Presentation materials
Original title: Comparing gravitational waveform models for binary black hole mergers: a hypermodels approach
The inference of source parameters from gravitational-wave signals relies on theoretical models that describe the emitted waveform. Different model assumptions on which the computation of these models is based could lead to biases in the analysis of gravitational-wave data. In this...
The Dutch contribution to the Laser Interferometer Space Antenna (LISA) covers both hardware and data analysis. Focusing on the hardware, the Netherlands will deliver 'The Eyes of LISA', known as the Quadrant Photo-Receivers (QPRs), made up of segmented InGaAs photodiodes with read-out electronics in an ultra-stable housing. Furthermore, The Netherlands is developing the Point Ahead Alignment...
The purpose of the cryogenic system of the mirror coating test facility is to keep the mirror samples at constant low temperature for optical measurements. Unlike the Einstein Telescope and Pathfinder, the system will not operate continuously. Discontinuous operation allows us to use a standard mechanical cryocooler along with energy storage. During measurements, the cryocooler is switched off...
Currently, the design sensitivity of the second generation Gravitational-Wave (GW) detectors is limited in the low and mid frequency range by Thermal Noise (TN) and Seismic Noise (SN).
Major improvements in GW instrumentation science are expected from the Thermal Noise (TN) reduction in the mid-frequency range of the detectors, achievable also by cooling down the mirrors to 10K.
In order to...
One of the fundamental limitations to the sensitivity of current gravitational wave (GW) detectors, especially in their mid-frequency range, is Brownian thermal noise. This noise source affects not only mirror coatings but also mirror substrates and suspensions, potentially limiting the sensitivity of third-generation GW detectors.
To overcome these limitations, the plan is to replace...
The precise monitoring and active damping of seismic noise are paramount in gravitational wave (GW) detectors. This presentation outlines our research focused on the application of Linear Variable Differential Transformers (LVDTs) as position sensors in these detectors. LVDTs, based on mutual induction, offer a non-contact, linear response.
A simulation framework has been developed using...
The ET-LF test masses will be at cryogenic temperature. A new suspension idea was proposed to ensure good thermal conductivity, low mechanical stress, and low thermal noise. The idea is based on the use of flexural joints in compression. The disadvantage of this suspension is that vertical frequencies are high (16 Hz) and there are many possibilities that the 4 suspensions have a different...
We want the future Einstein Telescope gravitational wave detector to be sensitive from 3Hz onwards. To reach this low frequency sensitivity we need to break the low frequency seismic wall and battle the controls noise that is limiting current detectors at 20Hz.
At Nikhef and the Vrije Universiteit Amsterdam, the Omnisens project is building a prototype of an active platform with a 6D sensor...
In this talk we present a comprehensive software overview that is necessary for simulation, design and fabrication of high tolerance cavities in 3G GW Interferometers. An in-depth review of software is given along with the prescribed workflows and production/metrology loops. We discuss the complementary of different software solutions and aplications of FFT, modal and ABCD(EF) matrix...
We propose a novel scheme how to obtain quantum back action evading measurement on a gravitational wave detector, by introducing negative radiation pressure coupling between the field and the end mirror. The scheme consists of replacing the end mirror with a double-faced one and adding another optical cavity next to it. The measurement is performed by sending a two-mode squeezed vacuum to both...
