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The DECi hertz Interferometer Gravitational-Wave Observatory (DECIGO) is aspace gravitational wave (GW) detector. DECIGO was originally designed to besensitive enough to observe primordial GW background (PGW). However, due to thelowered upper limit of the PGW by the Planck observation, further improvementof the target sensitivity of DECIGO is required. In the previous studies,DECIGO's parameters were optimized to maximize the signal-to-noise ratio (SNR)of the PGW to quantum noise including the effect of diffraction loss. Tosimulate the SNR more realistically, we optimize DECIGO's parametersconsidering the GWs from double white dwarfs (DWDs) and the thermal noise oftest masses. We consider two cases of the cutoff frequency of GWs from DWDs. Inaddition, we consider two kinds of thermal noise: thermal noise in a residualgas and internal thermal noise. To investigate how the mirror geometry affectsthe sensitivity, we calculate it by changing the mirror mass, keeping themirror thickness, and vice versa. As a result, we obtained the optimums for theparameters that maximize the SNR that depends on the mirror radius. This resultshows that a thick mirror with a large radius gives a good SNR and enables usto optimize the design of DECIGO based on the feasibility study of the mirrorsize in the future.

Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental Noises