DECIGO: The Japanese space gravitational wave antenna

Sato, S.; Kawamura, Seiji; Ando, Masaki; Nakamura, Takashi; Tsubono, K.; Araya, Akito; Funaki, Ikkoh; Ioka, Kunihito; Kanda, Nobuyuki; Moriwaki, Shigenori; Musha, Mitsuru; Nakazawa, K.; Numata, Kenji; Sakai, Shin‐ichiro; Seto, Naoki; Takashima, Takeshi; Tanaka, Takahiro; Agatsuma, K.; Aoyanagi, Koh-suke; Arai, K.; Asada, Hideki; Aso, Y.; Chiba, Takeshi; Ebisuzaki, Toshikazu; Ejiri, Yumiko; Enoki, Motohiro; Eriguchi, Yoshiharu; Fujimoto, Masa–Katsu; Fujita, Ryuichi; Fukushima, Mitsuhiro; Futamase, Toshifumi; Ganzu, Katsuhiko; Harada, Tomohiro; Hashimoto, Tatsuaki; Hayama, K.; Hikida, Wataru; Himemoto, Y.; Hirabayashi, H.; Hiramatsu, Takashi; Hong, Feng−Lei; Horisawa, Hideyuki; Hosokawa, Mizuhiko; Ichiki, Kiyotomo; Ikegami, Takayasu; Inoue, Kaiki Taro; Ishidoshiro, K.; Ishihara, Hideki; Ishikawa, Takehiko; Ishizaki, Hideharu; Ito, Hiroyuki; Itoh, Y.; Kawashima, Nobuki; Kawazoe, F.; Kishimoto, Naoki; Kiuchi, Kenta; Kobayashi, S.; Kohri, Kazunori; Koizumi, Hiroyuki; Kojima, Yasufumi; Kokeyama, K.; Kokuyama, Wataru; Kotake, Kei; Kozai, Yoshihide; Kudoh, Hideaki; Kunimori, Hiroo; Kuninaka, Hitoshi; Kuroda, K.; Maeda, Keiichi; Matsuhara, Hideo; Mino, Yasushi; Miyakawa, O.; Miyoki, S.; Morimoto, Mutsuko Y.; Morioka, T.; Morisawa, Toshiyuki; Mukohyama, Shinji; Nagano, S.; Naito, Isao; Nakamura, Kouji; Nakano, Hiroyuki; Nakao, Ken–ichi; Nakasuka, Shinichi; Nakayama, Yoshinori; Nishida, E.; Nishiyama, Kazutaka; Nishizawa, A.; Niwa, Yasumasa; Noumi, Taiga; Obuchi, Yasunari; Ohashi, M.; Ohishi, N.; Ohkawa, Masashi; Okada, Norio; Onozato, Kouji; Oohara, Ken–ichi; Sago, Norichika; Saijo, Motoyuki; Sakagami, Masa–aki; Sakata, S.; Sasaki, Misao; Satō, Takashi; Shibata, Masaru; Shinkai, H.; Somiya, K.; Sotani, Hajime; Sugiyama, Naoshi; Suwa, Yudai; Suzuki, Riéko; Tagoshi, Hideyuki; Takahashi, Fuminobu; Takahashi, Keitaro; Takahashi, Ryutaro; Takahashi, Ryuichi; Takahashi, Tadayuki; Takahashi, Hideya; Takamori, A.; Takano, Tadashi; Taniguchi, Keisuke; Taruya, Atsushi; Tashiro, Hiroyuki; Torii, Yasuo; Toyoshima, Morio; Tsujikawa, Shinji; Tsunesada, Y.; Ueda, Akitoshi; Ueda, Ken–ichi; Utashima, Masayoshi; Wakabayashi, Yaka; Yamakawa, Hiroshi; Yamamoto, K.; Yamazaki, Toshitaka; Yokoyama, Jun′ichi; Yoo, Chul-Moon; Yoshida, Shijun; Yoshino, T.

doi:10.1088/1742-6596/154/1/012040

Cited by 39 publications

(26 citation statements)

References 10 publications

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“…Most of the laser power entering the interferometer is scattered into the surrounding vacuum system. For all of the interferometers, the measured optical losses were significantly higher than expected from the initial, tabletop measurements (Sato et al, 1999). A small fraction of the losses came from absorption in the mirror substrate and on the high-reflectivity dielectric mirror coatings within the FabryPérot arms (in the case of LIGO, Virgo, and TAMA) (Hild et al, 2006;Brooks et al, 2009).…”

Section: A Excess Optical Lossmentioning

confidence: 76%

Gravitational radiation detection with laser interferometry

2014

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Gravitational-wave detection has been pursued relentlessly for over 40 years. With the imminent operation of a new generation of laser interferometers, it is expected that detections will become a common occurrence. The research into more ambitious detectors promises to allow the field to move beyond detection and into the realm of precision science using gravitational radiation. In this article, the state of art for the detectors is reviewed and an outlook for the coming decades is described.

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Section: A Excess Optical Lossmentioning

confidence: 76%

Gravitational radiation detection with laser interferometry

2014

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“…We defer more thorough study of possible detection by currently planned GW detectors (advanced LIGO, NGO, DECIGO, etc. ), but do note that these signal amplitudes are weak (advanced LIGO [46] and probable modes of operation of DECIGO [47,48] offer strain sensitivities of ∼ 10 −24 − 10 −23 ). Thus, the exact parameters of the jet, as well as the jet's internal structure model, might affect the possibility of detection.…”

Section: B Resultsmentioning

confidence: 99%

Gravitational wave memory from gamma ray bursts’ jets

Birnholtz

Piran

2013

Phys. Rev. D

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While the possible roles of GRBs' progenitors as Gravitational Waves (GW) sources have been extensively studied, little attention has been given to the GRB jet itself as a GW source. We expect the acceleration of the jet to produce a Gravitational Wave Memory signal. While all relativistic jet models display anti-beaming of GW radiation away from the jet axis, thus radiating away from directions of GRBs' γ radiation, this effect is not overwhelming. The decrease of the signal amplitude towards the cone of γ-ray detectability is weak, and for some models and parameters the GW signal reaches a significant amplitude for much of the γ-ray cone. Thus both signals may be jointly detected. We find different waveforms and Fourier signatures for uniform jets and structured jet models -thus offering a method of using GW signatures to probe the internal structure and acceleration of GRB jets. The GW signal peaks just outside the jet (core) of a uniform (structuted) jet. Within the jet (core) the GW signal displays wiggles, due to a polarization effect; thus for a uniform jet, the peak amplitude accompanies a smoother signal than the peak of a structured jet. For the most probable detection angle and for typical GRB parameters, we expect frequencies 600Hz and amplitudes h ∼ 10 −25 . Our estimates of the expected signals suggest that the signals are not strong enough for a single cluster of DECIGO nor for aLIGO's sensitivities. However, sensitivies of ∼ 10 −25 / √ Hz in the DECIGO band should suffice to detect typical long GRBs at 2Gpc and short GRBs at 200M pc, implying a monthly event of a long GRB and a detection of a short GRB every decade. In addition, we expect much more frequent detection of GW from GRBs directed away from us, including orphan afterglows. The ultimate DECIGO sensitivy should increase the range and enable detecting these signals in all models even to high cosmological z.

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“…This is the first time that we are able to study the Universe with both vision and hearing. This multi-messenger observations of both gravitational wave (GW) and their electromagnetic (EM) counterparts allow us to use gravitational wave (GW) as standard sirens [3]: the intrinsic total gravitational luminosity can be derived to unprecedented precision from the precise way in which GW evolves, given the much higher sensitivity of the future ground-and space-based GW experiments such as the Einstein Telescope (ET) [4], 40-km LIGO [5], eLISA [6], and DECIGO [7]; then coupled to the measured absolute strain amplitude of GW, the luminosity distance D cos to the source can be accurately determined as well; finally, from the EM counterpart, a unique host galaxy can be identified, which makes it possible to obtain a spectroscopic redshift follow-up z obs . As such, GW provides a new technique to measure the Hubble constant from nearby galaxies (redshift z 1)…”

Section: Introductionmentioning

confidence: 99%

Accurate method to determine the systematics due to the peculiar velocities of galaxies in measuring the Hubble constant from gravitational-wave standard sirens

2019

Phys. Rev. D

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We propose a novel approach to accurately pin down the systematics due to the peculiar velocities of galaxies in measuring the Hubble constant from nearby galaxies in current and future gravitational-wave (GW) standardsiren experiments. Given the precision that future GW standard-siren experiments aim to achieve, the peculiar velocities of nearby galaxies will be a major source of uncertainty. Unlike the conventional backward reconstruction that requires additional redshift-independent distance indicators to recover the peculiar velocity field, we forwardly model the peculiar velocity field by using a high-fidelity mock galaxy catalog built from highresolution dark matter only (DMO) N-body simulations with a physically motivated subhalo abundance matching (SHAM) technique without introducing any free parameters. Our mock galaxy catalog can impressively well reproduce the observed spectroscopic redshift space distortions (RSDs) in highly non-linear regimes down to very small scales, which is a robust test of the velocity field of our mock galaxy catalog. Based on this mock galaxy catalog, we accurately, for the first time, derive the peculiar velocity probability distributions for the SDSS main galaxy samples. We find that the systematics induced by the peculiar velocities of SDSS like galaxies on the measured Hubble constant can be reduced to below 1%(1σ) for GW host galaxies with a Hubble flow redshift just above 0.13, a distance that can be well probed by future GW experiments and galaxy surveys.

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DECIGO: The Japanese space gravitational wave antenna

Cited by 39 publications

References 10 publications

Gravitational radiation detection with laser interferometry

Gravitational radiation detection with laser interferometry

Gravitational wave memory from gamma ray bursts’ jets

Accurate method to determine the systematics due to the peculiar velocities of galaxies in measuring the Hubble constant from gravitational-wave standard sirens

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