Core Noise Requirements, and GW Sensitivities of AMIGO

TL;DR

This paper reviews the noise requirements and GW sensitivities of the AMIGO mission, a mid-frequency gravitational wave observatory, and discusses steps for its technological implementation.

Contribution

It provides an analysis of noise requirements and sensitivities for AMIGO's different configurations, advancing mid-frequency GW detection technology.

Findings

GW sensitivities for different AMIGO configurations derived

Noise requirements linked to design white and acceleration noises

Implementation steps for AMIGO mission outlined

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.