Current status of space gravitational wave antenna DECIGO and B-DECIGO

Kawamura, Seiji; Ando, Masaki; Seto, Naoki; Sato, S.; Musha, Mitsuru; Kawano, Isao; Yokoyama, Jun′ichi; Tanaka, Takahiro; Ioka, Kunihito; Akutsu, T.; Takashima, Takeshi; Agatsuma, K.; Araya, Akito; Aritomi, N.; Asada, Hideki; Chiba, Takeshi; Eguchi, S.; Enoki, Motohiro; Fujimoto, Masa–Katsu; Fujita, Ryuichi; Futamase, Toshifumi; Harada, Tomohiro; Hayama, K.; Himemoto, Y.; Hiramatsu, Takashi; Hong, Fei; Hosokawa, Mizuhiko; Ichiki, Kiyotomo; Ikari, Satoshi; Ishihara, Hideki; Ishikawa, Tomohiro; Itoh, Y.; Ito, Takahiro; Iwaguchi, Shoki; Izumi, K.; Kanda, Nobuyuki; Kanemura, Shinya; Kawazoe, F.; Kobayashi, S.; Kohri, Kazunori; Kojima, Yasufumi; Kokeyama, K.; Kotake, Kei; Kuroyanagi, Sachiko; Maeda, Keiichi; Matsushita, Sachiko; Michimura, Yuta; Morimoto, Takeshi; Mukohyama, Shinji; Nagano, Koji; Nagano, S.; Naito, T.; Nakamura, Kouji; Nakamura, Takashi; Nakano, Hiroyuki; Nakao, Ken–ichi; Nakasuka, Shinichi; Nakayama, Yoshinori; Nakazawa, K.; Nishizawa, A.; Ohkawa, Masashi; Oohara, Ken–ichi; Sago, Norichika; Saijo, Motoyuki; Sakagami, Masa–aki; Sakai, Shin‐ichiro; Satō, Takashi; Shibata, Masaru; Shinkai, Hisa-aki; Shoda, A.; Somiya, K.; Sotani, Hajime; Takahashi, Ryutaro; Takahashi, Hideya; Takamori, A.; Taniguchi, Keisuke; Taruya, Atsushi; Tsubono, K.; Tsujikawa, Shinji; Ueda, Akitoshi; Ueda, Ken–ichi; Watanabe, Izumi; Yagi, Kent; Yamada, Rika; Yokoyama, Shuichiro; Yoo, Chul-Moon; Zhu, Zong-Hong

doi:10.48550/arxiv.2006.13545

Cited by 100 publications

(137 citation statements)

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“…The last in conjunction with the following decades from an astronomical point of view belong to the gravitational wave astronomy branch of physics. Indeed, the LIGO-Virgo collaboration have already established the new branch of physics [1][2][3][4][5][6], the gravitational wave astronomy branch, and with the upcoming LISA [7,8] and future space missions BBO [9,10] and DECIGO [11,12], it is expected that our perception regarding the early Universe and astrophysical phenomena will be further enlightened. Already, the GW170817 event [3] followed by a kilonova Gamma Ray Burst [4,5] which arrived almost simultaneously with the gravitational waves, have formed and changed our perception about modified gravity theories since many models which generate tensor perturbations with propagation speed different from that of light's in the vacuum, are excluded from being phenomenologically viable theories [13][14][15][16].…”

Section: Introductionmentioning

confidence: 99%

A Refined Einstein-Gauss-Bonnet Inflationary Theoretical Framework

Oikonomou

2021

Preprint

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We provide a refined and much more simplified Einstein-Gauss-Bonnet inflationary theoretical framework, which is compatible with the GW170817 observational constraints on the gravitational wave speed. As in previous works, the constraint that the gravitational wave speed is c 2 T = 1 in natural units, results to a constraint differential equation that relates the coupling function of the scalar field to the Gauss-Bonnet invariant ξ(φ) and the scalar potential V (φ). Adopting the slow-roll conditions for the scalar field and the Hubble rate, and in contrast to previous works, by further assuming that κ ξ ξ 1, which is motivated by slow-roll arguments, we succeed in providing much more simpler expressions for the slow-roll indices and for the tensor and scalar spectral indices and for the tensor-to-scalar ratio. We exemplify our refined theoretical framework by using an illustrative example with a simple power-law scalar coupling function ξ(φ) ∼ φ ν and as we demonstrate the resulting inflationary phenomenology is compatible with the latest Planck data. Moreover, this particular model produces a blue-tilted tensor spectral index, so we discuss in brief the perspective of describing the NANOGrav result with this model as is indicated in the recent literature.

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Section: Introductionmentioning

confidence: 99%

A Refined Einstein-Gauss-Bonnet Inflationary Theoretical Framework

Oikonomou

2021

Preprint

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“…T HE astounding detection of a binary black hole merger in 2015 by advanced LIGO and Virgo [2] has set the stage for the more than 50 subsequent gravitational wave (GW) events from both binary black holes and binary neutron stars which have been detected since [3,4]. With planned groundbased detectors across the globe such as KAGRA [5], LIGO-India [6], the Einstein Telescope [7], Cosmic Explorer [8], and space-based detectors such as LISA [9] and DECIGO [10], the future of gravitational wave physics promises unprecedented precision at a wide range of frequencies. In addition, Pulsar Timing Arrays (PTAs) are starting to reach the sensitivity to detect a possible background of gravitational waves [11].…”

Section: Jan Morrismentioning

confidence: 99%

Polarization distortions of lensed gravitational waves

Dalang,

Cusin,

Lagos

2021

Preprint

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In general relativity (GR), gravitational waves (GWs) propagate the well-known plus and cross polarization modes which are the signature of a massless spin-2 field. However, diffraction of GWs caused by intervening objects along the line of sight can cause the apparent rise of additional polarizations due to GW-curvature interactions. In this paper, we continue the analysis of [1] on lensing of gravitational waves beyond geometric optics. In particular, we calculate the lensing effect caused by a point-like lens, in the regime where its Schwarzschild radius R s is much smaller than the wavelength λ of the signal, itself smaller than the impact parameter b. In this case, the curvature of spacetime induces distortions in the polarization of the wave such that effective scalar and vector polarizations may appear. We find that the amplitude of these apparent non-GR polarizations is suppressed by a factor R s λ /b 2 with respect to the amplitude of the GR-like tensor modes. We estimate the probability to develop these extra polarization modes for a nearly monochromatic GW in the Pulsar Timing Arrays band traveling through a distribution of galaxies.

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“…IMRIs are likely to exist in dense globular clusters and galactic nuclei [40,41] and are one of the prime sources for future-generation detectors [42,43]. In particular, IMRIs with total mass < 2000M may be detectable with the current generation of detectors [44] with higher mass binaries detectable by future space-based missions such as LISA [45] and beyond [46,47].…”

Section: Introductionmentioning

confidence: 99%

Survey of gravitational wave memory in intermediate mass ratio binaries

Islam¹,

Field²,

Khanna³

et al. 2021

Preprint

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The non-linear gravitational wave (GW) memory effect is a distinct prediction in general relativity. While the effect has been well studied for comparable mass binaries, it has mostly been overlooked for intermediate mass ratio inspirals (IMRIs). We offer a comprehensive analysis of the phenomenology and detectability of memory effects, including contributions from subdominant harmonic modes, in heavy IMRIs consisting of a stellar mass black hole and an intermediate mass black hole. When formed through hierarchical mergers, for example when a GW190521-like remnant captures a stellar mass black hole, IMRI systems have a large total mass, large spin on the primary, and possibly residual eccentricity; features that potentially raise the prospect for memory detection. We compute both the displacement and spin non-linear GW memory from the m = 0 gravitational waveforms computed within a black hole perturbation theory framework that is partially calibrated to numerical relativity waveforms. We probe the dependence of memory effects on mass ratio, spin, and eccentricity and consider the detectability of a memory signal from IMRIs using current and future GW detectors. We find that (i) while eccentricity introduces additional features in both displacement and spin memory, it does not appreciatively change the prospects of detectability, (ii) including higher modes into the memory computation can increase singal-to-noise (SNR) values by about 7% in some cases, (iii) the SNR from displacement memory dramatically increases as the spin approaches large, positive values, (iv) spin memory from heavy IMRIs would, however, be difficult to detect with future generation detectors even from highly spinning systems. Our results suggest that hierarchical binary black hole mergers may be a promising source for detecting memory and could favorably impact memory forecasts.

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Current status of space gravitational wave antenna DECIGO and B-DECIGO

Cited by 100 publications

References 0 publications

A Refined Einstein-Gauss-Bonnet Inflationary Theoretical Framework

A Refined Einstein-Gauss-Bonnet Inflationary Theoretical Framework

Polarization distortions of lensed gravitational waves

Survey of gravitational wave memory in intermediate mass ratio binaries

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