Core Noise Requirements, and GW Sensitivities of AMIGO

Abstract

AMIGO - The Astrodynamical Middle-frequency Interferometric GW (Gravitation-Wave) Observatory is a first-generation mid-frequency GW mission bridging the sensitivity gap between the high-frequency GW detectors and low-frequency space GW detectors. In our previous works, we have obtained appropriate heliocentric orbit formations of nominal arm length 10,000 km with their first-generation time-delay configurations satisfying frequency noise reduction requirement, and we have also worked out thrust-fuel friendly constant-arm heliocentric orbit formations. In this paper, we review and study noise requirements and present the corresponding GW sensitivities. From the design white position noises and acceleration noises, we obtain the GW sensitivities for the first-generation Michelson X TDI configuration of b-AMIGO (baseline AMIGO), AMIGO, and e-AMIGO (enhanced AMIGO). In view of the current technology development, we study and indicate steps to implement the AMIGO mission concept.

arXiv commentrevision to match the IJMPD in-press version

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Cited by in corpus (3)

• Multiband gravitational wave observations of stellar binary black holes at the low to middle and high frequencies
• Probing Supermassive Black Hole Binaries with Orbital Resonances of Laser-Ranged Satellite
• Arm-Locking Frequency Noise Suppression for Astronomical Middle-Frequency Interferometric Gravitational Wave Observatory