Gravitational Wave Detector Zoo

Digital Discovery of interferometric Gravitational Wave Detectors
Mario Krenn^†,1, Yehonathan Drori^†,2,3, Rana X Adhikari^2,3
(† = equal contribution)
¹Max Planck Institute for the Science of Light
²LIGO Laboratory
³California Institute of Technology

Here we present the technical details of solutions discovered by Urania, and the
corresponding PyKat and Finesse files for reproducing the solutions. All solutions
are superior to the LIGO Voyager baseline. As all solutions have superior sensitivity
compared to the LIGO Voyager baseline (which itself is parametrically optimized),
it means that the solution not only has better parameter settings, but necessarily
have new improved topologies.

Goals of the GW Detector Zoo

Getting the gravitational wave community involved to explore and understand the AI-guided solutions,
and learn new AI-inspired ideas and concepts of high-sensitivity interferometers.

• Every interested researcher is invited to contribute their findings to the Zoo (via Issues or Pull Requests).
• We will keep updating the Zoo with new computational results or conceptualization insights.

Details on these four superior solutions can be found at Broadband, Cosmology, Supernova and Neutron Star Post-Merger.

Solutions types

We have solutions for various frequency regimes, with different noise sources, and different
geometric constraints. We sort them by the following properties:

Frequency ranges

• Post-Merger: 800Hz-3000Hz
• Narrow Post-Merger: 2700-3000Hz
• Supernova: 200-1000Hz
• Primodial Black Holes: 10-30Hz
• Broadband: 20-5000Hz

Noise sources

• Quantum: Laser frequency noise, laser intensity noise, quantum noise (thermal noise discussed in detail in paper appendix)

Geometry constraints

• Large: UIFO diameters constraint to 4 kilometres
• Small: Two 4 kilometer arms, and 400x400 meter filters

Solutions

The 50 solutions are sorted by type, and then by sensitivity. Solution0 is the
best performing one, the last solution has lowest sensitivity while being better
than the LIGO Voyager baseline.

• Broad Band, Quantum, Large
  • Solution 0
  • Solution 1
• Narrow Post-Merger, Quantum, Large
  • Solution 0
  • Solution 1
  • Solution 2
  • Solution 3
  • Solution 4
  • Solution 5
  • Solution 6
  • Solution 7
  • Solution 8
• Post-Merger, Quantum, Large
  • Solution 0
  • Solution 1
  • Solution 2
  • Solution 3
  • Solution 4
  • Solution 5
  • Solution 6
  • Solution 7
  • Solution 8
  • Solution 9
  • Solution 10
  • Solution 11
  • Solution 12
  • Solution 13
  • Solution 14
  • Solution 15
  • Solution 16
  • Solution 17
  • Solution 18
  • Solution 19
  • Solution 20
  • Solution 21
  • Solution 22
  • Solution 23
  • Solution 24
• Supernova, Quantum, Large
  • Solution 0
  • Solution 1
  • Solution 2
• Primodial Black Holes, Quantum, Large
  • Solution 0
  • Solution 1
  • Solution 2
  • Solution 3
  • Solution 4
  • Solution 5
  • Solution 6
• Broad Band, Quantum, Small
  • Solution 0
  • Solution 1
  • Solution 2
  • Solution 3

Software

• Plotting the solution .kat files of GWAlgo
• Reproducing the sensitivity plots from a .kat file