Speaker
Description
The sensitivity of gravitational wave (GW) interferometers is ultimately limited by
the quantum noise, which is due to vacuum fluctuations of the optical fields that entering from the dark port of the detector. Quantum noise affects the interferometer sensitivity in the entire bandwidth and it has two complementary effects: the shot noise, which depends on phase fluctuations of the optical field, dominates at high frequencies and decreases with laser power; radiation pressure noise, which depends on amplitude fluctuation of the optical field, perturbing the position of suspended mirrors at low frequencies and increases with laser power.
One way to improve the sensitivity of GW detectors is to inject squeezed vacuum into the dark port and a frequency-dependent-squeezing (FDS) generation is needed to achieve a broadband quantum noise reduction (for the next observation run). In AdV+ interferometer (the ongoing upgrade of Advanced Virgo) a 300 m long filter cavity was installed to produce FDS. The observable squeezing level can be reduced by the misalignments in the detection of squeezed light. Optimizing the alignments is fundamental and in this poster I will show the development of the automatic alignment loop in the AdV+ squeezing system using dither lines techniques.
Details
Barbara Garaventa, PhD student and research fellow, University of Genoa/INFN Genoa. (on behalf of AdV+ Quantum Noise Virgo team)
| Is this abstract from experiment? | Yes |
|---|---|
| Name of experiment and experimental site | EGO VIRGO |
| Is the speaker for that presentation defined? | Yes |
| Internet talk | Maybe |
