Numerical simulation of time delay interferometry for TAIJI and new LISA

Wang, Gang; Ni, Wei-Tou

doi:10.1088/1674-4527/19/4/58

Cited by 34 publications

(29 citation statements)

References 62 publications

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“…11) (Table 5) Table 5. Comparison of the resulting path length differences for the first-generation TDI's listed in [24]…”

Section: Numerical Results Of the First-generation Tdi For Amigo-s-8-mentioning

confidence: 99%

“…One needs to match the two optical paths using Time Delay Interferometry (TDI) to lessen the stability requirement. For TDI configurations and their numerical simulations for various missions, see Tinto and Dhurandhar [23], Wang and Ni [24] and references therein. Experimental demonstration of TDI in laboratory for LISA is worked out in 2010-2012 (Vine et al [25], Mirtyk et al [26]).…”

Section: Sensitivitymentioning

confidence: 99%

“…In this section, we calculate the difference between the two path lengths for TDI configurations and plot the difference as function of the signal arriving epoch of TDI in the first-generation TDI configurations ---Michelson X, Y & Z; Sagnac α, β & γ; Relay U, V & W; Beacon P, Q & R; Monitor E, F & G for various orbit choices of section 3 for AMIGO-S, AMIGO-E1, and AMIGO-EM. We use the iteration and interpolation methods to calculate the time in the barycentric coordinate system as in our early papers [24]. We do this for AMIGO-S-8-12deg in section 4.1, for AMIGO-S-2-6deg in section 4.2, for AMIGO-S-2-4deg in section 4.3, for AMIGO-E1 in section 4.4, and for AMIGO-EM-L4 in section 4.5.…”

Section: Time Delay Interferometrymentioning

confidence: 99%

“…where a Newton and a 1PN are the Newtonian and first-order post-Newtonian acceleration from the major celestial bodies in the solar system considered as point mass, a fig is the acceleration due to the figure effects from the Sun, Earth and Moon, and a asteroid is the acceleration from Newtonian perturbation of the 340 asteroids. The explicit interactions in our CGC ephemeris framework are fully described in references [24,36,37]. The thruster needs to provide acceleration a thruster a thruster = a traj  a traj (10) to maintain the constant arm length trajectories.…”

Section: Thruster Accelerationmentioning

confidence: 99%

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Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Wang

2020

Int. J. Mod. Phys. D

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AMIGO is a first-generation Astrodynamical Middle-frequency Interferometric GW Observatory. The scientific goals of AMIGO are: to bridge the spectra gap between first-generation high-frequency and low-frequency GW sensitivities; to detect intermediate mass BH coalescence; to detect inspiral phase and predict time of binary black hole coalescence together with neutron star coalescence for ground interferometers; to detect compact binary inspirals for studying stellar evolution and galactic population. The mission concept is to use time delay interferometry for a nearly triangular formation of 3 drag-free spacecraft with nominal arm length 10,000 km, emitting laser power 2-10 W and telescope diameter 300-360 mm. The design GW sensitivity in the middle frequency band is 3 × 10 −21 Hz -1 . Four options of orbits are under study: (i) Earth-like solar orbits (2-20 degrees behind the Earth); (ii) 600,000 km high orbit formation around the Earth; (iii) 50,000 km-250,000 high orbit formation around the Earth; (iv) near Earth-Moon L4 (or L5) halo orbit formation. All four options have LISAlike formations, that is the triangular formation is 60º inclined to the orbit plane. For AMIGO, the first-generation time delay interferometry is good enough for the laser frequency noise suppression. We also investigate for each options of orbits under study, whether constant equal-arm implementation is feasible. For the solar-orbit option, the acceleration to maintain the formation can be designed to be less than 15 nm/s 2 with the thruster requirement in the 15 μN range. AMIGO would be a good place to implement the constant equal-arm option. Fuel requirement, thruster noise requirement and test mass acceleration actuation requirement are briefly considered. From the orbit study, the solar orbit option is the first mission orbit choice. We study the deployment for this orbit option. A last-stage launch from 300 km LEO (Low Earth Orbit) to an appropriate 2-degree-behindthe-Earth AMIGO formation in 95 days requires only a v of 75 m/s.

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“…11) (Table 5) Table 5. Comparison of the resulting path length differences for the first-generation TDI's listed in [24]…”

Section: Numerical Results Of the First-generation Tdi For Amigo-s-8-mentioning

confidence: 99%

Section: Sensitivitymentioning

confidence: 99%

Section: Time Delay Interferometrymentioning

confidence: 99%

Section: Thruster Accelerationmentioning

confidence: 99%

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Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Wang

2020

Int. J. Mod. Phys. D

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“…Some other studies about Taiji have also been conducted in Refs. [36][37][38]. Nevertheless, the forecast for the capability of Taiji in the future cosmological parameter estimation has never been seriously studied.…”

Section: Introductionmentioning

confidence: 99%

Prospects for improving cosmological parameter estimation with gravitational-wave standard sirens from Taiji

et al. 2020

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Taiji, a space-based gravitational-wave detector, consists of three satellites forming an equilateral triangle with arm length of 3 × 10 6 km, orbiting around the Sun. Taiji is able to observe standard siren events of massive black hole binary (MBHB) merger, which is helpful to probe the expansion of the universe. In this paper, we preliminarily forecast the capability of Taiji for improving cosmological parameter estimation with the gravitational-wave standard siren data. We simulate five-year standard siren data based on three fiducial cosmological models and three MBHB growth and formation models. It is found that the standard siren data from Taiji can effectively break the cosmological parameter degeneracies generated by the cosmic microwave background (CMB) anisotropies data, especially for dynamical dark energy models. The constraints on cosmological parameters are significantly improved by the data combination CMB+Taiji, compared to the CMB data alone. Compared to the current optical cosmological observations, Taiji can still provide help in improving the cosmological parameter estimation to some extent. In addition, we consider an ideal scenario to investigate the potential of Taiji on constraining cosmological parameters. We conclude that the standard sirens of MBHB from Taiji will become a powerful cosmological probe in the future.

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Numerical Simulations of Arm-locking for Taiji Space Gravitational Waves Detection

Liu

Jin

2021

Microgravity Sci. Technol.

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Numerical simulation of time delay interferometry for TAIJI and new LISA

Cited by 34 publications

References 62 publications

Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Prospects for improving cosmological parameter estimation with gravitational-wave standard sirens from Taiji

Numerical Simulations of Arm-locking for Taiji Space Gravitational Waves Detection

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