| dc.description.abstract | The observation of Gravitational Waves(GW) is one of the most exciting dis- coveries of this century. Since 1974, Hulse and Taylor discovered the binary star system emits energies, people realized the prediction of GW from general rela- tivity is possible. In 2015, an advanced Laser Interferometer Gravitational wave Observatory called aLIGO succeed in directly detecting the GW signals from a binary black hole merger. During this decade, with advanced Virgo and KA- GRA’s joining, the sensitivity dramatically increases, and the events discovered increased from that binary black hole system to 90 events in the latest catalog. The observation of GW is detecting the displacement of test masses in the km- scale observatory, with the most frontier technologies applied, the requirements of detecting the GW strain is can be satisfied. As the GW becomes one of the important cosmological resources, the accuracy of the sources is required to reach with other astronomy research. This is why the calibration of the response of the interferometer is crucial, the error estimation of calibration is a crucial part of the parameter estimation of the GW source.
KAGRA, the third km-scale GW observatory located in Japan, Gifu, joined the observation network in April 2020 and features two unique technologies - underground and cryogenic. KAGRA is the first observatory built on the under- ground site, in order to reduce the seismic noise, and the cryogenic system is to reduce the thermal noise.
In this thesis, we discuss the error estimation analysis based on the simu- lated frequency domain calibration data of KAGRA during the period O3GK in April 2020. We develop a calibration pipeline based on the maximum likelihood method to crosscheck with the previous pipeline based on the Bayesian method. The maximum likelihood method provides a faster pipeline for crosscheck in the ratio around. By crosscheck between these two method, and the results proves that these two are consistence, so that we can improve the accuracy of GW observation with more reliable parameters and faster pipeline. | en_US |