Speaker
Description
One of the limiting factors for gravitational wave detection sensitivity to date is the coating thermal noise in the lower audio-band. The use of cryogenically cooled crystalline silicon in combination with high-quality silicon-based coatings for the test mass mirrors will allow tackling the thermal noise problem. In the gravitational wave interferometry, moving the laser wavelengths to 2 µm will enable this approach. Therefore, despite the fact that the Einstein Telescope's low-frequency (ET-LF) wavelength is specified as 1550 nm and the high-frequency (ET-HF) one as 1064 nm at room temperature, the Gravitational Wave International Committee recommended the research and development of squeezing sources at a 2 µm wavelength as an alternative wavelength. Here, we present possible approaches for the development of the squeezed light sources for ET at various wavelengths.
