Speaker
Description
Third-generation ground-based gravitational-wave detectors promise a transformative leap in sensitivity, unlocking the ability to detect signals from the Universe's earliest epochs. Meeting these ambitious goals requires overcoming numerous noise sources, both technical and fundamental, with laser frequency noise emerging as a critical challenge. Suppression of this noise must go far beyond the achievements of second-generation detectors, demanding a rethinking of stabilization strategies.
In current interferometers, frequency noise suppression relies on a combination of a suspended Input Mode Cleaner (IMC) cavity, a rigid Reference Cavity to manage low Fourier-frequency noise during lock acquisition of kilometer-scale arm cavities, and feedback from the common-arm degree of freedom of the Interferometer. However, in third-generation detectors, the much lower cavity pole of the arm cavities renders the common-arm reference impractical, necessitating a fundamental rethinking of the frequency stabilization strategy.
The next-generation IMC must assume a far more demanding role of frequency reference over an extended bandwidth, requiring exceptional stability across the entire control-loop bandwidth. This shift introduces big challenges, including stricter requirements for seismic isolation, suppression of thermal and radiation pressure noise on the cavity mirrors, and mitigation of thermal coating effects. Furthermore, achieving the requisite signal-to-noise ratio for precise frequency noise sensing calls for innovative approaches in sensing and feedback control design.
Aim of the talk is to present these new problems and the state of the art preliminary solutions devised by the community.
Details
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| Internet talk | Yes |
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| Is this an abstract from experimental collaboration? | No |
| Name of experiment and experimental site | N/A |
| Is the speaker for that presentation defined? | Yes |