakai, K.; Sakai, Y.; Sakuno, Y.; Sato, S.; Sato, T.; Sawada, T.; Sekiguchi, T.; Sekiguchi, Y.; Shibagaki, S.; Shimizu, R.; Shimoda, T.; Shimode, K.; Shinkai, H.; Shishido, T.; Shoda, A.; Somiya, K.; Son, E. J.; Sotani, H.; Sugimoto, R.; Suzuki, T.; Tagoshi, H.; Takahashi, H.; Takahashi, R.; Takamori, A.; Takano, S.; Takeda, H.; Takeda, M.; Tanaka, H.; Tanaka, K.; Tanaka, K.; Tanaka, T.; Tanaka, T.; Tanioka, S.; Martín, E. N. Tapia San; Telada, S.; Tomaru, T.; Tomigami, Y.; Tomura, T.; Travasso, F.; Trozzo, L.; Tsang, T.; Tsubono, K.; Tsuchida, S.; Tsuzuki, T.; Tuyenbayev, D.; Uchikata, N.; Uchiyama, T.; Ueda, A.; Uehara, T.; Ueno, K.; Ueshima, G.; Uraguchi, F.; Ushiba, T.; Putten, Maurice H. P. M. van; Vocca, H.; Wang, J.; Wu, C. -M.; Wu, H. -C.; Wu, S. -R.; Xu, W. -R.; Yamada, T.; Yamamoto, Ka.; Yamamoto, Ko.; Yamamoto, T.; Yokogawa, K.; Yokoyama, J.; Yokozawa, T.; Yoshioka, T.; Yuzurihara, H.; Zeidler, S.; Zhao, Y.; Zhu, Z. -H.

doi:10.48550/arxiv.2005.05574

Cited by 56 publications

(79 citation statements)

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“…The success of ground-breaking ground-based experiments in measuring gravitational waves (GWs) in recent years, since the first detection from a merger of a binary black hole [1] by the Advanced LIGO [2] and the Advanced VIRGO [3] collaboration has exceeded most expectations. By now there is an operational worldwide network of GW detectors of second generation technology, as the twin Advanced LIGO detectors in the US have been joined by the Advanced Virgo detector in Europe [3], and more recently also by the KAGRA detector in Japan [4]. These experiments have been continually reaching higher sensitivities, which yield more frequent GW detections, and the influx of GW data has been steeply growing [5][6][7].…”

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confidence: 99%

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Quadratic-in-spin interactions at fifth post-Newtonian order probe new physics

Kim,

Levi,

Yin

2021

Preprint

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We derive the observable binding energies and their relations to the angular momentum for the next-to-next-to-next-to-leading order (N 3 LO) of all quadratic-in-spin interactions in post-Newtonian (PN) gravity. Our results are valid for all generic compact binaries, and enter at the fifth PN order for maximally-rotating compact objects, thus pushing the state of the art. This is accomplished through an extension of the effective field theory of spinning gravitating objects. We find a new operator that contributes to the observables at this order, making the associated Wilson coefficient a new probe for candidate theories of gravity and for QCD.

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confidence: 99%

“…These terms involve new Wilson coefficients, that at this point absorb all numerical and mass factors, in contrast with those in (4). The terms on the second line of (7) are a new type of operators that would be relevant only for spinning objects.…”

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confidence: 99%

Quadratic-in-spin interactions at fifth post-Newtonian order probe new physics

Kim,

Levi,

Yin

2021

Preprint

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“…Inference of the cosmological parameters from the gravitational wave (GW) sources is one of the key science goals of the currently ongoing network of GW detectors (Abbott et al 2018) such as LIGO (Aasi et al 2015), Virgo (Acernese et al 2014), and for the upcoming GW detectors such as KAGRA (Akutsu et al 2020), LIGO-India (Unnikrishnan 2013), LISA (Amaro-Seoane et al 2017), Cosmic Explorer (Reitze et al 2019;Hall & Evans 2019), and Einstein Telescope (Punturo et al 2010), as it can provide accurate measurement to the luminosity distance of the GW sources within the framework of the general theory of relativity, and without invoking any additional distance calibration. This was shown for the first time in the seminal work by Schutz (1986), which justifies the reason for calling GW sources the standard sirens.…”

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confidence: 99%

The redshift dependence of black hole mass distribution: Is it reliable for standard sirens cosmology?

Mukherjee¹

2021

Preprint

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An upper limit on the mass of a black hole set by the pair-instability supernovae (PISN) process can be useful in inferring the redshift of the gravitational wave (GW) sources by lifting the degeneracy between mass and redshift. However, for this technique to work, it is essential that the PISN mass-scale is redshift independent or at least has a predictable redshift dependence. We show that the observed PISN mass-scale is likely to exhibit a strong redshift dependence due to a non-zero value of the delay time between the formation of a star and the merging of two black holes. This will lead to a merger of black holes formed at a different cosmic time, over which the stellar metallicity of the parent star can vary significantly. As a result, the observed PISN mass scale inferred from GW sources will be redshift dependent. Due to the unknown form of the delay-time distribution, the redshift dependence of the PISN mass cut-off of the binary black holes (BBHs) cannot be well characterized and will exhibit a large variation with the change in redshift. As a result, the use of a fixed PISN mass scale to infer the redshift of the BBHs from the observed masses will be systematically biased. Though this uncertainty is not severe for the third observation run conducted by the LIGO-Virgo-KAGRA collaboration, in the future this uncertainty will cause a systematic error in the redshift inferred from PISN mass scale. The corresponding systematic error will be a bottleneck in achieving a few percent precision measurements of the cosmological parameters using this method in the future. The origin of the redshift dependence of the mass distribution of BBHs proposed in this analysis will also be useful for understanding the population of GW sources inferred using both well-detected events and the stochastic GW background.

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“…Since the first detection, by the Advanced LIGO [1] and Advanced VIRGO [2] collaboration, of gravitational waves (GWs) from a merger of a binary black hole [3], we have been rapidly shifting to a new era of gravitationalwave astronomy. At present we already have a worldwide network of next-generation ground-based GW experiments, including the twin Advanced LIGO detectors in the US, Advanced Virgo in Europe [2], and the more recent experiment KAGRA in Japan [4]), and this network is expected to quickly expand and improve. These experiments will continue to provide a steeply increasing influx of GW data of higher quality [5][6][7].…”

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confidence: 99%

“…where the entries in the 4-loop master integrals F (4) denote the exponents of the 10 denominators, and we suppress labels for various iǫ prescriptions, and dependence in ω of the coefficients to be fixed from evaluating the corresponding cuts.…”

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confidence: 99%

A tale of tails through generalized unitarity

Edison¹,

Levi²

2022

Preprint

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We introduce a novel framework to study high-order gravitational effects on a binary from the scattering of its emitted gravitational radiation. Here we focus on the radiation-reaction due to the background of the binary's gravitational potential, namely on the so-called tail effects. We start from the effective field theory of a binary composite particle, and through multi-loop and generalized unitarity methods, we derive the effective action of the dynamical multipoles, the energy spectrum, and the observable flux due to these effects. We proceed through the third subleading such radiationreaction effect -at the four-loop level and the seventh order in post-Newtonian gravity -shedding new light on the higher-order effects, and completing the state of the art.

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Overview of KAGRA: Detector design and construction history

Cited by 56 publications

References 0 publications

Quadratic-in-spin interactions at fifth post-Newtonian order probe new physics

Quadratic-in-spin interactions at fifth post-Newtonian order probe new physics

The redshift dependence of black hole mass distribution: Is it reliable for standard sirens cosmology?

A tale of tails through generalized unitarity

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