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Dr Jennifer Wright (LIGO Hanford Observatory)Optical DesignPresentation
Jitter noise limits the LIGO H1 sensitivity between 100 and 500 Hz and L1 below 40 Hz. This is caused by motion in the pointing of the input beam from the in-air laser enclosure, relative to the rest of the detector which is in vacuum. This beam jitter imposes first order higher order modes on the light, and couples into the output of the detector as intensity noise due to imperfections in the...
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Anna Green (Nikhef, Maastricht University)Optical DesignPresentation
As the designs of next generation GW facilities like ET and CE progress, we will need to specify requirements for each optical element. These should build on the success of current optics, while incorporating the experiences of 2G (e.g. point absorbers) and accounting for new behaviours we know to anticipate from new material choices. One challenge is how to actually write these requirements...
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Mattia Boldrini (European Gravitational Observatory - EGO)Optical DesignPresentation
Accomodating stable recycling cavities in Advanced Virgo+ would fundamentally change the behavior of the interferometer in a variety of ways, introducing many advantages in terms of residual noise in the sensitivity curve, but also necessarily forcing to re-design the control scheme to account for the four new mirrors in the folded cavities.
The Virgo Interferometer Sensing & Control team...
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Anna Green (Nikhef, Maastricht University), Mikhail Korobko (University of Hamburg)Optical DesignPresentation
The Einstein Telescope has begun to transition from ‘concept’ to ‘project’ – meaning the tricky work of integrating the many essential technologies, currently still in R&D, into one coherent detector design. Over the last two years, intensive efforts have resulted in new optical layouts, informed by basic optical requirements towards the sensitivity and controllability of each interferometer,...
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Matthew Todd (Syracuse University)Optical DesignPresentation
The relative intensity noise of a laser source impacts the interferometers non-trivially. Understanding how the intensity noise couples to different parts of the interferometer yields various important metrics to the stability and performance of the detector. These metrics also change in time as the interferometer thermalizes. Though current detectors’ differential arm sensitivities are not...
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Matteo Ianni (INFN, Section of Rome Tor Vergata, Rome, Italy. University of Rome Tor Vergata, Department of Physics, Rome, Italy)Optical DesignPresentation
Enhancing the sensitivity of gravitational-wave detectors represents a major challenge as it requires stable operation at progressively higher optical powers. Increased circulating power within the Fabry–Pérot arm cavities amplifies thermal effects, leading to wavefront aberrations that, if not properly compensated, can significantly degrade the instrument’s performance.
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For the foreseen O5... -
Ward Amar (LAPP - CNRS)Optical DesignPresentation
In this talk, I present the optical design studies that we made for implementing stable power and signal recycling cavities for the gravitational wave detector Advanced Virgo+. We show that, despite the limited space available in the present infrastructure, a reshaping of the vacuum envelope allows accommodating two folded stable recycling cavities at the input and at the output of the...
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Kevin KunsOptical DesignPresentation
Future upgrades and detectors aim to both reduce quantum noise by 10 dB and to increase the circulating power in the interferometer arm cavities. Achieving these goals will be extremely challenging due, in part, to the degradations to the squeezed state caused by mode mismatch between the internal interferometer optical cavities and between the auxiliary external cavities. There are two types...
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Anne Daumas (APC - CNRS)Optical DesignPresentation
Challenges related to the current Virgo optical configuration have led to a redesign of the interferometer's recycling cavities, in order to improve instrument sensitivity and control. The new, non-degenerate (or “stable”) recycling cavities design requires, among other changes, a complete redesign of the auxiliary benches hosting the injection and detection optics. In this talk we will...
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