Author: "Zong, Hong" / Topic: physics - Searchworks@Jio Institute Digital Library Search Results

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244 results on '"Zong, Hong"'

1. Towards a reliable reconstruction of the power spectrum of primordial curvature perturbation on small scales from GWTC-3

Author: Li-Ming Zheng, Zhengxiang Li, Zu-Cheng Chen, Huan Zhou, and Zong-Hong Zhu
Subjects: Physics, QC1-999
Abstract: Primordial black holes (PBHs) can be both candidates of dark matter and progenitors of binary black holes (BBHs) detected by the LIGO-Virgo-KAGRA collaboration. Since PBHs could form in the very early Universe through the gravitational collapse of primordial density perturbations, the population of BBHs detected by gravitational waves encodes much information on primordial curvature perturbation. In this work, we take a reliable and systematic approach to reconstruct the power spectrum of the primordial curvature perturbation from GWTC-3, under the hierarchical Bayesian inference framework, by accounting for the measurement uncertainties and selection effects. In addition to just considering the single PBH population model, we also report the results considering the multi-population model, i.e., the mixed PBH and astrophysical black hole binaries model. We find that the maximum amplitude of the reconstructed power spectrum of primordial curvature perturbation can be ∼2.5×10−2 at O(105)Mpc−1 scales, which is consistent with the PBH formation scenario from inflation at small scales.
Published: 2023
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2. Optimized localization for gravitational waves from merging binaries

Author: Eric Thrane, Xing-Jiang Zhu, Gregory Ashton, Zhi-Qiang You, and Zong-Hong Zhu
Subjects: Physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Bayesian inference, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, General Relativity and Quantum Cosmology, Neutron star, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The Advanced LIGO and Virgo gravitational wave observatories have opened a new window with which to study the inspiral and mergers of binary compact objects. These observations are most powerful when coordinated with multi-messenger observations. This was underlined by the first observation of a binary neutron star merger GW170817, coincident with a short Gamma-ray burst, GRB170817A, and the identification of the host galaxy NGC~4993 from the optical counterpart AT~2017gfo. Finding the fast-fading optical counterpart critically depends on the rapid production of a sky-map based on LIGO/Virgo data. Currently, a rapid initial sky map is produced followed by a more accurate, high-latency, $\gtrsim{12}{\rm{hr}}$ sky map. We study optimization choices of the Bayesian prior and signal model which can be used alongside other approaches such as reduced order quadrature. We find these yield up to a $60\%$ reduction in the time required to produce the high-latency localisation for binary neutron star mergers., 9 pages, 10 figures, accepted to MNRAS
Published: 2021
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3. Constraining cosmological parameters from strong lensing with DECIGO and B-DECIGO sources

Author: Zong-Hong Zhu, Shaoqi Hou, and Xi-Long Fan
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational wave, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Omega, General Relativity and Quantum Cosmology, Cosmology, LIGO, Redshift, symbols.namesake, Gravitational lens, Space and Planetary Science, symbols, Luminosity distance, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: Gravitational lensing has long been used to measure or constrain cosmology models. Although the lensing effect of gravitational waves has not been observed by LIGO/Virgo, it is expected that there can be a few to a few hundreds lensed events to be detected by the future Japanese space-borne interferometers DECIGO and B-DECIGO, if they are running for 4 years. Given the predicted lensed gravitational wave events, one can estimate the constraints on the cosmological parameters via the lensing statistics and the time delay methods. With the lensing statistics method, the knowledge of the lens redshifts, even with the moderate uncertainty, will set the tight bound on the energy density parameter $\Omega_M$ for matter, that is, $0.288\lesssim\Omega_M\lesssim0.314$ at best. The constraint on the Hubble constant $H_0$ can be determined using the time delay method. It is found out that at $5\sigma$, $|\delta H_0|/H_0$ ranges from $3\%$ to $11\%$ for DECIGO, and B-DECIGO will give less constrained results, $8\%-15\%$. In this work, the uncertainties on the luminosity distance and the time delay distance are set to be $10\%$ and $20\%$, respectively. The improvement on measuring these distances will tighten the bounds., Comment: 11 pages, 13 figures. Revised according to Referee's comments
Published: 2021
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4. Intraday multiband optical variability of BL Lacertae object S5 0716+714

Author: Xiaoyuan Zhang, Yan Dai, Zong-Hong Zhu, Yue Fang, Jianghua Wu, and Nankun Meng
Subjects: Physics, Space and Planetary Science, Astronomy and Astrophysics, Astrophysics, BL Lac object
Abstract: We monitored the BL Lac object S5 0716+714 in four optical wavebands with four telescopes on 11 nights from 2012 to 2017. The object was active during most of those nights. It was brightest on 2012 November 7 with 11.720 mag in the I band and reached the faintest state on 2016 January 22 with 15.770 mag in the R band corresponding to ∼15.230 mag in the I band. Intraday variations in all bands were found on 6 d, while in partial bands on 3 d. Strong bluer-when-brighter chromatism was observed on 8 nights. Correlation analyses revealed interband time delays from 4 to 40 min in the intraday variability on 5 nights. Both hard and soft lags were observed in this object, indicating complicated emission process in the jet. The analysis on the interband time delays indicated that the radiative cooling may dominate the optical time lags in S5 0716+714 occasionally, but cannot be invoked as the sole explanation.
Published: 2021
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5. Axial Magnetic Force Analysis and Optimized Design for Single-Phase BLDC Slim Fan Motors

Author: Yie-Tone Chen, Ruey-Hsun Liang, Zong-Hong Tang, and Yen-Kun Liou
Subjects: Physics, Stator, Acoustics, 020208 electrical & electronic engineering, Ripple, Phase (waves), 02 engineering and technology, Magnetic flux, law.invention, Magnetic field, Vibration, Magnetic circuit, Control and Systems Engineering, law, Magnet, 0202 electrical engineering, electronic engineering, information engineering, Electrical and Electronic Engineering
Abstract: The typical manner to generate the axial magnetic force is to utilize the magnetic path design by upward magnet offset (UMO) that is the permanent magnet (PM) shifted upward relative to the stator in the single-phase BLDC slim fan motors. The other special method is to increase a permeable material, with an air-gap (AG i-m ), under the PM to generate the axial magnetic force. The axial magnetic force and its ripples are the important factors in the slim fan design and will further affect the performances of the acoustic noise and axial vibration. In this article, a magnetic circuit model is constructed to execute the mathematical theoretical analysis of the magnetic field. The trait of the phase opposition between the magnetic force ripples generated in the stator core and lower iron plate is used to optimize the ripple of the total axial magnetic force by the offset effect, and in the meantime, to remain the desirous average value. A 3-D model is created to execute the finite-element analysis and simulation. The cross-matching simulation among the different degrees of UMO and AGi-m is executed and an optimized model is defined. A solid model of a slim fan motor is verified in the practical experiment, and the results present the effectiveness in the reduction of acoustic noise and vibration.
Published: 2021
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6. Hubble diagram at higher redshifts: model independent calibration of quasars

Author: Zong-Hong Zhu, Ryan E. Keeley, Xiaogang Zheng, Shuo Cao, Arman Shafieloo, Xiaolei Li, and Marek Biesiada
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), Lambda, Omega, Redshift, Luminosity, Supernova, Space and Planetary Science, Range (statistics), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In this paper, we present a model-independent approach to calibrate the largest quasar sample. Calibrating quasar samples is essentially constraining the parameters of the linear relation between the $\log$ of the ultraviolet (UV) and X-ray luminosities. This calibration allows quasars to be used as standardized candles. There is a strong correlation between the parameters characterizing the quasar luminosity relation and the cosmological distances inferred from using quasars as standardized candles. We break this degeneracy by using Gaussian process regression to model-independently reconstruct the expansion history of the Universe from the latest type Ia supernova observations. Using the calibrated quasar dataset, we further reconstruct the expansion history up to redshift of $z\sim 7.5$. Finally, we test the consistency between the calibrated quasar sample and the standard $\rm{\Lambda}CDM$ model based on the posterior probability distribution of the GP hyperparameters. Our results show that the quasar sample is in good agreement with the standard $\rm{\Lambda}CDM$ model in the redshift range of the supernova, despite of mildly significant deviations taking place at higher redshifts. Fitting the standard $\rm{\Lambda}CDM$ model to the calibrated quasar sample, we obtain a high value of the matter density parameter $\Omega_m = 0.382^{+0.045}_{-0.042}$, which is marginally consistent with the constraints from other cosmological observations., Comment: 9 pages, 7 figures
Published: 2021
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7. Redshift evolution of the Amati relation: calibrated results from the Hubble diagram of quasars at high redshifts

Author: Yan Dai, Xiao-Gang Zheng, He Gao, Zong-Hong Zhu, and Zhengxiang Li
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Cosmic distance ladder, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Cosmology, Luminosity, Supernova, Space and Planetary Science, 0103 physical sciences, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: Gamma-ray bursts (GRBs) have long been proposed as a complementary probe to type Ia supernovae (SNe Ia) and the cosmic microwave background to explore the expansion history of the high-redshift universe, mainly because they are bright enough to be detected at greater distances. Although they lack definite physical explanations, many empirical correlations between GRB isotropic energy or luminosity and some directly detectable spectral or temporal properties have been proposed to make GRBs standard candles. Since the observed GRB rate falls off rapidly at low redshifts, this thus prevents a cosmology independent calibration of these correlations. In order to avoid the circularity problem, SN Ia data are usually used to calibrate the luminosity relations of GRBs in the low redshift region (limited by the redshift range for SN Ia sample), and then they are extrapolate the luminosity relations to the high redshift region. This approach is based on the assumption of no redshift evolution for GRB luminosity relations. In this work, we suggest the use of a complete quasar sample in the redshift range of 0.5 z γ-ray equivalent energy of GRBs in relevant redshift bins. By fitting the newly calibrated data, we find strong evidence that the most commonly used Amati relation between spectral peak energy and isotropic-equivalent radiated energy shows no, or marginal, evolution with redshift. Indeed, at different redshifts, the coefficients in the Amati relation could have a maximum variation of 0.93% at different redshifts, and there could be no coincidence in the range of 1σ.
Published: 2021

8. Cosmological consequences of a scalar field with oscillating equation of state. III. Unifying inflation with dark energy and small tensor-to-scalar ratio

Author: Shuxun Tian and Zong-Hong Zhu
Subjects: Inflation (cosmology), Physics, Spectral index, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Equation of state (cosmology), media_common.quotation_subject, Scalar (mathematics), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Universe, symbols.namesake, 0103 physical sciences, symbols, Dark energy, Planck, 010306 general physics, Scalar field, Astrophysics - Cosmology and Nongalactic Astrophysics, Mathematical physics, media_common
Abstract: We investigate the inflationary consequences of the oscillating dark energy model proposed by Ti��n [\href{https://doi.org/10.1103/PhysRevD.101.063531}{Phys. Rev. D {\bf 101}, 063531 (2020)}], which aims to solve the cosmological coincidence problem with multi-accelerating Universe (MAU). We point out that the inflationary dynamics belong to slow-roll inflation. The spectral index of scalar perturbations and the tensor-to-scalar ratio $r$ are shown to be consistent with current \textit{Planck} measurements. Especially, this model predicts $r\sim10^{-7}$, which is far below the observation limits. This result motivates us to explore the smallness of $r$ in the general MAU. We propose a quintessential generalization of the original model and prove $r, 8 pages, 3 figures, published in Phys. Rev. D
Published: 2021
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9. Overview of KAGRA: Calibration, detector characterization, physical environmental monitors, and the geophysics interferometer

Author: R. Shimizu, Ettore Majorana, H. B. Jin, P. Jung, M. Fukunaga, G-Z. Huang, F. E. Peña Arellano, H. Pang, Kunihiro Nagano, John J. Oh, Atsushi Nishizawa, M. Nakano, C. Kozakai, Yasufumi Kojima, S. Saito, Takayuki Tomaru, T. Tomura, Y. Fujikawa, Kazuhiro Hayama, Hajime Sotani, Shigeo Nagano, Masatake Ohashi, S. Otabe, Naoki Aritomi, Chunglee Kim, Tatsuhiro Yamada, Kipp Cannon, Shuen De Wu, Yuhang Zhao, Fumihiro Uraguchi, Hideki Asada, Ryutaro Takahashi, Kei Kotake, Yutaro Enomoto, Naoko Ohishi, L. W. Luo, K. Inayoshi, S. Bae, S. Ha, Sadakazu Haino, T. Narikawa, Yoshiyuki Obuchi, Ryo Yamazaki, K. Hattori, Y. Tomigami, K. Ueno, Zhoujian Cao, Keiko Kokeyama, Kentaro Somiya, G. Ge, K. Yamashita, Wei-Tou Ni, Satoshi Tsuchida, Takashi Sato, M. Zhan, Akiteru Takamori, Masaki Ando, Y. Nakayama, F. K. Lin, W-R. Xu, T. Sawada, Seog Oh, Ray-Kuang Lee, C. P. Ooi, C. Chen, Takahiro Tanaka, S. Ide, H. Vocca, J. Wang, Albert K. H. Kong, T. Yoshioka, Lijing Shao, T. Shimoda, Y. Okutani, R. Flaminio, S. Eguchi, T. Sekiguchi, Y. Sakuno, R. Kozu, Hyang Woon Lee, Zong-Hong Zhu, Y. Hiranuma, Wen-Biao Han, Hideaki Hayakawa, K. Chen, Y. Mori, Yuki Fujii, H. Ohta, Y. Miyazaki, A. Shoda, B. H. Hsieh, Y. Sakai, K. Sakai, S. Oshino, T. Ushiba, Luca Baiotti, Simon Zeidler, Yousuke Itoh, Hiroyuki Nakano, Takaaki Kajita, Yuki Inoue, S. Shibagaki, Hiroyuki Takeda, Chau Ron Wu, Y-K. Chu, M. Kamiizumi, Guo-Chin Liu, Yoshiaki Himemoto, I. M. Pinto, S. Sato, Y. Kuromiya, Yuta Michimura, N. Hirata, A. Miyamoto, Y. Huang, K. L. Li, Yi Chen, Yuichiro Sekiguchi, Kimio Tsubono, Hideyuki Tagoshi, S. Imam, H. L. Lin, M. Chan, Rajesh Kumar, L. C.C. Lin, K. Kusayanagi, K. Okutomi, D. C. Y. Hui, Sachiko Kuroyanagi, K. Kaihotsu, J. Kim, Jinsook Kim, K. Ito, Takashi Uchiyama, Kunihito Ioka, L. Nguyen Quynh, K. Yokogawa, R. Bajpai, K. Shimode, Norikatsu Mio, Koya Arai, Toshihiro Tsuzuki, L. Naticchioni, T. Shishido, R. Nakashima, M. Takeda, Akito Araya, A. Parisi, T. Yokozawa, E. N. Tapia San Martin, Souichi Telada, M. H. P. M. van Putten, Jishnu Suresh, Y. Arai, K. Miyo, K. Oohara, N. Kawai, Soichiro Morisaki, C. Jeon, W. S. Kim, T. Uehara, Jun'ichi Yokoyama, Nobutada Kimura, K. Oh, D. Tuyenbayev, Kentaro Komori, N. Kita, T. Kawasaki, T. Tsang, Hong Wu, Yi Yang, Kuo-Chuan Pan, S. Tanioka, K. Jung, A. Hagiwara, D. Gao, R. Negishi, C-Y. Lin, E. Capocasa, Shinji Miyoki, H. Chu, G. Ueshima, Tomotada Akutsu, M. A. Barton, Y. M. Kim, C-Y. Chiang, Hisa-aki Shinkai, L. Trozzo, Norichika Sago, K. Kwak, J. Kume, Takahiro Yamamoto, Nobuyuki Kanda, S. Nozaki, H. K. Tanaka, H. Yuzurihara, Masako Kakizaki, Eiichi Hirose, Kouji Nakamura, F-L. Lin, M. Leonardi, Haruki Kitazawa, J-S. Tsao, Takuya Tsutsui, M. Marchio, Yoichi Aso, J. Park, K. Izumi, F. Travasso, Hirotaka Takahashi, Nami Uchikata, Mitsuhiro Fukushima, H. Y. Huang, G. Kang, H. Zhang, A. Ueda, Sakae Araki, Osamu Miyakawa, Chin Guo Kuo, Y. Moriwaki, K. Yamamoto, Toshio Suzuki, Hyun Lee, Y. Bae, Masashi Ohkawa, K. Hasegawa, T. Washimi, Kyohei Kawaguchi, B. Ikenoue, H-S. Kuo, P. W. Huang, Kazuyuki Tanaka, Y. Saito, S. Takano, E. J. Son, W. Ogaki, Z. Hong, R. Sugimoto, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and KAGRA
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], data acquisition, interferometer, General Physics and Astronomy, FOS: Physical sciences, detector: noise, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Optics, 0103 physical sciences, Calibration, detector: calibration, KAGRA, laser: interferometer, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, 010308 nuclear & particles physics, business.industry, geophysics, Detector, gravitational radiation, KAGRA gravitational wave kamioka, gravitational radiation detector, Characterization (materials science), detector: sensitivity, Interferometry, F32 Calibration and operation of gravitational wave detector, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, Astrophysics - Instrumentation and Methods for Astrophysics, business, detector: sensitivity, data acquisition, interferometer, geophysics, detector: noise, detector: calibration, KAGRA, gravitational radiation detector, gravitational radiation, laser: interferometer
Abstract: KAGRA is a newly built gravitational wave observatory, a laser interferometer with a 3 km arm length, located in Kamioka, Gifu, Japan. In this series of articles, we present an overview of the baseline KAGRA, for which we finished installing the designed configuration in 2019. This article describes the method of calibration (CAL) used for reconstructing gravitational wave signals from the detector outputs, as well as the characterization of the detector (DET). We also review the physical environmental monitors (PEM) system and the geophysics interferometer (GIF). Both are used for characterizing and evaluating the data quality of the gravitational wave channel. They play important roles in utilizing the detector output for gravitational wave searches. These characterization investigations will be even more important in the near future, once gravitational wave detection has been achieved, and in using KAGRA in the gravitational wave astronomy era., Comment: 2021/02/08 Accepted by PTEP
Published: 2021
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10. Current status of space gravitational wave antenna DECIGO and B-DECIGO

Author: Ken-ichi Oohara, Takahiro Ito, Shuichiro Yokoyama, Kiyotomo Ichiki, Akito Araya, Shoki Iwaguchi, Tomohiro Harada, Seiji Kawamura, Masaru Shibata, Hirotaka Takahashi, Keisuke Taniguchi, Chul-Moon Yoo, Shinji Tsujikawa, Kazunori Kohri, Fumiko Kawazoe, Yoshiaki Himemoto, Shin-ichiro Sakai, Ayaka Shoda, Zong Hong Zhu, Keiichi Maeda, Motohiro Enoki, Taigen Morimoto, Shinichi Nakasuka, Hisa-aki Shinkai, Shuhei Matsushita, Hiroyuki Nakano, Yoshinori Nakayama, Motoyuki Saijo, Masa-aki Sakagami, Takamori Akiteru, Ryutaro Takahashi, Takeo Naito, Kazuhiro Hayama, Rika Yamada, Shinya Kanemura, Kazuhiro Agatsuma, Takashi Hiramatsu, S. Eguchi, Shuichi Sato, Kunihito Ioka, Feng-Lei Hong, Hideki Ishihara, Takeshi Chiba, Akitoshi Ueda, Kei Kotake, Tomotada Akutsu, Hideki Asada, Mitsuru Musha, Takashi Nakamura, Yuta Michimura, Shiho Kobayashi, Ken-ichi Nakao, K. Tsubono, Keiko Kokeyama, Kentaro Somiya, Toshifumi Futamase, Masa Katsu Fujimoto, Masashi Ohkawa, Masaki Ando, Naoki Seto, Shigeo Nagano, Mizuhiko Hosokawa, K. Izumi, Ken-ichi Ueda, Tomohiro Ishikawa, Takahiro Tanaka, Norichika Sago, Takeshi Takashima, Naoki Aritomi, Shinji Mukohyama, Satoshi Ikari, Yousuke Itoh, Atsushi Nishizawa, Atsushi Taruya, Isao Kawano, Ryuichi Fujita, Kent Yagi, Koji Nagano, Nobuyuki Kanda, Kouji Nakamura, Sachiko Kuroyanagi, Yasufumi Kojima, Hajime Sotani, Kazuhiro Nakazawa, Takashi Sato, Jun'ichi Yokoyama, and Izumi Watanabe
Subjects: Gravitational-wave observatory, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Metric expansion of space, 0103 physical sciences, F30 Instrumentation and technique, 010306 general physics, QC, QB, Physics, Spacecraft, 010308 nuclear & particles physics, Gravitational wave, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Black hole, Neutron star, Interferometry, F31 Expectation and estimation of gravitational radiation, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, business, Heliocentric orbit
Abstract: Deci-hertz Interferometer Gravitational Wave Observatory (DECIGO) is the future Japanese space mission with a frequency band of 0.1 Hz to 10 Hz. DECIGO aims at the detection of primordial gravitational waves, which could be produced during the inflationary period right after the birth of the universe. There are many other scientific objectives of DECIGO, including the direct measurement of the acceleration of the expansion of the universe, and reliable and accurate predictions of the timing and locations of neutron star/black hole binary coalescences. DECIGO consists of four clusters of observatories placed in the heliocentric orbit. Each cluster consists of three spacecraft, which form three Fabry-Perot Michelson interferometers with an arm length of 1,000 km. Three clusters of DECIGO will be placed far from each other, and the fourth cluster will be placed in the same position as one of the three clusters to obtain the correlation signals for the detection of the primordial gravitational waves. We plan to launch B-DECIGO, which is a scientific pathfinder of DECIGO, before DECIGO in the 2030s to demonstrate the technologies required for DECIGO, as well as to obtain fruitful scientific results to further expand the multi-messenger astronomy., Comment: 10 pages, 3 figures
Published: 2021

11. Event rate predictions of strongly lensed gravitational waves with detector networks and more realistic templates

Author: Zhiqiang You, Lilan Yang, Shichao Wu, Xuheng Ding, Kai Liao, Zong-Hong Zhu, Marek Biesiada, and Zhoujian Cao
Subjects: Physics, COSMIC cancer database, Einstein Telescope, Gravitational wave, Monte Carlo method, Detector, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Event (particle physics), Earth's rotation
Abstract: Strong lensing of gravitational waves (GWs) is attracting growing attention of the community. The event rates of lensed GWs by galaxies were predicted in numerous papers, which used some approximations to evaluate the GW strains detectable by a single detector. The joint-detection of GW signals by a network of instruments will increase the detecting ability of fainter and farther GW signals, which could increase the detection rate of the lensed GWs, especially for the 3rd generation detectors, e.g., Einstein Telescope (ET) and Cosmic Explorer (CE). Moreover, realistic GW templates will improve the accuracy of the prediction. In this work, we consider the detection of galaxy-scale lensed GW events under the 2nd, 2.5th, and 3rd generation detectors with the network scenarios and adopt the realistic templates to simulate GW signals. Our forecast is based on the Monte Carlo technique which enables us to take Earth's rotation into consideration. We find that the overall detection rate is improved, especially for the 3rd generation detector scenarios. More precisely, it increases by ~37% adopting realistic templates, and under network detection strategy, further increases by ~58% comparing with adoption of the realistic templates, and we estimate that the 3rd generation GW detectors will detect hundreds lensed events per year. The effect from the Earth's rotation is weakened in the detector network strategy., 7pages, 1 figure, accepted by MNRAS
Published: 2021

12. Primordial black holes and scalar-induced secondary gravitational waves from inflationary models with a noncanonical kinetic term

Author: Zong-Hong Zhu, Zhu Yi, Yungui Gong, and Qing Gao
Subjects: Physics, Gravitational-wave observatory, 010308 nuclear & particles physics, Gravitational wave, Dark matter, Scalar (mathematics), Spectral density, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Pulsar, 0103 physical sciences, Production (computer science), 010306 general physics
Abstract: With the enhancement mechanism provided by a noncanonical kinetic term with a peak, the amplitude of primordial curvature perturbations can be enhanced by seven orders of magnitude at small scales while keeping to be consistent with observations at large scales. The peak function and inflationary potential are not restricted in this mechanism. We use the Higgs model and T-model as examples to show how abundant primordial black hole dark matter with different mass and scalar induced secondary gravitational waves with different peak frequency are generated. We also show that the enhanced power spectrum for the primordial curvature perturbations and the energy density of the scalar induced secondary gravitational waves can have either a sharp peak or a broad peak. The primordial black holes with the mass around ${10}^{\ensuremath{-}14}\ensuremath{-}{10}^{\ensuremath{-}12}\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ produced with the enhancement mechanism can make up almost all dark matter, and the scalar induced secondary gravitational waves accompanied with the production of primordial black holes can be tested by the pulsar timing arrays and spaced based gravitational wave observatory. Therefore, the mechanism can be tested by primordial black hole dark matter and gravitational wave observations.
Published: 2021
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13. Primordial black holes and secondary gravitational waves from the Higgs field

Author: Yungui Gong, Zong-Hong Zhu, Bin Wang, and Zhu Yi
Subjects: High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Cosmic microwave background, Dark matter, FOS: Physical sciences, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, 010306 general physics, media_common, Inflation (cosmology), Physics, 010308 nuclear & particles physics, Gravitational wave, Universe, Higgs field, High Energy Physics - Theory (hep-th), Higgs boson, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We devise a novel mechanism and for the first time demonstrate that the Higgs model in particle physics can drive the inflation to satisfy the cosmic microwave background observations and simultaneously enhance the curvature perturbations at small scales to explain the abundance of dark matter in our universe in the form of primordial black holes. The production of primordial black holes is accompanied by the secondary gravitational waves induced by the first order Higgs fluctuations which is expected observable by space-based gravitational wave detectors. We propose possible cosmological probes of Higgs field in the future observations for primordial black holes dark matter or stochastic gravitational waves., added discussion on the running of the self-coupling, published in PRD
Published: 2021
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14. Early dark energy in k -essence

Author: Shuxun Tian and Zong-Hong Zhu
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Order (ring theory), General Relativity and Quantum Cosmology (gr-qc), Dynamical system, General Relativity and Quantum Cosmology, Coincidence, Physical cosmology, Theoretical physics, Dark energy, Neutrino, Scalar field, Energy (signal processing), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Early dark energy (EDE) that becomes subdominant around the epoch of matter-radiation equality can be used to ease the Hubble tension. However, there is a theoretical problem that why the energy scale of EDE is in coincidence with that of matter-radiation equality when their physics are completely unrelated. Sakstein and Trodden [Phys. Rev. Lett. 124, 161301 (2020)] proposed a mechanism to solve this coincidence problem with $\mathcal{O}({\rm eV})$-mass neutrino. In this paper, in order to solve the coincidence problem, we propose a new scenario for EDE, in which the onset and ending of EDE are triggered by the radiation-matter transition. The specific example we study is a $k$-essence model. The cosmic evolution equations can be recast into a two-dimensional dynamical system and its main properties are analyzed. Our results suggest that $k$-essence seems unable to realize the new scenario for EDE. However, an EDE model with different scenario is realized in $k$-essence. In this model, the ending of EDE can be triggered by the radiation-matter transition while the onset depends on the initial conditions of the scalar field. Therefore, the obtained model can only be used to solve half of the coincidence problem. The full resolution in the framework of our initial proposed scenario is worthy of more research., Comment: 5 pages, 2 figures, published in Phys. Rev. D
Published: 2021
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15. Gravitational memory effects and Bondi-Metzner-Sachs symmetries in scalar-tensor theories

Author: Shaoqi Hou and Zong-Hong Zhu
Subjects: High Energy Physics - Theory, Nuclear and High Energy Physics, Angular momentum, General relativity, Lorentz transformation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Lorentz group, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Tensor, 010306 general physics, Mathematical physics, Physics, 010308 nuclear & particles physics, Space-Time Symmetries, Scalar (physics), Equations of motion, Null (physics), High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), Gauge Symmetry, symbols, lcsh:QC770-798, Classical Theories of Gravity
Abstract: The relation between gravitational memory effects and Bondi-Metzner-Sachs symmetry of the asymptotically flat spacetimes is studied in the scalar-tensor theory. For this purpose, the solutions to the equations of motion near the future null infinity are obtained in the generalized Bondi-Sachs coordinates with a suitable determinant condition. It turns out that the Bondi-Metzner-Sachs group is also a semi-direct product of an infinitesimal dimensional supertranslation group and the Lorentz group as in general relativity. There are also degenerate vacua in both the tensor and the scalar sectors in the scalar-tensor theory. The supertranslation relates the vacua in the tensor sector, while in the scalar sector, it is the Lorentz transformation that transforms the vacua to each other. So there are the tensor memory effect similar to the one in general relativity, and the scalar memory effect, which is new. The evolution equations for the Bondi mass and angular momentum aspects suggest that the null energy fluxes and the angular momentum fluxes across the null infinity induce the transition among the vacua in the tensor and the scalar sectors, respectively., Comment: 29 pages, 2 figures. Add discussions on KK reduction, and soft theorems. Feynman diagrams were fixed. Correct typos
Published: 2021
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16. Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo's first three observing runs

Author: A. Grimaldi, M. A. Barton, Samuele Cortese, Charlie Hoy, Charalampos Markakis, L. Trozzo, Albert Lazzarini, Benno Willke, A. Grado, P. Booker, C. Cahillane, Norichika Sago, J. Hennig, V. Gayathri, J. Baird, M. Jeunon, Sascha Husa, Samaya Nissanke, S. Walsh, A. Hreibi, M. J. Szczepańczyk, M. Chaturvedi, G. Venugopalan, S. R. Mohite, Alessandra Buonanno, Gabrielle Allen, H. Y. Cheung, Rana X. Adhikari, Om Sharan Salafia, F. Donovan, Edoardo Milotti, B. Lantz, M. A. Bizouard, B. K. Berger, Denis Martynov, Claudia Moreno, N. V. Krishnendu, Marco Bazzan, Satoshi Tsuchida, C. Ingram, D. A. Melchor, F. Marion, E. Goetz, Matthew Giesler, D.B. DeBra, Giuseppe Castaldi, S. G. Crowder, K. Ito, E. Lalande, M. Cannavacciuolo, E. N. Clark, Geoffrey Lovelace, L. Nguyen Quynh, J. D. E. Creighton, Lijing Shao, M. Carpinelli, J. Liu, A. Pasqualetti, R. Bajpai, F. Garufi, Archana Pai, Surendra Nadh Somala, Yoshiyuki Obuchi, C. Talbot, Carl-Johan Haster, S. Nozaki, H. Sun, V. JaberianHamedan, Tyson Littenberg, T. Washimi, T. D. Creighton, L. A. Rees, Silvia Corezzi, S. Bae, Kai-Feng Chen, F. Paoletti, Felice Sorrentino, C. L. Chan, P. Szewczyk, A. K. Prajapati, M. Patel, C. M. Mow-Lowry, Sergey P. Vyatchanin, L. Aiello, Luigi Troiano, M. Gosselin, R. Green, H. Yuzurihara, D. Hoyland, B. F. Whiting, J. Casanueva Diaz, V. M. Bedakihale, Masako Kakizaki, R. Maggiore, C. Van Den Broeck, E. Sowell, E. Coccia, M. E. Zucker, B. A. Weaver, G. Vajente, S. M. Gaebel, T. Shimoda, Y. Okutani, J. G. Rollins, A. Mhaske, H. Hansen, T. Wlodarczyk, Laura Cadonati, L. Rolland, S. T. Countryman, S. Penn, R. M. S. Schofield, K. Mogushi, H. Estelles, Y. Huang, P. A. Duverne, S. Karki, D. Moraru, A. Dmitriev, E. Floden, V. B. Adya, A. Renzini, G. L. Mansell, Y. K. Lecoeuche, G. M. Harry, L. Naticchioni, T. Shishido, Salvatore Vitale, A. Cumming, F. Di Renzo, Gianpietro Cagnoli, L.-W. Wei, S. Katsanevas, Madeline Wade, M. Tse, D. S. Tsai, D. M. Macleod, T. D. Ramirez, M. T. 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Hattori, C. Palomba, L. E. Sanchez, K. J. Wagner, D. Hartwig, K. Okutomi, Anupam Sharma, Tim Dietrich, Lionel London, M. S. Shahriar, Sachiko Kuroyanagi, Imre Bartos, B. Idzkowski, V. Loriette, V. Skliris, Enrico Calloni, G. Traylor, S. Soni, Alexander C. Jenkins, Olivier Minazzoli, Thomas Corbitt, A. Markowitz, Takamasa Suzuki, Koya Arai, M. Razzano, Hiroki Takeda, B. Grace, Leopoldo Milano, G. Dálya, Guoying Zhao, C. Gier, Slawomir Gras, L. Salconi, C. A. Costa, S. W. S. Ng, S. M. Aronson, T. Tsang, Akiteru Takamori, N. Koper, Roman Schnabel, H. L. Griggs, R. K. Choudhary, M. Cifaldi, Prafulla K. Panda, V. Quetschke, Rainer Weiss, F. Ricci, X. Liu, Vijay Varma, D. Estevez, J. T. Whelan, M. MacInnis, Rémi Soulard, S. D'Antonio, H. B. Jin, S. Appert, Y. Setyawati, P. Rapagnani, J. E. Brau, J. Feicht, T. Mistry, V. Boudart, Souichi Telada, Aykutlu Dana, Martin M. Fejer, Hideyuki Tagoshi, J. R. Smith, R. Bork, S. Ghonge, P. B. Covas, Paul Hill, S. L. Nadji, Binlei Ding, Efim A. Khazanov, G. Ballardin, M. Caesar, David Blair, K. AultONeal, Robert Bruntz, Andreas Freise, Vincenzo Pierro, M. Pedraza, Z. Yang, R. Quitzow-James, N. N. Janthalur, T. Sawada, Paul D. Lasky, R. K. Hasskew, P. Shawhan, I. Ferrante, J. W. Westhouse, Rico K. L. Lo, D. Ganapathy, D. D. White, Matthew Pitkin, S. M. Scott, L. van der Schaaf, S. A. Pai, Satya Mohapatra, P. McClincy, D. J. McManus, Joey Shapiro Key, S. Meshkov, Seog Oh, S. Bernuzzi, A. M. Holgado, F. Martelli, Karan Jani, R. Shink, Monica Colpi, E. Capocasa, L. Rei, R. Kozu, Andrew Lundgren, W. S. Kim, Shuji Saito, S. D. Linker, P. Charlton, K. Yamashita, Gijs Nelemans, E. D. Hall, N. Bose, M. Granata, J. Bryant, Mark A. Scheel, K. Martinovic, O. Edy, C. Ooi, J. R. Sanders, Daniel E. Holz, B. J. J. Slagmolen, Dalziel J. Wilson, F. Clara, A. Lockwood, K. Holt, R. Shimizu, T. L. Carver, F. Cavalier, K. Hasegawa, S. C. Tait, A. Paolone, K. Shukla, Tatiana da Silva Pereira, F. Salemi, Koh Ueno, Peter Graham Jones, A. W. Jones, R. De Pietri, J. S. Areeda, T. Prestegard, V. Spagnuolo, S. Imam, Rocco Romano, M. Kinley-Hanlon, John D. Scott, R. A. Mercer, S. Ossokine, Jinsook Kim, Y. Mori, C. K. Cheong, Toshihiro Tsuzuki, Jonathan E. Thompson, Kohei Inayoshi, F. Aubin, G. Stratta, T. Yokozawa, Jesper Munch, Achamveedu Gopakumar, Guo-Chin Liu, B. B. Lane, Zifan Zhou, I. A. Bilenko, J. L. Mango, L. Mereni, M. De Laurentis, V. Benedetto, B. Patricelli, D. S. Wu, Margaret Millhouse, M. Kasprzack, David J. Ottaway, A. Paoli, S. G. Gaonkar, Haixing Miao, H. Ohta, S. L. Danilishin, C. Périgois, Santosh Roy, F. Di Giovanni, G. Bogaert, K. L. Dooley, Aaron Zimmerman, A. Romero, Taiki Tanaka, A. R. Guimaraes, Fangchen Feng, Hong Guo, Lisa Barsotti, T. Sato, Anirban Dasgupta, R. Sugimoto, M. Vardaro, Y. Bai, A. K. Divakarla, I. C. F. Wong, R. J. G. Jonker, C. Chan, Nobuyuki Kanda, J. Südbeck, Hartmut Grote, G. Losurdo, G. G. Fronzé, H. K. Tanaka, Eiichi Hirose, Kouji Nakamura, R. S. Bankar, M. C. Milovich-Goff, Neil J. Cornish, Sarah Antier, F-L. Lin, Alessandra Corsi, D. Laghi, Nicolas Sanchis-Gual, P. Grassia, B. Shams, Kipp Cannon, D. M. Wilken, Riccardo Buscicchio, E. J. Daw, Maurizio Canepa, F. Magaña-Sandoval, P. Puppo, Javier M. Antelis, S. J. Kapadia, E. A. Huerta, H. L. Sawant, R. Goetz, Stefano Ansoldi, Tarun Souradeep, Wen-Biao Han, Wolfango Plastino, Antonio Marquina, Eric Hennes, C. L. Romel, A. S. Ubhi, T. A. Ferreira, K. D. Giardina, J. K. Wofford, M. A. Page, T. Ushiba, R. Nakashima, A. L. Urban, B. J. Piotrzkowski, B. E. Ewing, Z. Mark, Luca Baiotti, Simon Zeidler, Luigi D'Onofrio, F. Frasconi, D. Singh, T. Yoshioka, R. Flaminio, M. C. Tringali, Yousuke Itoh, Walid Chaibi, Odylio D. Aguiar, I. W. Martin, S. Hochheim, H. S. Chen, Francesco Puosi, J. Chen, N. A. Robertson, Patrick Godwin, M. C. Araya, Srishti Tiwari, C. Lazzaro, Patricia Schmidt, A. Trovato, J. G. Bartlett, P. G. Murray, Jung-Hoon Kim, N. Gohlke, Fabien Kéfélian, J. H. Hough, P. W. F. Forsyth, S. R. Thondapu, J. R. Palamos, David Jonathan Hofman, G. Baltus, Michele Zanolin, I. Magaña Hernandez, B. Nayak, T. J. Massinger, T. Vo, V. Kalogera, G. D. Hammond, Javed Rana, Lee McCuller, Takuya Tsutsui, P. Gewecke, P. Weßels, Jonathan Blackman, L. C.-C. Lin, M. Seglar-Arroyo, T. D. Abbott, M. Marchio, K. Toland, H. Yamamoto, K. Soni, M. Chan, A. M. Baer, A. Schönbeck, Zoheyr Doctor, V. D'Emilio, Giacomo Bruno, Daniel Wysocki, S. Fairhurst, L. Wallace, José A. Font, I. A. O. MacMillan, N. Singh, A. Królak, K. W. Chung, R. Frey, M. Test, Michael L. Norman, H. Y. Huang, E. A. Muñiz, S. Brunett, M. Mateu-Lucena, Jonathan R. Gair, C. Chen, A. Bisht, Kim Janssens, B. D'Angelo, Carlos O. Lousto, Hongyu Shen, D. C. Coyne, K. Izumi, Takayuki Tomaru, L. Giacoppo, C. North, Thomas Dent, P. Corban, T. Hardwick, F. Travasso, P. Ajith, Michał Bejger, M. Croquette, S. X. Rail, A. K. Y. Li, Hirotaka Takahashi, J. Jiang, Nami Uchikata, V. Hui, A. Perreca, G. Gemme, M. Drago, Zhihui Du, G. 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De Matteis, Archisman Ghosh, Institut Lumière Matière [Villeurbanne] (ILM), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut des Fonctions Optiques pour les Technologies de l'informatiON (Institut FOTON), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Kastler Brossel (LKB [Collège de France]), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Paris-Est Marne-la-Vallée (UPEM), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Institut des Hautes Études Scientifiques (IHES), IHES, KAGRA, Virgo, LIGO Scientific, Spectroscopies optiques des matériaux verres, amorphes et à nanoparticules (SOPRANO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut des Hautes Etudes Scientifiques (IHES), Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, A., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Aleman, K. M., Allen, G., Allocca, A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Ando, M., Angelova, S. V., Ansoldi, S., Antelis, J. M., Antier, S., Appert, S., Arai, Koya, Arai, Koji, Arai, Y., Araki, S., Araya, A., Araya, M. C., Areeda, J. S., Arène, M., Aritomi, N., Arnaud, N., Aronson, S. M., Asada, H., Asali, Y., Ashton, G., Aso, Y., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Babak, S., Badaracco, F., Bader, M. K. M., Bae, S., Bae, Y., Baer, A. M., Bagnasco, S., Bai, Y., Baiotti, L., Baird, J., Bajpai, R., Ball, M., Ballardin, G., Ballmer, S. W., Bals, M., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Bankar, R. S., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Baylor, A. C., Bazzan, M., Bécsy, B., Bedakihale, V. M., Bejger, M., Belahcene, I., Benedetto, V., Beniwal, D., Benjamin, M. G., Bennett, T. F., Bentley, J. D., Benyaala, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bhandari, A. V., Bhattacharjee, D., Bhaumik, S., Bidler, J., Bilenko, I. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., Bitossi, M., Bizouard, M. -A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boer, M., Bogaert, G., Boldrini, M., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, N., Bose, S., Bossilkov, V., Boudart, V., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Bryant, J., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buscicchio, R., Buskulic, D., Byer, R. L., Cadonati, L., Caesar, M., Cagnoli, G., Cahillane, C., Cain, H. W., Bustillo, J. Calderón, Callaghan, J. D., Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, J., Cao, Z., Capocasa, E., Capote, E., Carapella, G., Carbognani, F., Carlin, J. B., Carney, M. F., Carpinelli, M., Carullo, G., Carver, T. L., Diaz, J. Casanueva, Casentini, C., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, W., Chakravarti, K., Champion, B., Chan, C. -H., Chan, C., Chan, C. L., Chan, M., Chandra, K., Chanial, P., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chen, A., Chen, C., Chen, H. Y., Chen, J., Chen, K., Chen, X., Chen, Y. -B., Chen, Y. -R., Chen, Z., Cheng, H., Cheong, C. K., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chiang, C-Y., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Cho, G., Cho, H. S., Choate, S., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, H., Chu, Q., Chu, Y-K., Chua, S., Chung, K. W., Ciani, G., Ciecielag, P., Cieślar, M., Cifaldi, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, E. N., Clark, J. A., Clarke, L., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D. E., Cohen, L., Colleoni, M., Collette, C. G., Colpi, M., Compton, C. M., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corezzi, S., Corley, K. R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Cousins, B., Couvares, P., Covas, P. B., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Criswell, A. W., Croquette, M., Crowder, S. G., Cudell, J. R., Cullen, T. J., Cumming, A., Cummings, R., Cuoco, E., Curyło, M., Canton, T. Dal, Dálya, G., Dana, A., Daneshgaranbajastani, L. M., D’Angelo, B., Danilishin, S. L., D’Antonio, S., Danzmann, K., Darsow-Fromm, C., Dasgupta, A., Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davies, G. S., Davis, D., Daw, E. J., Dean, R., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Del Favero, V., De Lillo, F., De Lillo, N., Del Pozzo, W., Demarchi, L. M., De Matteis, F., D’Emilio, V., Demos, N., Dent, T., Depasse, A., De Pietri, R., De Rosa, R., De Rossi, C., Desalvo, R., De Simone, R., Dhurandhar, S., Díaz, M. C., Diaz-Ortiz, M., Didio, N. A., Dietrich, T., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., D’Onofrio, L., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Drago, M., Driggers, J. C., Drori, Y., Du, Z., Ducoin, J. -G., Dupej, P., Durante, O., D’Urso, D., Duverne, P. -A., Dwyer, S. E., Easter, P. J., Ebersold, M., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Eguchi, S., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Enomoto, Y., Errico, L., Essick, R. C., Estellés, H., Estevez, D., Etienne, Z., Etzel, T., Evans, M., Evans, T. M., Ewing, B. E., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farah, A. M., Farinon, S., Farr, B., Farr, W. M., Farrow, N. W., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Feicht, J., Fejer, M. M., Feng, F., Fenyvesi, E., Ferguson, D. L., Fernandez-Galiana, A., Ferrante, I., Ferreira, T. A., Fidecaro, F., Figura, P., Fiori, I., Fishbach, M., Fisher, R. P., Fittipaldi, R., Fiumara, V., Flaminio, R., Floden, E., Flynn, E., Fong, H., Font, J. A., Fornal, B., Forsyth, P. W. F., Franke, A., Frasca, S., Frasconi, F., Frederick, C., Frei, Z., Freise, A., Frey, R., Fritschel, P., Frolov, V. V., Fronzé, G. G., Fujii, Y., Fujikawa, Y., Fukunaga, M., Fukushima, M., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gais, J., Galaudage, S., Gamba, R., Ganapathy, D., Ganguly, A., Gao, D., Gaonkar, S. G., Garaventa, B., García-Núñez, C., García-Quirós, C., Garufi, F., Gateley, B., Gaudio, S., Gayathri, V., Ge, G., Gemme, G., Gennai, A., George, J., Gergely, L., Gewecke, P., Ghonge, S., Ghosh, Abhirup., Ghosh, Archisman, Ghosh, Shaon, Ghosh, Shrobana, Ghosh, Sourath, Giacomazzo, B., Giacoppo, L., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Giesler, M., Giri, P., Gissi, F., Glanzer, J., Gleckl, A. E., Godwin, P., Goetz, E., Goetz, R., Gohlke, N., Goncharov, B., González, G., Gopakumar, A., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Granata, V., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, A. M., Gretarsson, E. M., Griffith, D., Griffiths, W., Griggs, H. L., Grignani, G., Grimaldi, A., Grimes, E., Grimm, S. J., Grote, H., Grunewald, S., Gruning, P., Guerrero, J. G., Guidi, G. M., Guimaraes, A. R., Guixé, G., Gulati, H. K., Guo, H. -K., Guo, Y., Gupta, Anchal, Gupta, Anuradha, Gupta, P., Gustafson, E. K., Gustafson, R., Guzman, F., Ha, S., Haegel, L., Hagiwara, A., Haino, S., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Han, W. -B., Haney, M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hansen, H., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hartwig, D., Hasegawa, K., Haskell, B., Hasskew, R. K., Haster, C. -J., Hattori, K., Haughian, K., Hayakawa, H., Hayama, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heinze, J., Heinzel, J., Heitmann, H., Hellman, F., Hello, P., Helmling-Cornell, A. F., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Hennig, M. H., Vivanco, F. Hernandez, Heurs, M., Hild, S., Hill, P., Himemoto, Y., Hines, A. S., Hiranuma, Y., Hirata, N., Hirose, E., Hochheim, S., Hofman, D., Hohmann, J. N., Holgado, A. M., Holland, N. A., Hollows, I. J., Holmes, Z. J., Holt, K., Holz, D. E., Hong, Z., Hopkins, P., Hough, J., Howell, E. J., Hoy, C. G., Hoyland, D., Hreibi, A., Hsieh, B-H., Hsu, Y., Huang, G-Z., Huang, H-Y., Huang, P., Huang, Y-C., Huang, Y. -J., Huang, Y. -W., Hübner, M. T., Huddart, A. D., Huerta, E. A., Hughey, B., Hui, D. C. Y., Hui, V., Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Ide, S., Idzkowski, B., Iess, A., Ikenoue, B., Imam, S., Inayoshi, K., Inchauspe, H., Ingram, C., Inoue, Y., Intini, G., Ioka, K., Isi, M., Isleif, K., Ito, K., Itoh, Y., Iyer, B. R., Izumi, K., Jaberianhamedan, V., Jacqmin, T., Jadhav, S. J., Jadhav, S. P., James, A. L., Jan, A. Z., Jani, K., Janssens, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jaume, R., Jenkins, A. C., Jeon, C., Jeunon, M., Jia, W., Jiang, J., Jin, H. -B., Johns, G. R., Jones, A. W., Jones, D. I., Jones, J. D., Jones, P., Jones, R., Jonker, R. J. G., Ju, L., Jung, K., Jung, P., Junker, J., Kaihotsu, K., Kajita, T., Kakizaki, M., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kamiizumi, M., Kanda, N., Kandhasamy, S., Kang, G., Kanner, J. B., Kao, Y., Kapadia, S. J., Kapasi, D. P., Karat, S., Karathanasis, C., Karki, S., Kashyap, R., Kasprzack, M., Kastaun, W., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaur, T., Kawabe, K., Kawaguchi, K., Kawai, N., Kawasaki, T., Kéfélian, F., Keitel, D., Key, J. S., Khadka, S., Khalili, F. Y., Khan, I., Khan, S., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, J., Kim, K., Kim, W. S., Kim, Y. -M., Kimball, C., Kimura, N., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kita, N., Kitazawa, H., Kleybolte, L., Klimenko, S., Knee, A. M., Knowles, T. D., Knyazev, E., Koch, P., Koekoek, G., Kojima, Y., Kokeyama, K., Koley, S., Kolitsidou, P., Kolstein, M., Komori, K., Kondrashov, V., Kong, A. K. H., Kontos, A., Koper, N., Korobko, M., Kotake, K., Kovalam, M., Kozak, D. B., Kozakai, C., Kozu, R., Kringel, V., Krishnendu, N. 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C., Mcisaac, C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Mehmet, M., Mehta, A. K., Melatos, A., Melchor, D. A., Mendell, G., Menendez-Vazquez, A., Menoni, C. S., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I., Michel, C., Michimura, Y., Middleton, H., Milano, L., Miller, A. L., Millhouse, M., Mills, J. C., Milotti, E., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mio, N., Mir, Ll. M., Mishkin, A., Mishra, C., Mishra, T., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Miyamoto, A., Miyazaki, Y., Miyo, K., Miyoki, S., Mo, Geoffrey, Mogushi, K., Mohapatra, S. R. P., Mohite, S. R., Molina, I., Molina-Ruiz, M., Mondin, M., Montani, M., Moore, C. 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A., Okutani, Y., Okutomi, K., Olivetto, C., Oohara, K., Ooi, C., Oram, R., O’Reilly, B., Ormiston, R. G., Ormsby, N. D., Ortega, L. F., O’Shaughnessy, R., O’Shea, E., Oshino, S., Ossokine, S., Osthelder, C., Otabe, S., Ottaway, D. J., Overmier, H., Pace, A. E., Pagano, G., Page, M. A., Pagliaroli, G., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pan, K., Panda, P. K., Pang, H., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Paolone, A., Parisi, A., Park, J., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, M., Patricelli, B., Payne, E., Pechsiri, T. C., Pedraza, M., Pegoraro, M., Pele, A., Arellano, F. E. Peña, Penn, S., Perego, A., Pereira, A., Pereira, T., Perez, C. J., Périgois, C., Perreca, A., Perriès, S., Petermann, J., Petterson, D., Pfeiffer, H. P., Pham, K. A., Phukon, K. S., Piccinni, O. 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J., Richardson, J. W., Richardson, L., Ricker, P. M., Riemenschneider, G., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rocha, J. A., Rodriguez, S., Rodriguez-Soto, R. D., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, J., Romano, R., Romel, C. L., Romero, A., Romero-Shaw, I. M., Romie, J. H., Rose, C. A., Rosińska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rowlinson, S. J., Roy, Santosh, Roy, Soumen, Rozza, D., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadiq, J., Sago, N., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sakellariadou, M., Sakuno, Y., Salafia, O. S., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sanchez, E. J., Sanchez, J. H., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Sanuy, A., Saravanan, T. R., Sarin, N., Sassolas, B., Satari, H., Sato, S., Sato, T., Sauter, O., Savage, R. L., Savant, V., Sawada, T., Sawant, D., Sawant, H. 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Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Abbott, R, Abbott, T, Abraham, S, Acernese, F, Ackley, K, Adams, A, Adams, C, Adhikari, R, Adya, V, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Aleman, K, Allen, G, Allocca, A, Altin, P, Amato, A, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Ando, M, Angelova, S, Ansoldi, S, Antelis, J, Antier, S, Appert, S, Arai, K, Arai, Y, Araki, S, Araya, A, Araya, M, Areeda, J, Arene, M, Aritomi, N, Arnaud, N, Aronson, S, Asada, H, Asali, Y, Ashton, G, Aso, Y, Aston, S, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Babak, S, Badaracco, F, Bader, M, Bae, S, Bae, Y, Baer, A, Bagnasco, S, Bai, Y, Baiotti, L, Baird, J, Bajpai, R, Ball, M, Ballardin, G, Ballmer, S, Bals, M, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Bankar, R, Barayoga, J, Barbieri, C, Barish, B, Barker, D, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, M, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Baylor, A, Bazzan, M, Becsy, B, Bedakihale, V, Bejger, M, Belahcene, I, Benedetto, V, Beniwal, D, Benjamin, M, Bennett, T, Bentley, J, Benyaala, M, Bergamin, F, Berger, B, Bernuzzi, S, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bhandari, A, Bhattacharjee, D, Bhaumik, S, Bidler, J, Bilenko, I, Billingsley, G, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Biswas, B, Bitossi, M, Bizouard, M, Blackburn, J, Blackman, J, Blair, C, Blair, D, Blair, R, Bobba, F, Bode, N, Boer, M, Bogaert, G, Boldrini, M, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, N, Bose, S, Bossilkov, V, Boudart, V, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branch, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Bruno, G, Bruntz, R, Bryant, J, Buikema, A, Bulik, T, Bulten, H, Buonanno, A, Buscicchio, R, Buskulic, D, Byer, R, Cadonati, L, Caesar, M, Cagnoli, G, Cahillane, C, Cain, H, Bustillo, J, Callaghan, J, Callister, T, Calloni, E, Camp, J, Canepa, M, Cannavacciuolo, M, Cannon, K, Cao, H, Cao, J, Cao, Z, Capocasa, E, Capote, E, Carapella, G, Carbognani, F, Carlin, J, Carney, M, Carpinelli, M, Carullo, G, Carver, T, Diaz, J, Casentini, C, Castaldi, G, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cerda-Duran, P, Cesarini, E, Chaibi, W, Chakravarti, K, Champion, B, Chan, C, Chan, M, Chandra, K, Chanial, P, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chen, A, Chen, C, Chen, H, Chen, J, Chen, K, Chen, X, Chen, Y, Chen, Z, Cheng, H, Cheong, C, Cheung, H, Chia, H, Chiadini, F, Chiang, C, Chierici, R, Chincarini, A, Chiofalo, M, Chiummo, A, Cho, G, Cho, H, Choate, S, Choudhary, R, Choudhary, S, Christensen, N, Chu, H, Chu, Q, Chu, Y, Chua, S, Chung, K, Ciani, G, Ciecielag, P, Cieslar, M, Cifaldi, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, E, Clark, J, Clarke, L, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Cohadon, P, Cohen, D, Cohen, L, Colleoni, M, Collette, C, Colpi, M, Compton, C, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrion, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coughlin, S, Coulon, J, Countryman, S, Cousins, B, Couvares, P, Covas, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Criswell, A, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cuoco, E, Curylo, M, Canton, T, Dalya, G, Dana, A, Daneshgaranbajastani, L, D'Angelo, B, Danilishin, S, D'Antonio, S, Danzmann, K, Darsow-Fromm, C, Dasgupta, A, Datrier, L, Dattilo, V, Dave, I, Davier, M, Davies, G, Davis, D, Daw, E, Dean, R, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Favero, V, De Lillo, F, De Lillo, N, Del Pozzo, W, Demarchi, L, De Matteis, F, D'Emilio, V, Demos, N, Dent, T, Depasse, A, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, De Simone, R, Dhurandhar, S, Diaz, M, Diaz-Ortiz, M, Didio, N, Dietrich, T, Di Fiore, L, Di Fronzo, C, Di Giorgio, C, Di Giovanni, F, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, D'Onofrio, L, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Drago, M, Driggers, J, Drori, Y, Du, Z, Ducoin, J, Dupej, P, Durante, O, D'Urso, D, Duverne, P, Dwyer, S, Easter, P, Ebersold, M, Eddolls, G, Edelman, B, Edo, T, Edy, O, Effler, A, Eguchi, S, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Ejlli, A, Enomoto, Y, Errico, L, Essick, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Ewing, B, Fafone, V, Fair, H, Fairhurst, S, Fan, X, Farah, A, Farinon, S, Farr, B, Farr, W, Farrow, N, Fauchon-Jones, E, Favata, M, Fays, M, Fazio, M, Feicht, J, Fejer, M, Feng, F, Fenyvesi, E, Ferguson, D, Fernandez-Galiana, A, Ferrante, I, Ferreira, T, Fidecaro, F, Figura, P, Fiori, I, Fishbach, M, Fisher, R, Fittipaldi, R, Fiumara, V, Flaminio, R, Floden, E, Flynn, E, Fong, H, Font, J, Fornal, B, Forsyth, P, Franke, A, Frasca, S, Frasconi, F, Frederick, C, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V, Fronze, G, Fujii, Y, Fujikawa, Y, Fukunaga, M, Fukushima, M, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Gais, J, Galaudage, S, Gamba, R, Ganapathy, D, Ganguly, A, Gao, D, Gaonkar, S, Garaventa, B, Garcia-Nunez, C, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gayathri, V, Ge, G, Gemme, G, Gennai, A, George, J, Gergely, L, Gewecke, P, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giacoppo, L, Giaime, J, Giardina, K, Gibson, D, Gier, C, Giesler, M, Giri, P, Gissi, F, Glanzer, J, Gleckl, A, Godwin, P, Goetz, E, Goetz, R, Gohlke, N, Goncharov, B, Gonzalez, G, Gopakumar, A, Gosselin, M, Gouaty, R, Grace, B, Grado, A, Granata, M, Granata, V, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, A, Gretarsson, E, Griffith, D, Griffiths, W, Griggs, H, Grignani, G, Grimaldi, A, Grimes, E, Grimm, S, Grote, H, Grunewald, S, Gruning, P, Guerrero, J, Guidi, G, Guimaraes, A, Guixe, G, Gulati, H, Guo, H, Guo, Y, Gupta, A, Gupta, P, Gustafson, E, Gustafson, R, Guzman, F, Ha, S, Haegel, L, Hagiwara, A, Haino, S, Halim, O, Hall, E, Hamilton, E, Hammond, G, Han, W, Haney, M, Hanks, J, Hanna, C, Hannam, M, Hannuksela, O, Hansen, H, Hansen, T, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Hartwig, D, Hasegawa, K, Haskell, B, Hasskew, R, Haster, C, Hattori, K, Haughian, K, Hayakawa, H, Hayama, K, Hayes, F, Healy, J, Heidmann, A, Heintze, M, Heinze, J, Heinzel, J, Heitmann, H, Hellman, F, Hello, P, Helmling-Cornell, A, Hemming, G, Hendry, M, Heng, I, Hennes, E, Hennig, J, Hennig, M, Vivanco, F, Heurs, M, Hild, S, Hill, P, Himemoto, Y, Hines, A, Hiranuma, Y, Hirata, N, Hirose, E, Hochheim, S, Hofman, D, Hohmann, J, Holgado, A, Holland, N, Hollows, I, Holmes, Z, Holt, K, Holz, D, Hong, Z, Hopkins, P, Hough, J, Howell, E, Hoy, C, Hoyland, D, Hreibi, A, Hsieh, B, Hsu, Y, Huang, G, Huang, H, Huang, P, Huang, Y, Hubner, M, Huddart, A, Huerta, E, Hughey, B, Hui, D, Hui, V, Husa, S, Huttner, S, Huxford, R, Huynh-Dinh, T, Ide, S, Idzkowski, B, Iess, A, Ikenoue, B, Imam, S, Inayoshi, K, Inchauspe, H, Ingram, C, Inoue, Y, Intini, G, Ioka, K, Isi, M, Isleif, K, Ito, K, Itoh, Y, Iyer, B, Izumi, K, Jaberianhamedan, V, Jacqmin, T, Jadhav, S, James, A, Jan, A, Jani, K, Janssens, K, Janthalur, N, Jaranowski, P, Jariwala, D, Jaume, R, Jenkins, A, Jeon, C, Jeunon, M, Jia, W, Jiang, J, Jin, H, Johns, G, Jones, A, Jones, D, Jones, J, Jones, P, Jones, R, Jonker, R, Ju, L, Jung, K, Jung, P, Junker, J, Kaihotsu, K, Kajita, T, Kakizaki, M, Kalaghatgi, C, Kalogera, V, Kamai, B, Kamiizumi, M, Kanda, N, Kandhasamy, S, Kang, G, Kanner, J, Kao, Y, Kapadia, S, Kapasi, D, Karat, S, Karathanasis, C, Karki, S, Kashyap, R, Kasprzack, M, Kastaun, W, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaur, T, Kawabe, K, Kawaguchi, K, Kawai, N, Kawasaki, T, Kefelian, F, Keitel, D, Key, J, Khadka, S, Khalili, F, Khan, I, Khan, S, Khazanov, E, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, Kimura, N, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kita, N, Kitazawa, H, Kleybolte, L, Klimenko, S, Knee, A, Knowles, T, Knyazev, E, Koch, P, Koekoek, G, Kojima, Y, Kokeyama, K, Koley, S, Kolitsidou, P, Kolstein, M, Komori, K, Kondrashov, V, Kong, A, Kontos, A, Koper, N, Korobko, M, Kotake, K, Kovalam, M, Kozak, D, Kozakai, C, Kozu, R, Kringel, V, Krishnendu, N, Krolak, A, Kuehn, G, Kuei, F, Kumar, A, Kumar, P, Kumar, R, Kume, J, Kuns, K, Kuo, C, Kuo, H, Kuromiya, Y, Kuroyanagi, S, Kusayanagi, K, Kwak, K, Kwang, S, Laghi, D, Lalande, E, Lam, T, Lamberts, A, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, La Rosa, I, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, H, Lee, J, Lee, K, Lee, R, Lehmann, J, Lemaitre, A, Leon, E, Leonardi, M, Leroy, N, Letendre, N, Levin, Y, Leviton, J, Li, A, Li, B, Li, J, Li, K, Li, T, Li, X, Lin, C, Lin, F, Lin, H, Lin, L, Linde, F, Linker, S, Linley, J, Littenberg, T, Liu, G, Liu, J, Liu, K, Liu, X, Llorens-Monteagudo, M, Lo, R, Lockwood, A, Lollie, M, London, L, Longo, A, Lopez, D, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Luck, H, Lumaca, D, Lundgren, A, Luo, L, Macas, R, Macinnis, M, Macleod, D, Macmillan, I, Macquet, A, Hernandez, I, Magana-Sandoval, F, Magazzu, C, Magee, R, Maggiore, R, Majorana, E, Makarem, C, Maksimovic, I, Maliakal, S, Malik, A, Man, N, Mandic, V, Mangano, V, Mango, J, Mansell, G, Manske, M, Mantovani, M, Mapelli, M, Marchesoni, F, Marchio, M, Marion, F, Mark, Z, Marka, S, Marka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martinez, M, Martinez, V, Martinovic, K, Martynov, D, Marx, E, Masalehdan, H, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Mateu-Lucena, M, Matichard, F, Matiushechkina, M, Mavalvala, N, Mccann, J, Mccarthy, R, Mcclelland, D, Mcclincy, P, Mccormick, S, Mcculler, L, Mcghee, G, Mcguire, S, Mcisaac, C, Mciver, J, Mcmanus, D, Mcrae, T, Mcwilliams, S, Meacher, D, Mehmet, M, Mehta, A, Melatos, A, Melchor, D, Mendell, G, Menendez-Vazquez, A, Menoni, C, Mercer, R, Mereni, L, Merfeld, K, Merilh, E, Merritt, J, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Meyers, P, Meylahn, F, Mhaske, A, Miani, A, Miao, H, Michaloliakos, I, Michel, C, Michimura, Y, Middleton, H, Milano, L, Miller, A, Millhouse, M, Mills, J, Milotti, E, Milovich-Goff, M, Minazzoli, O, Minenkov, Y, Mio, N, Mir, L, Mishkin, A, Mishra, C, Mishra, T, Mistry, T, Mitra, S, Mitrofanov, V, Mitselmakher, G, Mittleman, R, Miyakawa, O, Miyamoto, A, Miyazaki, Y, Miyo, K, Miyoki, S, Mo, G, Mogushi, K, Mohapatra, S, Mohite, S, Molina, I, Molina-Ruiz, M, Mondin, M, Montani, M, Moore, C, Moraru, D, Morawski, F, More, A, Moreno, C, Moreno, G, Mori, Y, Morisaki, S, Moriwaki, Y, Mours, B, Mow-Lowry, C, Mozzon, S, Muciaccia, F, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muniz, E, Murray, P, Musenich, R, Nadji, S, Nagano, K, Nagano, S, Nakamura, K, Nakano, H, Nakano, M, Nakashima, R, Nakayama, Y, Nardecchia, I, Narikawa, T, Naticchioni, L, Nayak, B, Nayak, R, Negishi, R, Neil, B, Neilson, J, Nelemans, G, Nelson, T, Nery, M, Neunzert, A, Ng, K, Ng, S, Nguyen, C, Nguyen, P, Nguyen, T, Quynh, L, Ni, W, Nichols, S, Nishizawa, A, Nissanke, S, Nocera, F, Noh, M, Norman, M, North, C, Nozaki, S, Nuttall, L, Oberling, J, O'Brien, B, Obuchi, Y, O'Dell, J, Ogaki, W, Oganesyan, G, Oh, J, Oh, K, Oh, S, Ohashi, M, Ohishi, N, Ohkawa, M, Ohme, F, Ohta, H, Okada, M, Okutani, Y, Okutomi, K, Olivetto, C, Oohara, K, Ooi, C, Oram, R, O'Reilly, B, Ormiston, R, Ormsby, N, Ortega, L, O'Shaughnessy, R, O'Shea, E, Oshino, S, Ossokine, S, Osthelder, C, Otabe, S, Ottaway, D, Overmier, H, Pace, A, Pagano, G, Page, M, Pagliaroli, G, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Pan, K, Panda, P, Pang, H, Pang, P, Pankow, C, Pannarale, F, Pant, B, Paoletti, F, Paoli, A, Paolone, A, Parisi, A, Park, J, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patel, M, Patricelli, B, Payne, E, Pechsiri, T, Pedraza, M, Pegoraro, M, Pele, A, Arellano, F, Penn, S, Perego, A, Pereira, A, Pereira, T, Perez, C, Perigois, C, Perreca, A, Perries, S, Petermann, J, Petterson, D, Pfeiffer, H, Pham, K, Phukon, K, Piccinni, O, Pichot, M, Piendibene, M, Piergiovanni, F, Pierini, L, Pierro, V, Pillant, G, Pilo, F, Pinard, L, Pinto, I, Piotrzkowski, B, Piotrzkowski, K, Pirello, M, Pitkin, M, Placidi, E, Plastino, W, Pluchar, C, Poggiani, R, Polini, E, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Pracchia, M, Pradier, T, Prajapati, A, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Principe, M, Prodi, G, Prokhorov, L, Prosposito, P, Prudenzi, L, Puecher, A, Punturo, M, Puosi, F, Puppo, P, Purrer, M, Qi, H, Quetschke, V, Quinonez, P, Quitzow-James, R, Raab, F, Raaijmakers, G, Radkins, H, Radulesco, N, Raffai, P, Rail, S, Raja, S, Rajan, C, Ramirez, K, Ramirez, T, Ramos-Buades, A, Rana, J, Rapagnani, P, Rapol, U, Ratto, B, Raymond, V, Raza, N, Razzano, M, Read, J, Rees, L, Regimbau, T, Rei, L, Reid, S, Reitze, D, Relton, P, Renzini, A, Rettegno, P, Ricci, F, Richardson, C, Richardson, J, Richardson, L, Ricker, P, Riemenschneider, G, Riles, K, Rizzo, M, Robertson, N, Robie, R, Robinet, F, Rocchi, A, Rocha, J, Rodriguez, S, Rodriguez-Soto, R, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, J, Romano, R, Romel, C, Romero, A, Romero-Shaw, I, Romie, J, Rose, C, Rosinska, D, Rosofsky, S, Ross, M, Rowan, S, Rowlinson, S, Roy, S, Rozza, D, Ruggi, P, Ryan, K, Sachdev, S, Sadecki, T, Sadiq, J, Sago, N, Saito, S, Saito, Y, Sakai, K, Sakai, Y, Sakellariadou, M, Sakuno, Y, Salafia, O, Salconi, L, Saleem, M, Salemi, F, Samajdar, A, Sanchez, E, Sanchez, J, Sanchez, L, Sanchis-Gual, N, Sanders, J, Sanuy, A, Saravanan, T, Sarin, N, Sassolas, B, Satari, H, Sato, S, Sato, T, Sauter, O, Savage, R, Savant, V, Sawada, T, Sawant, D, Sawant, H, Sayah, S, Schaetzl, D, Scheel, M, Scheuer, J, Schindler-Tyka, A, Schmidt, P, Schnabel, R, Schneewind, M, Schofield, R, Schonbeck, A, Schulte, B, Schutz, B, Schwartz, E, Scott, J, Scott, S, Seglar-Arroyo, M, Seidel, E, Sekiguchi, T, Sekiguchi, Y, Sellers, D, Sergeev, A, Sengupta, A, Sennett, N, Sentenac, D, Seo, E, Sequino, V, Setyawati, Y, Shaffer, T, Shahriar, M, Shams, B, Shao, L, Sharifi, S, Sharma, A, Sharma, P, Shawhan, P, Shcheblanov, N, Shen, H, Shibagaki, S, Shikauchi, M, Shimizu, R, Shimoda, T, Shimode, K, Shink, R, Shinkai, H, Shishido, T, Shoda, A, Shoemaker, D, Shukla, K, Shyamsundar, S, Sieniawska, M, Sigg, D, Singer, L, Singh, D, Singh, N, Singha, A, Sintes, A, Sipala, V, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smetana, J, Smith, J, Smith, R, Somala, S, Somiya, K, Son, E, Soni, K, Soni, S, Sorazu, B, Sordini, V, Sorrentino, F, Sorrentino, N, Sotani, H, Soulard, R, Souradeep, T, Sowell, E, Spagnuolo, V, Spencer, A, Spera, M, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Steer, D, Steinlechner, J, Steinlechner, S, Stops, D, Stover, M, Strain, K, Strang, L, Stratta, G, Strunk, A, Sturani, R, Stuver, A, Sudbeck, J, Sudhagar, S, Sudhir, V, Sugimoto, R, Suh, H, Summerscales, T, Sun, H, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Suzuki, T, Swinkels, B, Szczepanczyk, M, Szewczyk, P, Tacca, M, Tagoshi, H, Tait, S, Takahashi, H, Takahashi, R, Takamori, A, Takano, S, Takeda, H, Takeda, M, Talbot, C, Tanaka, H, Tanaka, K, Tanaka, T, Tanasijczuk, A, Tanioka, S, Tanner, D, Tao, D, Tapia, A, Martin, E, Mertin, E, Tasson, J, Telada, S, Tenorio, R, Terkowski, L, Test, M, Thirugnanasambandam, M, Thomas, M, Thomas, P, Thompson, J, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tolley, A, Tomaru, T, Tomigami, Y, Tomura, T, Tonelli, M, Torres-Forne, A, Torrie, C, E Melo, I, Toyra, D, Trapananti, A, Travasso, F, Traylor, G, Tringali, M, Tripathee, A, Troiano, L, Trovato, A, Trozzo, L, Trudeau, R, Tsai, D, Tsang, K, Tsang, T, Tsao, J, Tse, M, Tso, R, Tsubono, K, Tsuchida, S, Tsukada, L, Tsuna, D, Tsutsui, T, Tsuzuki, T, Turconi, M, Tuyenbayev, D, Ubhi, A, Uchikata, N, Uchiyama, T, Udall, R, Ueda, A, Uehara, T, Ueno, K, Ueshima, G, Ugolini, D, Unnikrishnan, C, Uraguchi, F, Urban, A, Ushiba, T, Usman, S, Utina, A, Vahlbruch, H, Vajente, G, Vajpeyi, A, Valdes, G, Valentini, M, Valsan, V, Van Bakel, N, Van Beuzekom, M, Van Den Brand, J, Van Den Broeck, C, Vander-Hyde, D, Van Der Schaaf, L, Van Heijningen, J, Vanosky, J, Van Putten, M, Van Remortel, N, Vardaro, M, Vargas, A, Varma, V, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venneberg, J, Venugopalan, G, Verkindt, D, Verma, Y, Veske, D, Vetrano, F, Vicere, A, Viets, A, Villa-Ortega, V, Vinet, J, Vitale, S, Vo, T, Vocca, H, Von Reis, E, Von Wrangel, J, Vorvick, C, Vyatchanin, S, Wade, L, Wade, M, Wagner, K, Walet, R, Walker, M, Wallace, G, Wallace, L, Walsh, S, Wang, J, Wang, W, Ward, R, Warner, J, Was, M, Washimi, T, Washington, N, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Weller, C, Wellmann, F, Wen, L, Wessels, P, Westhouse, J, Wette, K, Whelan, J, White, D, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williams, M, Williamson, A, Willis, J, Willke, B, Wilson, D, Winkler, W, Wipf, C, Wlodarczyk, T, Woan, G, Woehler, J, Wofford, J, Wong, I, Wu, C, Wu, D, Wu, H, Wu, S, Wysocki, D, Xiao, L, Xu, W, Yamada, T, Yamamoto, H, Yamamoto, K, Yamamoto, T, Yamashita, K, Yamazaki, R, Yang, F, Yang, L, Yang, Y, Yang, Z, Yap, M, Yeeles, D, Yelikar, A, Ying, M, Yokogawa, K, Yokoyama, J, Yokozawa, T, Yoon, A, Yoshioka, T, Yu, H, Yuzurihara, H, Zadrozny, A, Zanolin, M, Zeidler, S, Zelenova, T, Zendri, J, Zevin, M, Zhan, M, Zhang, H, Zhang, J, Zhang, L, Zhang, R, Zhang, T, Zhao, C, Zhao, G, Zhao, Y, Zhou, Z, Zhu, X, Zhu, Z, Zimmerman, A, Zucker, M, Zweizig, J, RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, RS: FSE MSP, UCL - SST/IRMP - Institut de recherche en mathématique et physique, Arai, K., Arene, M., Becsy, B., Bustillo, J. C., Diaz, J. C., Cavaglia, M., Cerda-Duran, P., Chiang, C. -Y., Chu, Y. -K., Cieslar, M., Cordero-Carrion, I., Curylo, M., Canton, T. D., Dalya, G., D'Angelo, B., D'Antonio, S., Deleglise, S., D'Emilio, V., Diaz, M. C., D'Onofrio, L., D'Urso, D., Estelles, H., Fronze, G. G., Garcia-Nunez, C., Garcia-Quiros, C., Ghosh, A., Ghosh, S., Gonzalez, G., Guixe, G., Gupta, A., Vivanco, F. H., Hsieh, B. -H., Huang, G. -Z., Huang, H. -Y., Huang, Y. -C., Hubner, M. T., Kefelian, F., Krolak, A., Kumar, R., Kuo, H. -S., Lemaitre, A., Lin, C. -Y., Lin, F. -K., Lin, F. -L., Luck, H., Hernandez, I. M., Magana-Sandoval, F., Magazzu, C., Marka, S., Marka, Z., Mir, L. M., Mo, G., Mukherjee, A., Mukherjee, S., Muniz, E. A., Quynh, L. N., O'Brien, B. D., O'Dell, J., O'Reilly, B., O'Shaughnessy, R., O'Shea, E., Arellano, F. E. P., Perigois, C., Perries, S., Purrer, M., Rosinska, D., Roy, S., Schonbeck, A., Sudbeck, J., Suzuki, T., Szczepanczyk, M. J., Tanaka, K., Tanaka, T., Martin, E. N. T. S., Mertin, E. N. T. S., Tiwari, S., Torres-Forne, A., E Melo, I. T., Toyra, D., Tsao, J. -S., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Der Schaaf, L., Van Heijningen, J. V., Van Putten, M. H. P. M., Van Remortel, N., Vasuth, M., Vicere, A., Von Reis, E. R. G., Von Wrangel, J., Wessels, P., Xu, W. -R., Yamamoto, K., Yang, Y., Yu, H., Zadrozny, A., Zhao, Y., LIGO Sci Collaboration, Virgo Collaboration, KAGRA Collaboration, Van Swinderen Institute for Particle Physics and G, and (Astro)-Particles Physics
Subjects: gravitational radiation: anisotropy, Physics and Astronomy (miscellaneous), gravitational radiation: stochastic, Astronomy, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Physics, Particles & Fields, Cosmology & Astrophysics, energy: flux, energy: density, gravitational radiation: energy, LIGO, QC, QB, Physics, Settore FIS/01, Spectral index, Galactic Center, Amplitude, General relativity, Sidereal time, Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gravitational radiation: power spectrum, Gravitation, data analysis method, Anisotropic stochastic gravitational-wave background, Experimental studies of gravity, FOS: Physical sciences, O3, O2, General Relativity and Quantum Cosmology (gr-qc), Astronomy & Astrophysics, Stochastic Background, Gravitational Waves, LIGO, Virgo, O1, O2, O3, O1, Gravitational waves, UPPER LIMITS, statistical analysis, 0103 physical sciences, advanced LIGO and Virgo, ddc:530, KAGRA, 010306 general physics, STFC, gravitational waves, Virgo, Gravitational Waves, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, RCUK, Galaxy, VIRGO, gravitational radiation: emission, spectrum: density, RADIATION, CROSS-CORRELATION SEARCH, Stochastic Background, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, galaxy
Abstract: We report results from searches for anisotropic stochastic gravitational-wave backgrounds using data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. For the first time, we include Virgo data in our analysis and run our search with a new efficient pipeline called {\tt PyStoch} on data folded over one sidereal day. We use gravitational-wave radiometry (broadband and narrow band) to produce sky maps of stochastic gravitational-wave backgrounds and to search for gravitational waves from point sources. A spherical harmonic decomposition method is employed to look for gravitational-wave emission from spatially-extended sources. Neither technique found evidence of gravitational-wave signals. Hence we derive 95\% confidence-level upper limit sky maps on the gravitational-wave energy flux from broadband point sources, ranging from $F_{\alpha, \Theta} < {\rm (0.013 - 7.6)} \times 10^{-8} {\rm erg \, cm^{-2} \, s^{-1} \, Hz^{-1}},$ and on the (normalized) gravitational-wave energy density spectrum from extended sources, ranging from $\Omega_{\alpha, \Theta} < {\rm (0.57 - 9.3)} \times 10^{-9} \, {\rm sr^{-1}}$, depending on direction ($\Theta$) and spectral index ($\alpha$). These limits improve upon previous limits by factors of $2.9 - 3.5$. We also set 95\% confidence level upper limits on the frequency-dependent strain amplitudes of quasimonochromatic gravitational waves coming from three interesting targets, Scorpius X-1, SN 1987A and the Galactic Center, with best upper limits range from $h_0 < {\rm (1.7-2.1)} \times 10^{-25},$ a factor of $\geq 2.0$ improvement compared to previous stochastic radiometer searches., Comment: 23 Pages, 9 Figures
Published: 2021
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17. Vibration isolation systems for the beam splitter and signal recycling mirrors of the KAGRA gravitational wave detector

Author: Hirotaka Takahashi, T. Sekiguchi, Nami Uchikata, Zong-Hong Zhu, Mitsuhiro Fukushima, H. Y. Huang, Ping Huang, Kimio Tsubono, M. Kamiizumi, R. Kozu, Shuji Saito, K. L. Li, Y. Moriwaki, Y. Mori, Atsushi Nishizawa, Souichi Telada, A. Miyamoto, T. Sawada, Kazuhiro Hayama, D. C. Y. Hui, W. S. Kim, Hiroyuki Nakano, S. Imam, Shigeo Nagano, H. L. Lin, S. Otabe, Takuya Tsutsui, Kei Kotake, Masashi Ohkawa, Jinsook Kim, K. Ito, Soichiro Morisaki, Takashi Sato, Yasufumi Kojima, C. Jeon, M. Marchio, Toshihiro Tsuzuki, T. Yamamoto, Yoichi Aso, Kohei Inayoshi, Nobuyuki Kanda, Hideaki Hayakawa, M. Takeda, Y. Tomigami, Hajime Sotani, Nobutada Kimura, Chunglee Kim, Yuka Fujii, Toshio Suzuki, M. Zhan, F. E. Peña Arellano, Fumihiro Uraguchi, T. Yokozawa, H. K. Tanaka, Hyun Lee, Eiichi Hirose, Kouji Nakamura, K. Yamashita, H. Vocca, Takahiro Tanaka, Satoshi Tsuchida, C. C. Kuo, D. Tuyenbayev, T. Yamada, Sadakazu Haino, H. Pang, C. Wu, K. Ueno, B. Ikenoue, F-L. Lin, Lijing Shao, T. Shimoda, Y. Okutani, K. Kaihotsu, Zhoujian Cao, Yoshiaki Himemoto, I. M. Pinto, S. Tanioka, K. Jung, Y. Sakuno, M. A. Barton, K. Izumi, Albert K. H. Kong, H-S. Kuo, M. Nakano, Wen-Biao Han, G. Ueshima, Y. Huang, Kyujin Kwak, K. Yamamoto, B. H. Hsieh, M. Leonardi, Y. Bae, Yuki Inoue, T. Ushiba, Yuichiro Sekiguchi, K. Shimode, J-S. Tsao, Shuen De Wu, S. Shibagaki, W. Ogaki, Simon Zeidler, Luca Baiotti, Yousuke Itoh, Z. Hong, Yuhang Zhao, E. Capocasa, Kyohei Kawaguchi, Hong Wu, Y. Kuromiya, L. Nguyen Quynh, Hiroyuki Takeda, Haruki Kitazawa, Y. Hiranuma, T. Narikawa, R. Bajpai, J. Park, Ryo Yamazaki, Y. M. Kim, H. Chu, A. Hagiwara, Hisa-aki Shinkai, C-Y. Lin, S. Sato, N. Hirata, Jun'ichi Yokoyama, Keiko Kokeyama, L. Naticchioni, T. Shishido, C-Y. Chiang, Yi Chen, R. Sugimoto, Y. Nakayama, Takashi Uchiyama, Kunihito Ioka, Yutaro Enomoto, K. Hattori, R. Nakashima, L. Trozzo, K. Oh, Yoshiyuki Obuchi, E. N. Tapia San Martin, Y. Sakai, K. Sakai, D. Gao, T. Yoshioka, N. Kawai, Norichika Sago, Akiteru Takamori, Kazuyuki Tanaka, S. Eguchi, F. K. Lin, R. Flaminio, H. B. Jin, T. Kawasaki, Akito Araya, Shinji Miyoki, G. Kang, H. Ohta, S. Takano, Kentaro Somiya, R. Hatoya, T. Kajita, A. Parisi, T. Washimi, S. Bae, A. Shoda, S. Oshino, S. Ide, H. Zhang, Masaki Ando, K. Hasegawa, E. J. Son, J. Kume, M. H. P. M. van Putten, Jishnu Suresh, Yi Yang, Yoshio Arai, C. Chen, A. Ueda, T. Tomura, K. Miyo, K. Oohara, Sakae Araki, Osamu Miyakawa, K. Okutomi, Sachiko Kuroyanagi, Tomotada Akutsu, Hideki Asada, R. Shimizu, L. C.-C. Lin, Naoki Aritomi, N. Kita, T. Tsang, Ryutaro Takahashi, Kuo-Chuan Pan, M. Chan, R. Negishi, Seog Oh, Takayuki Tomaru, Jung-Hoon Kim, Ettore Majorana, P. Jung, M. Fukunaga, G-Z. Huang, Yoshihiko Saito, Kunihiro Nagano, John J. Oh, G. Ge, C. Kozakai, Y. Fujikawa, Wei-Tou Ni, Kentaro Komori, Hideyuki Tagoshi, S. Nozaki, Norikatsu Mio, Kai-Feng Chen, S. Ha, T. Uehara, H. Yuzurihara, Masako Kakizaki, Kipp Cannon, L. W. Luo, Yuta Michimura, Rajesh Kumar, K. Kusayanagi, Ray-Kuang Lee, Hyang Woon Lee, Y. Miyazaki, Guo-Chin Liu, J. Z. Wang, Y-K. Chu, K. Yokogawa, Koji Arai, Masatake Ohashi, Naoko Ohishi, W-R. Xu, C. P. Ooi, F. Travasso, Laboratoire d'Annecy de Physique des Particules (LAPP), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)
Subjects: Gravitational-wave observatory, Physics and Astronomy (miscellaneous), 7. Clean energy, 01 natural sciences, Signal, law.invention, gravitational wave detectors, Optics, law, gravitational waves, vibration isolation, underground experiments, gravitational wave detectors, 0103 physical sciences, KAGRA, Interferometric gravitational wave detector, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, mirror, Physics, 010308 nuclear & particles physics, Payload, business.industry, Detector, oscillation, optics, vibration isolation, Vibration isolation, underground experiments, gravitational waves, mechanical engineering, gravitational radiation detector: interferometer, business, Beam splitter, mechanics, performance
Abstract: KAGRA is an underground interferometric gravitational wave detector which is currently being commissioned. This detector relies on high-performance vibration-isolation systems to suspend its key optical components. These suspensions come in four different configurations, of which the type-B is used for the beam splitter and signal recycling mirrors. The type-B suspension comprises the payload, three geometric anti-spring filters for vertical isolation and one inverted pendulum for horizontal isolation. The payload comprises the optic, its marionette and their recoil masses, which hold local displacement sensors and coil magnet actuators used for damping the resonant modes of oscillation of the suspension itself. The beam splitter version has a modified lower section to accommodate a wider optical component. The payload is also equipped with an optical lever, used to monitor and control the position of the suspended optics from the ground. All four suspensions have now been installed in vacuum chambers. We describe the mechanical, electrical and control design, and the measured performance compared to requirements.
Published: 2021
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18. Wideband Monitoring Observations of PSR J1803-3002A in the Globular Cluster NGC 6522

Author: L. Toomey, Andrew Cameron, Jingbo Wang, Qi-Jun Zhi, Lei Zhang, Songbo Zhang, Di Li, George Hobbs, Zong-Hong Zhu, Shi Dai, Shuangqiang Wang, Richard N. Manchester, and Yi Feng
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, 01 natural sciences, Radio telescope, symbols.namesake, Pulsar, Space and Planetary Science, Millisecond pulsar, Globular cluster, 0103 physical sciences, Faraday effect, symbols, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Circular polarization, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We report the first wideband monitoring observations of PSR J1803−3002A, a relatively bright millisecond pulsar (MSP) in the globular cluster NGC 6522 with a spin period of 7.1 ms and no known binary companion. These observations were performed using the Parkes 64 m radio telescope with the Ultra-Wideband Low receiver system, which covers 704–4032 MHz. We confirm that PSR J1803−3002A is an isolated MSP located near the cluster center and probe the emission properties of the pulsar over the wide observed band. The mean pulse profile consists of three components, with the outer components becoming more prominent at higher frequencies, and a mean spectral index for the pulsed emission of −1.66 ± 0.07 over the observed band. The fractional linear and circular polarization increase with increasing frequency, which is unusual for pulsars. We determine a Faraday rotation measure of −107 ± 6 rad m−2 for the pulsar. PSR J1803−3002A is a distant pulsar in the Galactic plane, but our observations show no evidence of pulse broadening due to interstellar scattering. These results demonstrate the power of ultra-wideband receivers and signal processing systems.
Published: 2020

19. Overview of KAGRA: KAGRA science

Author: D. C. Y. Hui, G. Ueshima, Tatsuhiro Yamada, T. Narikawa, Ryo Yamazaki, Keiko Kokeyama, Soichiro Morisaki, C. Jeon, Kipp Cannon, Akito Araya, L. W. Luo, C. C. Kuo, Kentaro Somiya, R. Shimizu, L. C.-C. Lin, T. Kajita, A. Parisi, Hideyuki Tagoshi, D. Tuyenbayev, Shigeo Nagano, Masaki Ando, Y. M. Kim, C-Y. Chiang, M. Chan, T. Yamamoto, Kei Kotake, Norikatsu Mio, K. Hasegawa, M. H. P. M. van Putten, Jishnu Suresh, L. Nguyen Quynh, S. Ha, R. Bajpai, S. Nozaki, Nobuyuki Kanda, K. Miyo, K. Oohara, S. Ide, Kyujin Kwak, Kai-Feng Chen, M. Zhan, L. Naticchioni, T. Shishido, Hideaki Hayakawa, H. Pang, Yoshio Arai, H. K. Tanaka, R. Nakashima, Y. Huang, M. A. Barton, Eiichi Hirose, F. Fujikawa, Kouji Nakamura, T. Uehara, M. Nakano, H. Yuzurihara, H. Chu, Takayuki Tomaru, W-R. Xu, C. P. Ooi, F-L. Lin, Shuen De Wu, Masako Kakizaki, H. Vocca, Hisa-aki Shinkai, Kazuhiro Hayama, M. Leonardi, Takashi Sato, Yoshiyuki Obuchi, R. Sugimoto, Atsushi Nishizawa, S. Oshino, Yoshiaki Himemoto, I. M. Pinto, Haruki Kitazawa, Yuka Fujii, Y. Hiranuma, G. Ge, Yuichiro Sekiguchi, Kimio Tsubono, S. Otabe, Kazuyuki Tanaka, Kwan-Lok Li, Y. Sakai, Hiroki Takeda, S. Takano, K. Sakai, F. K. Lin, K. Kaihotsu, Souichi Telada, T. Sawada, E. J. Son, Kazumi Kashiyama, W. S. Kim, Takashi Uchiyama, Kunihito Ioka, Tenglin Li, J. Kume, K. Yamashita, Satoshi Tsuchida, Shinji Miyoki, Masatake Ohashi, T. Yoshioka, W. Ogaki, T. Tomura, Lijing Shao, K. Shimode, N. Kita, R. Flaminio, Z. Hong, T. Shimoda, Y. Okutani, Kentaro Komori, Naoko Ohishi, T. Tsang, Hideki Asada, Y. Tomigami, Jung-Hoon Kim, Kuo-Chuan Pan, J. Z. Wang, Y-K. Chu, K. Yokogawa, R. Negishi, Tomotada Akutsu, Hong Wu, Nobutada Kimura, Naoki Aritomi, Koji Arai, Seog Oh, Takahiro Tanaka, A. Hagiwara, C-Y. Lin, Ryutaro Takahashi, B. H. Hsieh, K. Hattori, Masashi Ohkawa, Y. Aso, Yuki Inoue, H. Ohta, Akiteru Takamori, Wen-Biao Han, H. B. Jin, S. Shibagaki, C. Z. Huang, Y. Nakayama, T. Ushiba, S. Eguchi, Luca Baiotti, Simon Zeidler, Yuhang Zhao, S. Sato, N. Hirata, A. Shoda, Yousuke Itoh, Yutaro Enomoto, T. Sekiguchi, Yi Chen, Zong-Hong Zhu, Y. Sakuno, Y. Mori, M. Kamiizumi, A. Miyamoto, Hiroyuki Nakano, J. Park, K. Ito, Y. Moriwaki, Yuta Michimura, K. Yamamoto, Y. Bae, Kyohei Kawaguchi, Rajesh Kumar, K. Kusayanagi, D. Gao, T. Kawasaki, Yi Yang, Ray-Kuang Lee, S. Tanioka, K. Jung, R. Kozu, E. Capocasa, Shuji Saito, Hyang Woon Lee, S. Imam, Jinsook Kim, Toshihiro Tsuzuki, E. N. Tapia San Martin, Kohei Inayoshi, M. Takeda, N. Kawai, T. Yokozawa, K. Okutomi, Sachiko Kuroyanagi, H. L. Lin, Y. Miyazaki, Guo-Chin Liu, Takuya Tsutsui, M. Marchio, Ettore Majorana, P. Jung, M. Fukunaga, Yoshihiko Saito, Kunihiro Nagano, John J. Oh, C. Kozakai, C. Chen, Yasufumi Kojima, Hajime Sotani, Chunglee Kim, Fumihiro Uraguchi, K. Izumi, Wei-Tou Ni, Sadakazu Haino, C. Wu, J-S. Tsao, K. Ueno, Zhoujian Cao, L. Trozzo, Norichika Sago, T. Washimi, S. Bae, F. E. Pe Na Arellano, Jun'ichi Yokoyama, K. Oh, Toshio Suzuki, Hyun Lee, F. Travasso, Hirotaka Takahashi, Nami Uchikata, Mitsuhiro Fukushima, H. Y. Huang, Ping Huang, B. Ikenoue, H-S. Kuo, G. Kang, H. Zhang, A. Ueda, Sakae Araki, Osamu Miyakawa, Albert K. H. Kong, Y. Kuromiya, Daichi Tsuna, LAPP - Laboratoire d'Annecy de Physique des Particules, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and KAGRA
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Observatory, 0103 physical sciences, laser: interferometer, KAGRA, 010303 astronomy & astrophysics, kagra gravitational wave kamioka, High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, gravitational radiation, Astronomy, detector: upgrade, gravitational radiation detector, detector: sensitivity, Interferometry, Upgrade, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], E02, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: KAGRA is a newly build gravitational-wave observatory, a laser interferometer with 3 km arm length, located in Kamioka, Gifu, Japan. In this paper in the series of KAGRA-featured articles, we discuss the science targets of KAGRA projects, considering not only the baseline KAGRA (current design) but also its future upgrade candidates (KAGRA+) for the near to middle term (~5 years)., 73 pages, 11 figures, accepted by Progress of Theoretical and Experimental Physics, in the series of KAGRA-featured articles
Published: 2020
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20. Overview of KAGRA: Detector design and construction history

Author: Yuta Michimura, Kyujin Kwak, Yoshiaki Himemoto, I. M. Pinto, Rajesh Kumar, K. Kusayanagi, G. Ge, R. Kozu, Soichiro Morisaki, Yuichiro Sekiguchi, Kai-Feng Chen, M. A. Barton, H. Chu, Shuji Saito, N. Kita, T. Tsang, S. Oshino, C. Z. Huang, T. Ushiba, Luca Baiotti, Simon Zeidler, Yousuke Itoh, F. Travasso, C. C. Kuo, D. Tuyenbayev, Hirotaka Takahashi, Nami Uchikata, Takashi Uchiyama, Kunihito Ioka, Kuo-Chuan Pan, M. Kamiizumi, A. Miyamoto, B. H. Hsieh, Toshio Suzuki, Hyun Lee, H. Yuzurihara, Ray-Kuang Lee, Hisa-aki Shinkai, Se-Hong Oh, J. Z. Wang, Y-K. Chu, K. Yokogawa, R. Negishi, Nobuyuki Kanda, T. Kawasaki, F. L. Lin, Shuen De Wu, Albert K. H. Kong, Yuhang Zhao, Yuki Inoue, S. Shibagaki, B. Ikenoue, Y. Tomigami, Hong Wu, Yutaro Enomoto, H. K. Tanaka, H-S. Kuo, Atsushi Nishizawa, Takahiro Tanaka, Eiichi Hirose, Kouji Nakamura, Hyang Woon Lee, Mitsuhiro Fukushima, Ping Huang, T. Sekiguchi, L. Trozzo, Norichika Sago, S. Sato, Kentaro Somiya, A. Hagiwara, Shinji Miyoki, Y. Sakuno, C-Y. Lin, Y. Miyazaki, K. Hasegawa, Yoshiyuki Obuchi, N. Hirata, Yi Chen, Koji Arai, Masaki Ando, S. Tanioka, K. Jung, M. Leonardi, R. Bajpai, Y. Hiranuma, Hideyuki Tagoshi, R. Sugimoto, Kipp Cannon, G. Ueshima, Kazuyuki Tanaka, Y. Saito, S. Takano, S. Bae, R. Shimizu, M. Marchio, T. Shishido, Zong-Hong Zhu, L. C.-C. Lin, M. Chan, Yoichi Aso, L. W. Luo, Haruki Kitazawa, J. Park, Jun'ichi Yokoyama, Y. Sakai, R. Nakashima, Satoshi Tsuchida, C. Chen, Takashi Sato, P. Jung, S. Eguchi, E. Capocasa, Yasufumi Kojima, Hiroyuki Nakano, T. Yoshioka, R. Flaminio, K. Sakai, T. Shimoda, E. J. Son, J. Kume, M. Fukunaga, K. Izumi, Hajime Sotani, Chunglee Kim, A. Shoda, K. Okutomi, Tomotada Akutsu, Sachiko Kuroyanagi, Akito Araya, T. Kajita, G. Kang, W. Ogaki, Masatake Ohashi, Z. Hong, Fumihiro Uraguchi, Kunihiro Nagano, O. Miyakawa, Kazuhiro Hayama, Tatsuhiro Yamada, Sadakazu Haino, C. Wu, M. H. P. M. van Putten, K. Ueno, S. Imam, Takayuki Tomaru, K. Miyo, K. Oohara, Naoko Ohishi, Y. M. Kim, Jinsook Kim, John J. Oh, Kentaro Komori, A. Ueda, Sakae Araki, Toshihiro Tsuzuki, T. Narikawa, E. N. Tapia San Martin, Kohei Inayoshi, M. Takeda, Keiko Kokeyama, Masashi Ohkawa, T. Yokozawa, N. Kawai, C. Kozakai, W-R. Xu, Yasunori Fujii, Y. Moriwaki, K. Shimode, C. P. Ooi, K. Yamamoto, Y. Huang, Y. Bae, Kyohei Kawaguchi, Shigeo Nagano, Kei Kotake, Wei-Tou Ni, Akiteru Takamori, H. Vocca, Norikatsu Mio, Yoshio Arai, T. Uehara, Naoki Aritomi, Ryutaro Takahashi, Guo-Chin Liu, T. Tomura, F. E. Peña Arellano, H. Pang, M. Nakano, T. Yamamoto, Hideaki Hayakawa, Kimio Tsubono, Hiroki Takeda, Souichi Telada, T. Sawada, W. S. Kim, Nobutada Kimura, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and KAGRA
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Physics - Instrumentation and Detectors, activity report, detector: design, laser: interferometer, noise: thermal, KAGRA, gravitational radiation detector, background, cryogenics, history, mirror, fabrication, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Cryogenics, fabrication, 01 natural sciences, General Relativity and Quantum Cosmology, law.invention, Telescope, Optics, law, 0103 physical sciences, noise: thermal, KAGRA, laser: interferometer, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, mirror, Instrumentation and Methods for Astrophysics (astro-ph.IM), activity report, detector: design, Physics, 010308 nuclear & particles physics, business.industry, background, Detector, Instrumentation and Detectors (physics.ins-det), gravitational radiation detector, Interferometry, cryogenics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], history, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: KAGRA is a newly built gravitational-wave telescope, a laser interferometer comprising arms with a length of 3\,km, located in Kamioka, Gifu, Japan. KAGRA was constructed under the ground and it is operated using cryogenic mirrors that help in reducing the seismic and thermal noise. Both technologies are expected to provide directions for the future of gravitational-wave telescopes. In 2019, KAGRA finished all installations with the designed configuration, which we call the baseline KAGRA. In this occasion, we present an overview of the baseline KAGRA from various viewpoints in a series of of articles. In this article, we introduce the design configurations of KAGRA with its historical background., 33 pages, 10 figures
Published: 2020
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21. Gravitational wave interference via gravitational lensing: Measurements of luminosity distance, lens mass, and cosmological parameters

Author: Kai Liao, Shaoqi Hou, Zong-Hong Zhu, and Xi-Long Fan
Subjects: Physics, 010308 nuclear & particles physics, Gravitational wave, Point particle, FOS: Physical sciences, Beat (acoustics), General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Interferometry, Gravitational lens, 0103 physical sciences, Astronomical interferometer, Waveform, 010306 general physics, Luminosity distance
Abstract: The gravitational lensing of gravitational waves might cause beat patterns detectable by interferometers. The feature of this kind of signal is the existence of the beat pattern in the early inspiral phase, followed by a seemingly randomly changing profile. After the strain peaks for the first time, the signal takes the usual waveform and the strain peaks for the second time. Once this signal is detected, the actual magnification factors can be obtained, so the true luminosity distance of the binary system is known. If the lens can be described by a point mass or a singular isothermal sphere, the functional forms of the time delay and the magnification factors are simple enough, so we can infer the mass of the lens or the cosmological parameters., 9 pages, 4 figures
Published: 2020
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22. Black hole mass function and its evolution -- the first prediction for the Einstein Telescope

Author: Zong-Hong Zhu, Kai Liao, Xuheng Ding, and Marek Biesiada
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Einstein Telescope, Gravitational wave, Monte Carlo method, Binary number, FOS: Physical sciences, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Redshift, Luminosity, Black hole, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The knowledge about the black hole mass function (BHMF) and its evolution would help to understand the origin of the BHs and how BH binaries formed at different stages of the history of the Universe. We demonstrate the ability of future third generation gravitational wave (GW) detector -- the Einstein Telescope (ET) to infer the slope of the BHMF and its evolution with redshift. We perform the Monte Carlo simulation of the measurements of chirp signals from binary BH systems (BBH) that could be detected by ET, including the BH masses and their luminosity distances ($d_L$). We use the mass of a primary black hole in each binary system to infer the BHMF as a power-law function with slope parameter as $\alpha$. Taking into account the bias that could be introduced by the uncertainty of measurements and by the selection effect, we carried out the numerical tests and find that only one thousand of GW events registered by ET ($\sim1\%$ amount of its yearly detection rate) could accurately infer the $\alpha$ with a precision of $\alpha\sim0.1$. Furthermore, we investigate the validity of our method to recover a scenario where $\alpha$ evolves with redshift as $\alpha(z) = \alpha_0 + \alpha_1\frac{z}{1+z}$. Taking a thousand of GW events and using $d_L$ as the redshift estimator, our tests show that one could infer the value of evolving parameter $\alpha_1$ accurately with the uncertainty level of $\sim0.5$. Our numerical tests verify the reliability of our method. The uncertainty levels of the inferred parameters can be trusted directly for the several sets of the parameter we assumed, yet shouldn't be treated as a universal level for the general case., Comment: 9 pages, 4 figures, 1 table; Accepted by ApJ
Published: 2020

23. Swift monitoring observations of Mrk 231: detection of ultraviolet variability

Author: Xinyu Dai, Francesco Shankar, Youjun Lu, Lilan Yang, and Zong Hong Zhu
Subjects: Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, medicine.disease_cause, 01 natural sciences, Spectral line, 0103 physical sciences, medicine, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Scattering, Spectral density, Astronomy and Astrophysics, Quasar, Light curve, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Ultraviolet
Abstract: We analyze 168 Swift monitoring observations of the nearest broad absorption line quasar Mrk 231 in the UV and X-ray bands, where we detect significant variability in the UV ($\sim$2246\AA) light curve with a null probability of $4.3\times10^{-10}$ for a constant model. Separately, from an archival sample of Swift observed active galactic nuclei (AGN), we measure the relation between UV excess variance and luminosity, finding that the normalized UV excess variance decreases with luminosity. Comparing to this mean relation, the normalized UV excess variance of Mrk 231 is smaller, however within the scatter characterising the full population. The upper limit of the X-ray excess variance is consistent with other AGN. The power spectrum density of the UV light curve can be well fit by a power law model with a slope of $1.82\pm0.14$ between $10^{-7.5}$ and $10^{-6}$ Hz, consistent with those for typical AGN, with no obvious quasi-periodical oscillation peaks. The UV variability and its power spectrum suggest that a significant amount of the UV emission of Mrk 231 is from the accretion disk. The consistencies in the normalized UV variability and the shape of the power spectrum density between Mrk 231 and other normal AGN suggest that the origin of UV variability of broad absorption line quasars is similar to other AGN, and dust scattering at large scales such as the torus is not a dominating process for the UV emission of Mrk 231. Significant scattering, if present, is constrained to smaller than $\sim$10 light days. We perform lagged correlation analysis between the UV and X-ray light curves and find the correlation insignificant within the present data., Comment: 8 pages, 4 figures, accepted by MNRAS
Published: 2018
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24. Radiative Cooling of the Thermally Isolated System in KAGRA Gravitational Wave Telescope

Author: A. Hagiwara, C-Y. Lin, Akito Araya, T. Kajita, M. A. Barton, R. Bajpai, Yoshiaki Himemoto, I. M. Pinto, G. Kang, M. H. P. M. van Putten, K. Miyo, K. Oohara, Tatsuhiro Yamada, Satoshi Tsuchida, Yoshiyuki Obuchi, T. Shimoda, P. Jung, M. Fukunaga, G-Z. Huang, Yuichiro Sekiguchi, B. H. Hsieh, Yuki Inoue, S. Shibagaki, Albert K. H. Kong, K. Chen, Yoshihiko Saito, H. C. Wu, Shigeo Nagano, Kei Kotake, Hisa-aki Shinkai, S. Wu, T. Shishido, R. Nakashima, T. Yoshioka, R. Flaminio, Hiroyuki Takeda, T. Narikawa, Keiko Kokeyama, S. Oshino, Takashi Uchiyama, John J. Oh, H. W. Lee, Soichiro Morisaki, G. Ge, S. Sato, Nobuyuki Kanda, N. Hirata, Y. Tomigami, A. Ueda, Yasufumi Kojima, Kunihito Ioka, Hajime Sotani, Chunglee Kim, Nobutada Kimura, H. K. Tanaka, Sakae Araki, Takahiro Tanaka, Yi Chen, Eiichi Hirose, Kouji Nakamura, F. Travasso, Hirotaka Takahashi, Kipp Cannon, T. Kawasaki, Osamu Miyakawa, D. Tuyenbayev, Fumihiro Uraguchi, Shinji Miyoki, Y. Sakuno, L. W. Luo, F-L. Lin, Wei-Tou Ni, H. Vocca, Masatake Ohashi, Toshio Suzuki, Jong-Dae Park, Takashi Sato, H. Pang, Mitsuhiro Fukushima, Koki Okutomi, K. Yamamoto, Ray-Kuang Lee, Sadakazu Haino, M. Nakano, F. E. Peiia Arellano, Kimio Tsubono, Hyun Lee, S. Imam, Naoko Ohishi, Yuka Fujii, Jinsook Kim, Sachiko Kuroyanagi, Y. Bae, G. Ueshima, Toshihiro Tsuzuki, Y. K. Chu, T. Tomura, Kohei Inayoshi, M. Marchio, S. Tanioka, Kyohei Kawaguchi, Souichi Telada, T. Sawada, T. Yokozawa, J. Z. Wang, K. Yokogawa, Yuta Michimura, B. Ikenoue, T. Sekiguchi, H. Yuzurihara, K. Hasegawa, Jun'ichi Yokoyama, E. N. Tapia San Martin, M. Leonardi, K. Jung, C. M. Kuo, W. S. Kim, Tomotada Akutsu, H-S. Kuo, N. Kawai, Zong-Hong Zhu, R. Sugimoto, Rajesh Kumar, Haruki Kitazawa, R. Kozu, Shuji Saito, K. Izumi, T. Yamamoto, K. Kusayanagi, Y. M. Kim, E. Capocasa, Kyujin Kwak, Seog Oh, Hideaki Hayakawa, Koji Arai, H. Chu, Y. Miyazaki, L. Trozzo, Norichika Sago, Atsushi Nishizawa, Koh Ueno, Y. Moriwaki, Guo-Chin Liu, S. Bae, C. M. Wu, Y. Hiranuma, W-R. Xu, C. P. Ooi, Kazuhiro Hayama, Y. Sakai, K. Sakai, R. Shimizu, L. C.-C. Lin, M. Chan, Kentaro Somiya, Edwin J. Son, Yoshio Arai, Masaki Ando, C. Chen, Naoki Aritomi, Ryutaro Takahashi, Akiteru Takamori, Chihiro Kozakai, Takayuki Tomaru, M. Takeda, K. Shimode, Yuhang Zhao, Hiroyuki Nakano, Yutaro Enomoto, W. Ogaki, Z. Hong, Masashi Ohkawa, Y. Aso, P. W. Huang, Y. Huang, Kazuyuki Tanaka, S. Takano, J. Kume, Norikatsu Mio, T. Uehara, Kentaro Komori, Hideyuki Tagoshi, N. Kita, T. Tsang, N. Uchikata, Kuo-Chuan Pan, R. Negishi, S. Eguchi, A. Shoda, T. Ushiba, Simon Zeidler, Luca Baiotti, Yousuke Itoh, Koji Nagano, M. Kamiizumi, A. Miyamoto, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and KAGRA
Subjects: History, Radiative cooling, Thermally isolated system, detector: noise, cavity: optical, 01 natural sciences, Education, law.invention, Telescope, fluctuation: thermal, law, 0103 physical sciences, noise: thermal, KAGRA, laser: interferometer, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, mirror, Physics, radiation: thermal, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, Astronomy, gravitational radiation detector, Computer Science Applications, injection, cryogenics, specific heat
Abstract: Radiative cooling of the thermally isolated system is investigated in KAGRA gravitational wave telescope. KAGRA is a laser interferometer-based detector and main mirrors constituting optical cavities are cool down to 20K to reduce noises caused by the thermal fluctuation. The mirror is suspended with the multi-stage pendulum to isolate any vibration. Therefore, this mirror suspension system has few heat links to reduce vibration injection. Thus, this system is mainly cooled down with thermal radiation. In order to understand the process of radiative cooling of the mirror, we analyzed cooling curve based on mass and specific heat. As a result, it was newly found that a cryogenic part called ”cryogenic duct-shield” seems to have large contribution in the beginning of the mirror cooling. This finding will help to design new cooling system for the next generation cryogenic gravitational wave detector.
Published: 2020
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25. Lensing rates of gravitational wave signals displaying beat patterns detectable by DECIGO and B-DECIGO

Author: Zong-Hong Zhu (朱宗宏), Pengbo Li (李鹏博), Seiji Kawamura, Xi-Long Fan (范锡龙), Shaoqi Hou (侯绍齐), Hai Yu (余海), and Marek Biesiada
Subjects: Physics, education.field_of_study, 010308 nuclear & particles physics, Gravitational wave, Population, Detector, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, symbols.namesake, Neutron star, Gravitational lens, 0103 physical sciences, symbols, 010306 general physics, education, Luminosity distance, Hubble's law
Abstract: The coherent nature of gravitational wave emanating from a compact binary system makes it possible to detect some interference patterns in two (or more) signals registered simultaneously by the detector. Gravitational lensing effect can be used to bend trajectories of gravitational waves, which might reach the detector at the same time. Once this happens, a beat pattern may form, and can be used to obtain the luminosity distance of the source, the lens mass, and cosmological parameters such as the Hubble constant. Crucial question is how many such kind of events could be detected. In this work, we study this issue for the future space-borne detectors: DECIGO and its downscale version, B-DECIGO. It is found out that there can be a few tens to a few hundreds of lensed gravitational wave events with the beat pattern observed by DECIGO and B-DECIGO per year, depending on the evolution scenario leading to the formation of double compact objects. In particular, black hole-black hole binaries are dominating population of lensed sources in which beat patterns may reveal. However, DECIGO could also register a considerable amount of lensed signals from binary neutron stars, which might be accompanied by electromagnetic counterparts. Our results suggest that, in the future, lensed gravitational wave signal with the beat pattern could play an important role in cosmology and astrophysics., Comment: 15 pages, 7 figures. Revised based on Referee's comments
Published: 2020
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26. Gravitational-wave constraints on the cosmic opacity at $z\sim 5$: forecast from space gravitational-wave antenna DECIGO

Author: Zong-Hong Zhu, Marek Biesiada, Shuaibo Geng, Jingzhao Qi, Tonghua Liu, Shuo Cao, and Yuting Liu
Subjects: Physics, COSMIC cancer database, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Opacity, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space (mathematics), Space and Planetary Science, Antenna (radio), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Since gravitational waves (GWs) propagate freely through a perfect fluid, coalescing compact binary systems as standard sirens allow to measure the luminosity distance directly and provide distance measurements unaffected by the cosmic opacity. DECi-hertz Interferometer Gravitational-wave Observatory (DECIGO) is a future Japanese space gravitational-wave antenna sensitive to frequency range between target frequencies of LISA and ground-based detectors. Combining the predicted future GW observations from DECIGO and three current popular astrophysical probes (HII regions, SNe Ia Pantheon sample, quasar sample) in electromagnetic (EM) domains, one would be able to probe the opacity of the Universe at different redshifts. In this paper, we show that the cosmic opacity parameter can be constrained to a high precision ($\Delta \epsilon\sim 10^{-2}$) out to high redshifts ($z\sim$5). In order to reconstruct the evolution of cosmic opacity without assuming any particular functional form of it, the cosmic opacity tests should be applied to individual redshift bins independently. Therefore, we also calculate the optical depth at individual redshifts and averaged $\tau(z)$ within redshift bins. Our findings indicate that, compared with the results obtained from the HII galaxies and Pantheon SNe Ia, there is an improvement in precision when the quasar sample is considered. While non-zero optical depth is statistically significant only for redshift ranges $0, Comment: 11pages, 9figures, accepted for publication in ApJ
Published: 2020
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27. Measuring the viscosity of dark matter with strongly lensed gravitational waves

Author: Marek Biesiada, Jin Li, Zong-Hong Zhu, Tonghua Liu, Jingzhao Qi, and Shuo Cao
Subjects: Coalescence (physics), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Einstein Telescope, Gravitational wave, Dark matter, Binary number, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Physics::Fluid Dynamics, Space and Planetary Science, Observatory, Big Bang Observer, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Based on the strongly lensed gravitational waves (GWs) from compact binary coalescence, we propose a new strategy to examine the fluid shear viscosity of dark matter (DM) in the gravitational wave domain, i.e., whether a GW experiences the damping effect when it propagates in DM fluid with nonzero shear viscosity. By assuming that the dark matter self-scatterings are efficient enough for the hydrodynamic description to be valid, our results demonstrate that future ground-based Einstein Telescope (ET) and satellite GW observatory (Big Bang Observer; BBO) may succeed in detecting any dark matter self-interactions at the scales of galaxies and clusters., Comment: 1 figure, 1 table, accepted for publication in MNRAS Letters
Published: 2020
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28. Cosmology-insensitive estimate of IGM baryon mass fraction from five localized fast radio bursts

Author: Bing Zhang, He Gao, Yuan-Pei Yang, Zong-Hong Zhu, Zhengxiang Li, and Jun-Jie Wei
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Type (model theory), Redshift, Galaxy, General Relativity and Quantum Cosmology, Baryon, Supernova, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Luminosity distance, Mass fraction
Abstract: Five fast radio bursts (FRBs), including three apparently non-repeating ones FRB 180924, FRB 181112, and FRB 190523, and two repeaters, FRB 121102 and FRB 180916.J0158+65, have already been localized so far. We apply a method developed recently by us (Li et al. 2019) to these five localized FRBs to give a cosmology-insensitive estimate of the fraction of baryon mass in the IGM, $f_{\rm IGM}$. Using the measured dispersion measure (DM) and luminosity distance $d_{\rm L}$ data (inferred from the FRB redshifts and $d_{\rm L}$ of type Ia supernovae at the same redshifts) of the five FRBs, we constrain the local $f_{\rm IGM} = 0.84^{+0.16}_{-0.22}$ with no evidence of redshift dependence. This cosmology-insensitive estimate of $f_{\rm IGM}$ from FRB observations is in excellent agreement with previous constraints using other probes. Moreover, using the three apparently non-repeating FRBs only we get a little looser but consistent result $f_{\rm IGM} = 0.74^{+0.24}_{-0.18}$. In these two cases, reasonable estimations for the host galaxy DM contribution (${\rm DM_{host}}$) can be achieved by modelling it as a function of star formation rate. The constraints on both $f_{\rm IGM}$ and ${\rm DM_{host}}$ are expected to be significantly improved with the rapid progress in localizing FRBs., Comment: 6 pages, 3 figures, accepted for publication in MNRAS Letters
Published: 2020
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29. Standard-siren cosmology using gravitational waves from binary black holes

Author: Zhi-Qiang You, Xing-Jiang Zhu, Eric Thrane, Zong-Hong Zhu, and Gregory Ashton
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, symbols.namesake, General Relativity and Quantum Cosmology, Binary black hole, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, Einstein Telescope, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxy, Black hole, Space and Planetary Science, symbols, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: Gravitational-wave astronomy provides a unique new way to study the expansion history of the Universe. In this work, we investigate the impact future gravitational-wave observatories will have on cosmology. Third-generation observatories like the Einstein Telescope and Cosmic Explorer will be sensitive to essentially all of the binary black hole coalescence events in the Universe. Recent work by \cite{farr2019future} points out that features in the stellar-mass black hole population break the mass-redshift degeneracy, facilitating precise determination of the Hubble parameter without electromagnetic counterparts or host galaxy catalogues. Using a hierarchical Bayesian inference model, we show that with one year of observations by the Einstein Telescope, the Hubble constant will be measured to $\lesssim 1\%$. We also show that this method can be used to perform Bayesian model selection between cosmological models. As an illustrative example, we find that a decisive statement can be made comparing the $\Lambda$CDM and RHCT cosmological models using two weeks of data from the Einstein Telescope., Comment: 10 pages, 7 figures, Accepted by ApJ
Published: 2020
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30. Revisiting scalar and tensor perturbations in a nonlocal gravity

Author: Zong-Hong Zhu and Shuxun Tian
Subjects: Physics, 010308 nuclear & particles physics, Gravitational wave, FOS: Physical sciences, Perturbation (astronomy), Observable, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, LIGO, Metric expansion of space, Auxiliary field, Amplitude, 0103 physical sciences, Computer Science::Data Structures and Algorithms, 010306 general physics, Luminosity distance, Mathematical physics
Abstract: Nonlocal RT gravity is a successful modified gravity theory, which not only explains the late-time cosmic acceleration but also behaves well in the solar system. Previous analysis generally assumes the auxiliary field $S_i$ vanishes at the cosmic background. However, we find the background $S_i$ is proportional to $a^2$ with the expansion of the universe. Then we discuss the influence of the nonzero background $S_i$ on the cosmic background evolution, the scalar and tensor perturbations. We find the cosmic background evolution is independent of $S_i$, and the influence of the nonzero background $S_i$ on the weak field limit at solar system scales is negligible. For the tensor perturbation, we find the only possible observable effect is the influence of nonzero background $S_i$ on the LIGO gravitational wave amplitude and also luminosity distance. Future high redshift gravitational wave observations could be used to constrain the background value of $S_i$., Comment: 5 pages, PRD in press
Published: 2019
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31. Direct test of the FLRW metric from strongly lensed gravitational wave observations

Author: Zong-Hong Zhu, Jingzhao Qi, Yu Pan, Shuo Cao, Zhoujian Cao, Jin Li, and Marek Biesiada
Subjects: 0301 basic medicine, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Galaxies and clusters, lcsh:Medicine, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Curvature, Article, Cosmology, General Relativity and Quantum Cosmology, 03 medical and health sciences, symbols.namesake, Theoretical physics, 0302 clinical medicine, Friedmann–Lemaître–Robertson–Walker metric, Homogeneity (physics), lcsh:Science, media_common, Physics, Multidisciplinary, Einstein Telescope, Gravitational wave, lcsh:R, Isotropy, Universe, 030104 developmental biology, gravitational waves, FLRW metric, symbols, lcsh:Q, 030217 neurology & neurosurgery, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The assumptions of large-scale homogeneity and isotropy underly the familiar Friedmann-Lema\^{\i}tre-Robertson-Walker (FLRW) metric that appears to be an accurate description of our Universe. In this paper, we propose a new strategy of testing the validity of the FLRW metric, based on the galactic-scale lensing systems where strongly lensed gravitational waves and their electromagnetic counterparts can be simultaneously detected. Each strong lensing system creates opportunity to infer the curvature parameter of the Universe. Consequently, combined analysis of many such systems will provide a model-independent tool to test the validity of the FLRW metric. Our study demonstrates that the third-generation ground based GW detectors, like the Einstein Telescope (ET) and space-based detectors, like the Big Bang Observer (BBO), are promising concerning determination of the curvature parameter or possible detection of deviation from the FLRW metric. Such accurate measurements of the FLRW metric can become a milestone in precision GW cosmology., Comment: 13 pages, 2 figures, 1 table
Published: 2019
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32. The gas depletion factor in galaxy clusters: implication from Atacama Cosmology Telescope Polarization experiment measurements

Author: Tonghua Liu, Shuo Cao, Marek Biesiada, Sylwia Miernik, Jingzhao Qi, Xiaogang Zheng, and Zong-Hong Zhu
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), FOS: Physical sciences, lcsh:Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Computer Science::Digital Libraries, 01 natural sciences, lcsh:QB460-466, 0103 physical sciences, Cluster (physics), lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, 010303 astronomy & astrophysics, Engineering (miscellaneous), Astrophysics::Galaxy Astrophysics, Galaxy cluster, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Gas depletion, polarization experiment, Atacama Cosmology Telescope, Redshift, Baryon, lcsh:QC770-798, Mass fraction, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The gas depletion factor $\gamma(z)$, i.e., the average ratio of the gas mass fraction to the cosmic mean baryon fraction of galaxy clusters, plays a very important role in the cosmological application of the gas mass fraction measurements. In this paper, using the newest catalog of 182 galaxy clusters detected by the Atacama Cosmology Telescope (ACT) Polarization experiment, we investigate the possible redshift evolution of $\gamma(z)$ through a new cosmology-independent method. The method is based on non-parametric reconstruction using the measurements of Hubble parameters from cosmic chronometers. Unlike hydrodynamical simulations suggesting constant depletion factor, our results reveal the trend of $\gamma(z)$ decreasing with redshift. This result is supported by a parametric model fit as well as by calculations on the reduced ACTPol sample and on the alternative sample of 91 SZ clusters reported earlier in ACT compilation. Discussion of possible systematic effects leaves an open question about validity of the empirical relation $M_{tot}$-$f_{gas}$ obtained on very close clusters. These results might pave the way to explore the hot gas fraction within large radii of galaxy clusters as well as its possible evolution with redshift, which should be studied further on larger galaxy cluster samples in the upcoming X-ray/SZ cluster surveys., Comment: 9 pages, 6 figures, 1 table. Comments welcome
Published: 2019
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33. Newtonian approximation and possible time-varying $G$ in nonlocal gravities

Author: Zong-Hong Zhu and Shuxun Tian
Subjects: Physics, Gravity (chemistry), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Gravitational constant, Gravitation, De Sitter universe, Binary star, Uniqueness, Constant (mathematics), Mathematical physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Newtonian approximation with a nonvanishing nonlocal background field is analyzed for the scalar-tensor nonlocal gravity and nonlocal Gauss-Bonnet gravity. For these two theories, our calculations show that the Newtonian gravitational constant $G$ is time-varying and $|\dot{G}/G|=\mathcal{O}(H_0)$ for the general case of cosmological background evolution, which is similar to the results of the Deser-Woodard and Maggiore-Mancarella theories. Therefore, observations about the orbit period of binary star (or star-planet) systems could rule out these theories. One thing worth mentioning is that the nonlocal Gauss-Bonnet gravity gives $\Psi=\Phi$ and a constant $G$ in the de Sitter phase. Our results also highlight the uniqueness of the RT model [M. Maggiore, \href{http://dx.doi.org/10.1103/PhysRevD.89.043008}{Phys. Rev. D {\bf 89}, 043008 (2014)}], which is the only nonlocal gravity theory that can successfully describe the gravitational phenomena from solar system to cosmological scales for now., Comment: 6 pages, version published in PRD
Published: 2019

34. Inspiraling Double Compact Object Detection and Lensing Rate: Forecast for DECIGO and B-DECIGO

Author: Shuo Cao, Marek Biesiada, Aleksandra Piórkowska-Kurpas, Seiji Kawamura, Shaoqi Hou, Xuheng Ding, Zong-Hong Zhu, and Xi-Long Fan
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Gravitational-wave observatory, Gravitational wave, Strong gravitational lensing, Population, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Context (language use), Compact star, Gravitational lens, Space and Planetary Science, Observatory, Astrophysics - High Energy Astrophysical Phenomena, education
Abstract: Emergence of gravitational wave (GW) astronomy revived the interest in exploring the low frequency GW spectrum inaccessible from the ground. Satellite GW observatory DECIGO in its original configuration and the currently proposed smaller scale B-DECIGO are aimed to cover deci-Hertz part of the GW spectrum, which fills the gap between LISA mili-Hertz and deca- to kilo-Hertz range probed by ground-based detectors. In this paper we forecast the detection rates of inspiraling double compact objects (DCOs) and the unresolved confusion noise from these sources in DECIGO and B-DECIGO. In the context of DECIGO we use, for the first time, the population synthesis intrinsic inspiral rates of NS-NS, BH-NS and BH-BH systems. We also estimate the expected gravitational lensing rates of such sources for DECIGO and B-DECIGO. The result is that yearly detection of DCOs inspirals for the DECIGO is of order of $10^4 - 10^5$, while for a much smaller scale B-DECIGO they are about $10^2 - 10^4$ depending on the DCO population considered. Taking into account that considerable part of these events would be detectable by ground-based GW observatories the added value of DECIGO/B-DECIGO could be substantial. DECIGO will also be able to register $5-50$ lensed NS-NS inspirals and up to O(100) BH-BH inspirals. On the contrary, predictions for the B-DECIGO are pessimistic: only the optimistic common envelope scenario of DCO formation could yield a few lensed BH-BH inspirals per year. We also address the question of the magnification bias in the GW event catalogs of DECIGO and B-DECIGO., 12 pages, 7 figures, submitted to the Astrophysical Journal
Published: 2021
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35. 'Conserved charges' of the Bondi-Metzner-Sachs algebra in the Brans-Dicke theory *

Author: Zong-Hong Zhu and Shaoqi Hou
Subjects: High Energy Physics - Theory, Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Lorentz transformation, Scalar (physics), FOS: Physical sciences, Astronomy and Astrophysics, Charge (physics), Conformal map, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Algebra, symbols.namesake, High Energy Physics - Theory (hep-th), 0103 physical sciences, Brans–Dicke theory, Homogeneous space, symbols, 010306 general physics, Instrumentation, Spin-½, Asymptotically flat spacetime
Abstract: The asymptotic symmetries in Brans-Dicke theory are analyzed using Penrose's conformal completion method, which is independent of the coordinate system used. These symmetries indeed include supertranslations and Lorentz transformations for an asymptotically flat spacetime. With the Wald-Zoupas formalism, "conserved charges" and fluxes of the Bondi-Metzner-Sachs algebra are computed. The scalar degree of freedom contributes only to the Lorentz boost charge, although it plays a role in various fluxes. The flux-balance laws are further used to constrain displacement memory, spin memory and center-of-mass memory effects., Comment: 34 pages, 0 figure. Corrected typos, and added some discussions. Accepted for publication in Chinese Physics C. Minor corrections
Published: 2021
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36. Lorentz Invariance Violation Limits from the Spectral-lag Transition of GRB 190114C

Author: En-Wei Liang, Shen-Shi Du, Lu-Yao Jiang, Xue-Feng Wu, Jun-Jie Wei, He Gao, Lin Lan, Zong-Hong Zhu, Bin-Bin Zhang, Zi-Ke Liu, and Zi-Ming Zhou
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photon, Astrophysics::High Energy Astrophysical Phenomena, Lag, FOS: Physical sciences, Astronomy and Astrophysics, Lorentz covariance, Gravitation, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Standard-Model Extension, Space and Planetary Science, Quantum gravity, Statistical physics, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Energy (signal processing)
Abstract: The spectral lags of gamma-ray bursts (GRBs) have been viewed as the most promising probes of the possible violations of Lorentz invariance (LIV). However, these constraints usually depend on the assumption of the unknown intrinsic time lag in different energy bands and the use of a single highest-energy photon. A new approach to test the LIV effects has been proposed by directly fitting the spectral lag behavior of a GRB with a well-defined transition from positive lags to negative lags. This method simultaneously provides a reasonable formulation of the intrinsic time lag and robust lower limits on the quantum-gravity energy scales ($E_{\rm QG}$). In this work, we perform a global fitting to the spectral lag data of GRB~190114C by considering the possible LIV effects based on a Bayesian approach. We then derive limits on $E_{\rm QG}$ and the coefficients of the Standard Model Extension. The Bayes factors output in our analysis shows a very strong evidence for the spectral-lag transition in GRB~190114C. Our constraints on a variety of isotropic and anisotropic coefficients for LIV are somewhat weaker than existing bounds, but they can be viewed as comparatively robust and have the promise to complement existing LIV constraints. The observations of GRBs with higher-energy emissions and higher temporal resolutions will contribute to a better formulation of the intrinsic time lag and more rigorous LIV constraints in the dispersive photon sector., 13 pages, 6 figures, 2 tables, the version accepted for publication in the Astrophysical Journal (ApJ)
Published: 2020
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37. Prospects of strongly lensed repeating fast radio bursts: complementary constraints on dark energy evolution

Author: Zhengxiang Li, Bin Liu, He Gao, and Zong-Hong Zhu
Subjects: Physics, education.field_of_study, COSMIC cancer database, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Canadian Hydrogen Intensity Mapping Experiment, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Radio telescope, symbols.namesake, 0103 physical sciences, symbols, Dark energy, 010306 general physics, education, Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Fast radio bursts (FRBs) are highly dispersed and probably extragalactic radio flashes with millisecond-duration. Recently, the Canadian Hydrogen Intensity Mapping Experiment (using the CHIME/FRB instrument) has reported detections of 13 FRBs during a pre-commissioning phase. It is more exciting that one of the 13 FRBs is a second source of repeaters which suggests that CHIME/FRB and other wide-field sensitive radio telescopes will find a substantial population of repeating FRBs. We have proposed strongly lensed repeating FRBs as a precision cosmological probe, e.g. constraining the Hubble constant and model-independently estimating the cosmic curvature. Here, we study complementary constraints on the equation of state of dark energy from strongly lensed FRBs to currently available popular probes. It is found that, in the framework of Chevalier-Polarski-Linder parametrization, adding time delay measurement of 30 strongly lensed FRB systems to cosmic microwave background radiation and type Ia supernovae can improve the dark energy figure of merit by a factor 2. In the precision cosmology era, this improvement is of great significance for studying the nature of dark energy., Comment: 16 pages, 4 figures, 1 table. arXiv admin note: text overlap with arXiv:1904.11751
Published: 2019
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38. Gravitational Lensing of Gravitational Waves: Rotation of Polarization Plane

Author: Zong-Hong Zhu, Xi-Long Fan, and Shaoqi Hou
Subjects: Physics, 010308 nuclear & particles physics, Gravitational wave, business.industry, Detector, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Polarization (waves), 01 natural sciences, General Relativity and Quantum Cosmology, Radiation pattern, Interferometry, symbols.namesake, Optics, Amplitude, Gravitational lens, 0103 physical sciences, Faraday effect, symbols, 010306 general physics, business
Abstract: Similar to the light, gravitational waves traveling in multiple paths may arrive at the same location if there is a gravitational lens on their way. Apart from the magnification of the amplitudes and the time delay between the gravitational wave rays, gravitational lensing also rotates their polarization planes. This results in the changes in the antenna pattern function, which describes the response of the detector to its relative orientation to the gravitational wave. These effects are all reflected in the strain, the signal registered by the interferometers. The gravitational wave rays in various directions stimulate different strains. Their strains differ from each other due to different magnification factors, the phases and the rotation of the polarization plane. The phase difference mainly comes from the time delay. Moreover, the rotation of the polarization plane seemingly introduces the \textit{apparent} vector polarizations, when these strains are compared with each other. Because of the smallness of the deflection angles, the effect of the rotation is negligible., Comment: 6 pages, 1 figure. Match the published version
Published: 2019
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39. How does the Earth's rotation affect predictions of gravitational wave strong lensing rates?

Author: Zong-Hong Zhu, Kai Liao, Lilan Yang, Xuheng Ding, and Marek Biesiada
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Einstein Telescope, Gravitational wave, Monte Carlo method, Detector, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rotation, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Amplitude, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Physics::Space Physics, 010303 astronomy & astrophysics, Event (particle physics), Astrophysics - Cosmology and Nongalactic Astrophysics, 0105 earth and related environmental sciences, Earth's rotation
Abstract: The next generation of ground-based gravitational wave (GW) detectors, e.g. the Einstein Telescope, is expected to observe a significant number of strongly lensed GW events as predicted in many previous papers. However, all these works ignored the impact of the Earth's rotation on this prediction. Multiple lensed images arrive at the Earth at different time, thus the ground-based detector has different responses to the lensed images due to different orientations of the detector relative to the GW source direction. Therefore the amplitudes of the GW signal from different images are modulated appropriately, in addition to the lensing magnification. In order to assess this effect, we performed Monte Carlo simulations to calculate the event rate of lensed GW signals. Our conclusion is that the Earth's rotation has a non-negligible impact on the event rate of lensed GW image. The updated event rates decrease by factors of $\sim40\%, \sim20\%, \sim10\%$, for NS-NS, BH-NS, BH-BH systems respectively., Comment: 9 pages, 3 figures, 1 table; Accepted by ApJ
Published: 2019
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40. KAGRA: 2.5 generation interferometric gravitational wave detector

Author: Hirotaka Takahashi, H. Tahara, T. Miyamoto, Kazuyuki Tanaka, Y. Saito, Mitsuhiro Fukushima, Y. Liu, Albert K. H. Kong, Yoshinori Fujii, G. Kang, Innocenzo M. Pinto, E. J. Son, Sakae Araki, Osamu Miyakawa, Hyun Lee, K. Hasegawa, B. Ikenoue, H-S. Kuo, B. H. Hsieh, Ken Ono, F. L. Lin, C. Z. Huang, Xu W. R., Takaaki Kajita, Yuki Inoue, Akiteru Takamori, Motoyuki Saijo, F. Matsushima, T. Yoshioka, Ken-ichi Nakao, Ni W. T., Kentaro Komori, M. A. Barton, T. Ushiba, R. Flaminio, Simon Zeidler, Luca Baiotti, F. Uraguchi, Y. Sakai, Ettore Majorana, K. Awai, Kieran Craig, K. Yamamoto, Daisuke Tatsumi, Atsushi Nishizawa, Yousuke Itoh, Oh S. H., K. Sakai, S. Kanbara, Kipp Cannon, R. Kozu, Jong-Dae Park, Mitsuru Musha, M. Fukunaga, S. Sato, Masashi Ohkawa, J. Kasuya, N. Uchikata, T. Matsui, Shinya Kanemura, Kyung-Suk Cho, Yutaro Enomoto, S. Wada, Hiroyuki Nakano, Y. Watanabe, Hisa-aki Shinkai, Yuta Michimura, S. Yamamoto, Katsuya Hashino, S. Ueki, Tomoya Kinugawa, J. Kim, A. Miyamoto, W. Morii, Y. Kataoka, Masatake Ohashi, Akito Araya, T. Furuhata, Tai Hyun Yoon, S. Kirii, T. Kaji, Satoshi Tsuchida, Kentaro Somiya, Sachiko Kuroyanagi, Naoki Seto, Nobutada Kimura, T. Kawasaki, Shinji Miyoki, Y. Sasaki, Naoko Ohishi, A. Suemasa, Takahiro Yamamoto, F. E. P. Arellano, T. Tomura, Nobuyuki Kanda, H. K. Tanaka, Masaki Ando, Shigeki Hirobayashi, S. Bae, M. Marchio, T. Ochi, T. Shimoda, M. Sasai, A. Yamamoto, Eiichi Hirose, Kouji Nakamura, Jun'ichi Yokoyama, H. Yuzurihara, Young-Min Kim, Yoichi Aso, Norichika Sago, Oh J. J., Y. K. Chu, M. H. P. M. van Putten, A. Shoda, Takashi Nakamura, Zong-Hong Zhu, C. Chen, Hideyuki Tagoshi, Y. Arai, T. Morozumi, Ting-Wai Chiu, Yasufumi Kojima, Rajesh Kumar, N. Sato, Chunglee Kim, Kimio Tsubono, Hyeseung Lee, C. P. Ooi, S. S. Pan, K. Miyo, K. Oohara, M. Kaneyama, M. Leonardi, Takayuki Tomaru, S. Saitou, Kazunari Eda, Takahiro Yamada, Koya Arai, Hiroki Takeda, T. Wakamatsu, Tomotada Akutsu, S. Tanioka, Kazuhiro Hayama, M. Nakano, Kohei Doi, Masako Kakizaki, Sadakazu Haino, K. Ueno, Yuichiro Sekiguchi, W. S. Kim, Norikatsu Mio, K. Izumi, Takamasa Suzuki, Seiji Kawamura, Haruki Kitazawa, Masa-Katsu Fujimoto, L. Naticchioni, T. Shishido, Naoki Aritomi, K. Yokogawa, E. Capocasa, Enzo Nicolas Tapia San Martin, Takashi Uchiyama, Kunihito Ioka, T. Uehara, T. Narikawa, Y. Moriwaki, Manami Sasaki, Ryutaro Takahashi, Keiko Kokeyama, Hyang Woon Lee, Koki Okutomi, Y. Obuchi, Jinsook Kim, T. Yokozawa, Y. Kitaoka, N. Kawai, Guo-Chin Liu, Takahiro Tanaka, W. Creus, Hideki Asada, Masaru Shibata, Shuhei Mano, Soichiro Morisaki, L. N. Quynh, S. Atsuta, C-Y. Lin, Takashi Sato, Koji Nagano, M. Kamiizumi, Shigeo Nagano, Kei Kotake, H. Vocca, F. Travasso, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), KAGRA, Laboratoire d'Annecy de Physique des Particules (LAPP), Akutsu, T., Ando, M., Arai, K., Arai, Y., Araki, S., Araya, A., Aritomi, N., Asada, H., Aso, Y., Atsuta, S., Awai, K., Bae, S., Baiotti, L., Barton, M. A., Cannon, K., Capocasa, E., Chen, C. -S., Chiu, T. -W., Cho, K., Chu, Y. -K., Craig, K., Creus, W., Doi, K., Eda, K., Enomoto, Y., Flaminio, R., Fujii, Y., Fujimoto, M. -K., Fukunaga, M., Fukushima, M., Furuhata, T., Haino, S., Hasegawa, K., Hashino, K., Hayama, K., Hirobayashi, S., Hirose, E., Hsieh, B. H., Huang, C. -Z., Ikenoue, B., Inoue, Y., Ioka, K., Itoh, Y., Izumi, K., Kaji, T., Kajita, T., Kakizaki, M., Kamiizumi, M., Kanbara, S., Kanda, N., Kanemura, S., Kaneyama, M., Kang, G., Kasuya, J., Kataoka, Y., Kawai, N., Kawamura, S., Kawasaki, T., Kim, C., Kim, J., Kim, J. C., Kim, W. S., Kim, Y. -M., Kimura, N., Kinugawa, T., Kirii, S., Kitaoka, Y., Kitazawa, H., Kojima, Y., Kokeyama, K., Komori, K., Kong, A. K. H., Kotake, K., Kozu, R., Kumar, R., Kuo, H. -S., Kuroyanagi, S., 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, S., Marchio, M., Matsui, T., Matsushima, F., Michimura, Y., Mio, N., Miyakawa, O., Miyamoto, A., Miyamoto, T., Miyo, K., Miyoki, S., Morii, W., Morisaki, S., Moriwaki, Y., Morozumi, T., Musha, M., Nagano, K., Nagano, S., Nakamura, K., Nakamura, T., Nakano, H., Nakano, M., Nakao, K., Narikawa, T., Naticchioni, L., Quynh, L. N., Ni, W. -T., Nishizawa, A., Obuchi, Y., Ochi, T., Oh, J. J., Oh, S. H., Ohashi, M., Ohishi, N., Ohkawa, M., Okutomi, K., Ono, K., Oohara, K., Ooi, C. P., Pan, S. -S., Park, J., Arellano, F. E. P., Pinto, I., Sago, N., Saijo, M., Saitou, S., Saito, Y., Sakai, K., Sakai, Y., Sasai, M., Sasaki, M., Sasaki, Y., Sato, S., Sato, N., Sato, T., Sekiguchi, Y., Seto, N., Shibata, M., Shimoda, T., Shinkai, H., Shishido, T., Shoda, A., Somiya, K., Son, E. J., Suemasa, A., Suzuki, T., Tagoshi, H., Tahara, H., Takahashi, H., Takahashi, R., Takamori, A., Takeda, H., Tanaka, H., Tanaka, K., Tanaka, T., Tanioka, S., Martin, E. N. T. S., Tatsumi, D., Tomaru, T., Tomura, T., Travasso, F., Tsubono, K., Tsuchida, S., Uchikata, N., Uchiyama, T., Uehara, T., Ueki, S., Ueno, K., Uraguchi, F., Ushiba, T., van Putten, M. H. P. M., Vocca, H., Wada, S., Wakamatsu, T., Watanabe, Y., Xu, W. -R., Yamada, T., Yamamoto, A., Yamamoto, K., Yamamoto, S., Yamamoto, T., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoon, T. H., Yoshioka, T., Yuzurihara, H., Zeidler, S., and Zhu, Z. -H.
Subjects: Physics - Instrumentation and Detectors, detector: cryogenics, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), detector: network, 7. Clean energy, 01 natural sciences, General Relativity and Quantum Cosmology, Laser interferometry, Einstein Telescope, temperature: low, 0103 physical sciences, LCGT, Interferometric gravitational wave detector, KAGRA, laser: interferometer, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], LIGO, mirror, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, detector: design, 0105 earth and related environmental sciences, Physics, COSMIC cancer database, Gravitational wave, Detector, gravitational radiation, Astronomy, Astronomy and Astrophysics, Gravitational Wave Detector, Instrumentation and Detectors (physics.ins-det), trigger, gravitational radiation detector, detector: sensitivity, VIRGO, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: 著者人数: KAGRA collaboration 198名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 和泉, 究), Number of authors: KAGRA collaboration 198 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Izumi, Kiwamu), Accepted: 2018-11-19, 資料番号: SA1180423000
Published: 2019
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41. Corrections to the gravitational wave phasing

Author: Zong-Hong Zhu, Xi-Long Fan, and Shaoqi Hou
Subjects: Physics, Work (thermodynamics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Gravitational wave, Isotropy, Phase (waves), Order (ring theory), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, Amplitude, High Energy Physics - Phenomenology (hep-ph), Quantum electrodynamics, 0103 physical sciences, Astronomical interferometer, Sensitivity (control systems), 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The gravitational wave, traveling a long cosmological distance to reach interferometers, interacts with the (homogeneous and isotropic) cosmological background, so generally speaking, its amplitude and phase are modified in some nontrivial way. As the sensitivity of interferometers is improved, one may detect corrections to the short-wavelength approximation, which naturally includes the information of cosmological evolution. In this work, the Newman-Penrose variable $\Psi_4$ has been calculated to show that there are two new corrections to the short-wavelength approximation. One formally occurs at the first post-Newtonian order but is highly suppressed by the Hubble parameters; the other occurs at the fifth post-Newtonian order, which is due to the variation of the amplitude. The first correction contains the evolution of the Universe, but it may not be easily detected. The second one indicates that the short-wavelength approximation has to be corrected, when the more accurate waveforms with the higher-order post-Newtonian terms are calculated., Comment: 12 pages, 2 figures. Match the published version
Published: 2019
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42. Testing the Schwarzschild metric in a strong field region with the Event Horizon Telescope

Author: Shuxun Tian and Zong-Hong Zhu
Subjects: Event Horizon Telescope, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, General relativity, Event horizon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Black hole, Theoretical physics, Schwarzschild metric, Astrophysics - High Energy Astrophysical Phenomena, Schwarzschild radius, Free parameter
Abstract: Testing gravity theory in the strong field region becomes a reality due to the observations of gravitational waves and black hole shadows. In this paper, we discuss how to constrain the possible deviations of the classical general relativity with the image of M87* observed by the Event Horizon Telescope. More precisely, we want to know where is the event horizon for a non-rotating black hole. General relativity predicts the horizon is located at the Schwarzschild radius $r_\textrm{s}$, while other gravity theories may give different predictions. We propose a parameterized Schwarzschild metric (PSM) in which the horizon is located at $r=nr_\textrm{s}$, where $n$ is a real free parameter, and prove general relativity with nonlinear electrodynamics allows $n\neq1$. In the weak field region, the PSM is equivalent to the Schwarzschild metric regardless of the value of $n$. In the strong field region, the difference between the PSM and Schwarzschild metric would leave an imprint on the shadow image. We present detailed calculations and discussions on the black hole shadows with large background light source and accretion disk in the PSM framework. More importantly, we point out that $n\approx2$ can be used to explain why the black hole mass measured by the shadow is a factor of about two larger than the previous gas dynamics measurements. If this explanation is confirmed to be right, then this phenomenon, together with the late-time cosmological acceleration, will be very important to test gravity theories., Comment: 14 pages, 9 figures, PRD accepted
Published: 2019
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43. Implications from simulated strong gravitational lensing systems: constraining cosmological parameters using Gaussian Processes

Author: Yuting Liu, Shuo Cao, Tonghua Liu, Xuan Ji, Shuaibo Geng, Zong-Hong Zhu, and Jia Zhang
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Strong gravitational lensing, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Omega, General Relativity and Quantum Cosmology, Redshift, Cosmology, symbols.namesake, Gravitational lens, Space and Planetary Science, 0103 physical sciences, symbols, Planck, Parametric equation, 010303 astronomy & astrophysics, Gaussian process, Astrophysics - Cosmology and Nongalactic Astrophysics, 0105 earth and related environmental sciences
Abstract: Strongly gravitational lensing systems (SGL) encodes cosmology information in source/lens distance ratios $\mathcal{D}_{\rm obs}=\mathcal{D}_{\rm ls}/\mathcal{D}_{\rm s}$, which can be used to precisely constrain cosmological parameters. In this paper, based on future measurements of 390 strong lensing systems from the forthcoming LSST survey, we have successfully reconstructed the distance ratio $\mathcal{D}_{\rm obs}$ (with the source redshift $z_s\sim 4.0$), directly from the data without assuming any parametric form. A recently developed method based on model-independent reconstruction approach, Gaussian Processes (GP) is used in our study of these strong lensing systems. Our results show that independent measurement of the matter density parameter ($\Omega_m$) could be expected from such strong lensing statistics. More specifically, one can expect $\Omega_m$ to be estimated at the precision of $\Delta\Omega_m\sim0.015$ in the concordance $\Lambda$CDM model, which provides comparable constraint on $\Omega_m$ with Planck 2015 results. In the framework of the modified gravity theory (DGP), 390 detectable galactic lenses from future LSST survey would lead to stringent fits of $\Delta\Omega_m\sim0.030$. \textbf{Finally, we have discussed three possible sources of systematic errors (sample incompleteness, the determination of length of lens redshift bin, and the choice of lens redshift shells), and quantified their effects on the final cosmological constraints. Our results strongly indicate that future strong lensing surveys, with the accumulation of a larger and more accurate sample of detectable galactic lenses, will considerably benefit from the methodology described in this analysis. }
Published: 2019
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44. First cryogenic test operation of underground km-scale gravitational-wave observatory KAGRA

Author: K. Yamamoto, Albert K. H. Kong, Yoshinori Fujii, S. Wada, Ken Ono, S. Tanioka, Kohei Doi, T. Miyamoto, Takamasa Suzuki, Naoki Seto, Nobutada Kimura, C. Chen, Hideyuki Tagoshi, Hyeseung Lee, Zong-Hong Zhu, Takahiro Yamada, Akito Araya, Soichiro Morisaki, Yuta Michimura, A. Miyamoto, E. N. Tapia San Martin, E. Capocasa, Norikatsu Mio, Tomoya Kinugawa, Rajesh Kumar, Daisuke Tatsumi, T. Matsui, N. Kawai, I. Murakami, B. H. Hsieh, Koki Okutomi, W. Creus, Takaaki Kajita, Yuki Inoue, S. Yamamoto, Katsuya Hashino, S. Atsuta, Shigeki Hirobayashi, M. H. P. M. van Putten, Yuichiro Sekiguchi, Y. M. Kim, Jinsook Kim, Hideki Asada, K. Miyo, K. Oohara, Y. Sakai, Atsushi Nishizawa, J. Kasuya, T. Yokozawa, Y. Moriwaki, Masaru Shibata, Kyung-Suk Cho, T. Kaji, Seiji Kawamura, S. Sato, Masa-Katsu Fujimoto, T. Furuhata, Yoshikazu Namai, K. Yokogawa, H. Yuzurihara, Shinji Miyoki, Y. Sasaki, Shigeo Nagano, K. Sakai, Yoshiyuki Obuchi, A. Hagiwara, C-Y. Lin, Takashi Uchiyama, Kei Kotake, Hyang Woon Lee, T. Yoshioka, Kunihito Ioka, Ken-ichi Nakao, R. Flaminio, T. Morozumi, Takayuki Tomaru, M. Kaneyama, Seog Oh, Kimio Tsubono, Koya Arai, Hiroki Takeda, Motoyuki Saijo, Hiroyuki Nakano, Y. K. Chu, T. Kawasaki, Naoki Aritomi, Satoshi Tsuchida, S. Bae, Jong-Dae Park, W-R. Xu, C. Z. Huang, T. Ushiba, Y. Kitaoka, F. E. Peña Arellano, Guo-Chin Liu, W. S. Kim, H. Vocca, Kieran Craig, T. Wakamatsu, Y. Liu, Tomotada Akutsu, T. Shimoda, C. P. Ooi, Takashi Sato, S. Kanbara, Simon Zeidler, Luca Baiotti, Yousuke Itoh, Ryutaro Takahashi, Y. Watanabe, Ting-Wai Chiu, S. Saitou, Koji Nagano, M. Kamiizumi, M. Nakano, A. Shoda, Sachiko Kuroyanagi, S. Ueki, Masashi Ohkawa, M. A. Barton, Akiteru Takamori, N. Sato, Masako Kakizaki, F. Matsushima, Hisa-aki Shinkai, T. Narikawa, Manami Sasaki, M. Marchio, T. Ochi, L. Nguyen Quynh, Kipp Cannon, J. Kim, G. Kang, Yoichi Aso, L. Naticchioni, T. Shishido, Shinya Kanemura, Keiko Kokeyama, Yutaro Enomoto, Masatake Ohashi, Takashi Nakamura, A. Suemasa, H. Tahara, Shuhei Mano, S. S. Pan, A. Ueda, Sakae Araki, Naoko Ohishi, Osamu Miyakawa, K. Izumi, M. Sasai, Y. Kataoka, Kazuyuki Tanaka, Takahiro Tanaka, F. Travasso, Y. Saito, Hirotaka Takahashi, Hyun Lee, Y. Arai, K. Hasegawa, B. Ikenoue, H-S. Kuo, Mitsuhiro Fukushima, F. L. Lin, Innocenzo M. Pinto, E. J. Son, Shinichi Terashima, N. Uchikata, T. Uehara, Jun'ichi Yokoyama, Kentaro Komori, Yasufumi Kojima, Chunglee Kim, Fumihiro Uraguchi, Sadakazu Haino, K. Ueno, R. Kozu, Norichika Sago, K. Awai, W. Morii, S. Kirii, Kentaro Somiya, T. Tomura, Masaki Ando, Kazunari Eda, Kazuhiro Hayama, Mitsuru Musha, Takahiro Yamamoto, Nobuyuki Kanda, H. K. Tanaka, Eiichi Hirose, Kouji Nakamura, M. Leonardi, Haruki Kitazawa, Ettore Majorana, M. Fukunaga, John J. Oh, Tai Hyun Yoon, Wei-Tou Ni, A. Yamamoto, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), KAGRA, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics - Instrumentation and Detectors, Gravitational-wave observatory, Physics and Astronomy (miscellaneous), Physics::Instrumentation and Detectors, sapphire, Physics::Optics, Cryogenics, 01 natural sciences, 7. Clean energy, General Relativity and Quantum Cosmology, law.invention, cryogenic laser interferometer, Observatory, law, underground, gravitational waves, mirror, Physics, Detector, Mathematics::History and Overview, Astrophysics::Instrumentation and Methods for Astrophysics, detector: stability, alignment, Instrumentation and Detectors (physics.ins-det), observatory, Interferometry, cryogenics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Instrumentation and Methods for Astrophysics, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Optics, 0103 physical sciences, noise: thermal, surface, KAGRA, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, Gravitational wave, business.industry, gravitational radiation, Michelson interferometer, temperature, frequency: low, gravitational radiation detector: interferometer, business
Abstract: 著者人数: KAGRA Collaboration 203名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 和泉, 究), Number of authors: KAGRA collaboration 203 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Izumi, Kiwamu), Accepted: 2019-06-11, 資料番号: SA1190107000
Published: 2019
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45. Complementary constraints on dark energy equation of state from strongly lensed gravitational wave

Author: Zong-Hong Zhu, Bin Liu, and Zhengxiang Li
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Einstein Telescope, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Strong gravitational lensing, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Cosmology, General Relativity and Quantum Cosmology, symbols.namesake, Space and Planetary Science, 0103 physical sciences, Dark energy, symbols, Baryon acoustic oscillations, 010303 astronomy & astrophysics, Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: It has been shown that time delay of strong gravitational lensing is not only an effective cosmological probe to constrain the Hubble constant, the matter density and the curvature of the universe but also useful for breaking the degeneracy of the dark energy equation of state and thus provide complementarity with other popular probes, such as type Ia supernovae, baryon acoustic oscillations, and cosmic microwave background radiation. Interestingly, compared to traditional strong lensing systems where quasars act as sources, strongly lensed gravitational waves (GWs) from compact binary coalescence and their electromagnetic (EM) counterparts systems have been recently proposed to be more powerful for studying cosmology since GWs and their EM counterparts are transients. Short durations of GWs and their EM counterparts are very advantageous to time delay measurement and lens profile modeling. Here, in the framework of Chevalier-Polarski-Linder (CPL) parametrization, we investigate improvement of constraining power on dark energy equation of state due to including time delay measurements of strong lensed GW systems. It is suggested that, on the basis of the third generation ground-based detector, e.g. Einstein Telescope, adding time delay of only 30 strong lensed GW systems to type Ia supernovae and cosmic microwave background radiation can improve the dark energy figure of merit by a factor 2. For the traditional standard siren method where the uncertainties of luminosity distances of GWs are $\sim10\%$, a few $\times~10^4$ events are expected to present similar constraints. In the precision cosmology era, this progress is of great significance for studying the nature of dark energy., Comment: 6 pages, 5 figures, 1 table, to appear in MNRAS
Published: 2019
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46. Cosmology-independent estimate of the fraction of baryon mass in the IGM from fast radio burst observations

Author: Zong-Hong Zhu, Bing Zhang, Jun-Jie Wei, He Gao, Yuan-Pei Yang, and Zhengxiang Li
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Type (model theory), 01 natural sciences, Galaxy, Cosmology, Redshift, General Relativity and Quantum Cosmology, Baryon, Supernova, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Luminosity distance, 0105 earth and related environmental sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The excessive dispersion measure (DM) of fast radio bursts (FRBs) has been proposed to be a powerful tool to study intergalactic medium (IGM) and to perform cosmography. One issue is that the fraction of baryons in the IGM, $f_{\rm IGM}$, is not properly constrained. Here we propose a method of estimating $f_{\rm IGM}$ using a putative sample of FRBs with the measurements of both DM and luminosity distance $d_{\rm L}$. The latter can be obtained if the FRB is associated with a distance indicator (e.g. a gamma-ray burst or a gravitational wave event), or the redshift $z$ of the FRB is measured and $d_{\rm L}$ at the corresponding $z$ is available from other distance indicators (e.g. type Ia supernovae) at the same redshift. Since $d_{\rm L}/{\rm DM}$ essentially does not depend on cosmological parameters, our method can determine $f_{\rm IGM}$ independent of cosmological parameters. We parameterize $f_{\rm IGM}$ as a function of redshift and model the DM contribution from a host galaxy as a function of star formation rate. Assuming $f_{\rm IGM}$ has a mild evolution with redshift with a functional form and by means of Monte Carlo simulations, we show that an unbiased and cosmology-independent estimate of the present value of $f_{\rm IGM}$ with a $\sim 12\%$ uncertainty can be obtained with 50 joint measurements of $d_{\rm L}$ and DM. In addition, such a method can also lead to a measurement of the mean value of DM contributed from the local host galaxy., Comment: 6 pages, 5 figures, to appear in ApJ
Published: 2019
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47. Quantization of the nonstandard propagating gravitational waves in the cosmological background

Author: Zong-Hong Zhu and Shuxun Tian
Subjects: Physics, 010308 nuclear & particles physics, Gravitational wave, General relativity, Astrophysics::High Energy Astrophysical Phenomena, Graviton, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Metric expansion of space, Massless particle, Quantization (physics), Space and Planetary Science, De Sitter universe, Quantum electrodynamics, 0103 physical sciences, 010303 astronomy & astrophysics, Luminosity distance
Abstract: Detections of gravitational wave (GW) stimulate the discussion of how GWs propagate in the expanding Universe. General relativity predicts that GWs are massless and propagate at the speed of light with no extra friction term, which relates to the attenuation of GWs, while some modified gravities may predict a different behavior. The mass and speed terms can be tightly constrained by the GW150914-like and GW170817/GRB 170817A events, respectively. However, the friction term remaining unconstrained. In this paper, we quantize the nonstandard propagating gravitational waves with nonzero friction term in the cosmological background, and study the influence of the friction term on the GW luminosity distance in quantum level, and the initial conditions of perturbations given by inflation. We find the quantum nature of the difference between GW and electromagnetic luminosity distance is graviton particle number non-conservation. For the initial conditions, we obtain an analytical expression of the power spectrum with nonzero friction term for the de Sitter background. In observations, both the GW luminosity distance and primordial GWs can be used to constrain the friction term., Comment: 15 pages in the preprint format, accepted for publication in Phys. Dark Universe
Published: 2019
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48. Multiple Measurements of Quasars Acting as Standard Probes: Exploring the Cosmic Distance Duality Relation at Higher Redshift

Author: Marek Biesiada, Tonghua Liu, Shuo Cao, Xiaogang Zheng, Zong-Hong Zhu, and Kai Liao
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMIC cancer database, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Duality relation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: General relativity reproduces main current cosmological observations, assuming the validity of cosmic distance duality relation (CDDR) at all scales and epochs. However, CDDR is poorly tested in the redshift interval between the farthest observed Type Ia supernovae (SN Ia) and that of the Cosmic Microwave background (CMB). We present a new idea of testing the validity of CDDR, through the multiple measurements of high-redshift quasars. Luminosity distances are derived from the relation between the UV and X-ray luminosities of quasars, while angular diameter distances are obtained from the compact structure in radio quasars. This will create a valuable opportunity where two different cosmological distances from the same kind of objects at high redshifts are compared. Our constraints are more stringent than other currently available results based on different observational data and show no evidence for the deviation from CDDR at $z\sim 3$. Such accurate model-independent test of fundamental cosmological principles can become a milestone in precision cosmology., 8 pages, 6 figures, 1 table, Accepted for publication in ApJ
Published: 2020
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49. Model-independent Constraints on Lorentz Invariance Violation: Implication from Updated Gamma-Ray Burst Observations

Author: Shuaibo Geng, Jingzhao Qi, Yujie Lian, Yuting Liu, Shuo Cao, Zong-Hong Zhu, Yu Pan, and Tonghua Liu
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, Planck energy, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Energy–momentum relation, Astrophysics, Lorentz covariance, 01 natural sciences, Redshift, symbols.namesake, Space and Planetary Science, Dispersion relation, 0103 physical sciences, symbols, Quantum gravity, Gamma-ray burst, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, 0105 earth and related environmental sciences
Abstract: Astrophysical observations provide a unique opportunity to test possible signatures of Lorentz Invariance Violation (LIV), due to the high energies and long distances involved. In quantum theory of gravity, one may expect the modification of the dispersion relation between energy and momentum for photons, which can be probed with the time-lag (the arrival time delay between light curves in different energy bands) of Gamma-ray bursts (GRBs). In this paper, by using the detailed time-delay measurements of GRB 160625B at different energy bands, as well as 23 time-delay GRBs covering the redshifts range of $z=0.168-2.5$ (which were measured at different energy channels from the light curves), we propose an improved model-independent method (based on the newly-compiled sample of $H(z)$ measurements) to probe the energy-dependent velocity due to the modified dispersion relation for photons. In the framework of a more complex and reasonable theoretical expression to describe the time delays, our results imply that the intrinsic time lags can be better described with more GRBs time delay data. More importantly, through direct fitting of the time-delay measurements of a sample of GRBs, our limit on the LIV energy scale is comparable to that with unknown constant for the intrinsic time lag, much lower than the Planck energy scale in both linear LIV and quadratic LIV cases., 7pages,3figures,Accepted for publication in ApJ
Published: 2020
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50. Cosmological investigation of multi-frequency VLBI observations of ultra-compact structure in $$z\sim 3$$ z ∼ 3 radio quasars

Author: Xiaogang Zheng, Xuan Ji, Shuo Cao, Marek Biesiada, Zong-Hong Zhu, Yu Pan, Jingzhao Qi, and Tengpeng Xu
Subjects: Physics, Physics and Astronomy (miscellaneous), Opacity, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Lambda, 01 natural sciences, Redshift, Cosmology, Angular diameter, 0103 physical sciences, Very-long-baseline interferometry, Angular resolution, 010303 astronomy & astrophysics, Engineering (miscellaneous)
Abstract: In this paper, we use multi-frequency angular size measurements of 58 intermediate-luminosity quasars reaching the redshifts $$z\sim 3$$ and demonstrate that they can be used as standard rulers for cosmological inference. Our results indicate that, for the majority of radio-sources in our sample their angular sizes are inversely proportional to the observing frequency. From the physical point of view it means that opacity of the jet is governed by pure synchrotron self-absorption, i.e. external absorption does not play any significant role in the observed angular sizes at least up to 43 GHz. Therefore, we use the value of the intrinsic metric size of compact milliarcsecond radio quasars derived in a cosmology independent manner from survey conducted at 2 GHz and rescale it properly according to predictions of the conical jet model. This approach turns out to work well and produce quite stringent constraints on the matter density parameter $$\Omega _m$$ in the flat $$\Lambda $$ CDM model and Dvali–Gabadadze–Porrati braneworld model. The results presented in this paper pave the way for the follow up engaging multi-frequency VLBI observations of more compact radio quasars with higher sensitivity and angular resolution.
Published: 2018
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