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The sensitivity of next-generation gravitational-wave detectors such asAdvanced LIGO and LCGT should be limited mostly by quantum noise with anexpected technical progress to reduce seismic noise and thermal noise. Thosedetectors will employ the optical configuration of resonant-sideband-extractionthat can be realized with a signal-recycling mirror added to the Fabry-PerotMichelson interferometer. While this configuration can reduce quantum noise ofthe detector, it can possibly increase laser frequency noise and intensitynoise. The analysis of laser noise in the interferometer with the conventionalconfiguration has been done in several papers, and we shall extend the analysisto the resonant-sideband-extraction configuration with the radiation pressureeffect included. We shall also refer to laser noise in the case we employ theso-called DC readout scheme.Comment: An error in Fig. 10 in the published version in PRD has been  corrected in this version; an erratum has been submitted to PRD. After  correction, this figure reflects a significant difference in the ways RF and  DC readout schemes are susceptible to laser noise. In addition, the levels of  mirror loss imbalances and input laser amplitude noise have also been updated  to be more realistic for Advanced LIG

Frequency noise and intensity noise of next-generation gravitational-wave detectors with RF/DC readout schemes