LPF - A Space Saga Part 6 @LISAcommunity

Uploaded May 2021 | Updated September 2026, 2 hours ago

It is May 4th 2021. The LPF mission has ended. LPF results exceeded all expectations. As LPF is sailing towards the sun, the LISA mission is even now in the first phase of realization. LISA will be the largest space structure ever, but LISA is no Death Star. LISA's mission: to probe the Dark Side of the Universe.

Happy Star Wars Day!

Find out more about LISA on lisamission.org

and about LPF’s final journey at
https://blogs.esa.int/rocketscience/2017/07/03/lisa-pathfinder-sails-toward-the-sun/

Experimental backscatter measurement rig for LISA beam dumps and FIOS characterisation

About the modes and tones of Black Hole Ringdowns

LISA Symposium XIV Day 1 Plenary Block 1 Complete

Predictions for Ultra Compact X-Ray Binaries from Combined GW and Electromagnetic Wave Observations

$Testing of a First-Generation Optical Truss Interferometer for the LISA Telescope The LISA telescope is a bidirectional component that is used to expand an outgoing laser beam to the far spacecraft as well as compress a small fraction of a large incoming beam to a diameter of a few mm at the optical bench. Since the telescope lies directly in the path of the long-baseline LISA interferometer, its structure must be dimensionally stable at the pm/âˆšHz level within the 0.1 mHz â€“ 1 Hz frequency band. A way to measure the displacement noise along the optical path of the telescope is with a compact optical truss interferometer (OTI), consisting of three Fabry-Perot cavities mounted along the telescope to monitor structural distortions over time. The premise is that variations in the cavity lengths will be due to dimensional changes in the telescope structure along three different lateral positions. We have developed a fiber-coupled Pound-Drever-Hall (PDH) system that integrates a fiber injector, mode matching optics, and a cavity input mirror into a compact input stage. These input stages will be attached around the primary mirror of the telescope, while the cavity return mirrors will be attached around the secondary mirror of the telescope. Using a PDH-like frequency locking scheme, variations in the cavity lengths will shift the frequency of the locked 1064 nm light which can be monitored through a beat signal between the light from each cavity and a separate laser that is locked to an ultra-stable reference cavity. We have designed and procured three first-generation OTI cavities and are currently testing the prototypes to verify pm/âˆšHz displacement sensitivity. We will present details regarding the design, fabrication, and assembly of the OTI units as well as preliminary results on the prototype testing and plans for future testing and verification. Authors: Kylan Jersey, Ian Harley-Trochimczyk, Yanqi Zhang, Felipe Guzman Presenter: Kylan Jersey$

RF differential phase measurements of the LISA fiber amplifier

Prospecting the precision of massive black hole spectroscopy with LISA

The James Webb Space Telescope - Gillian Wright (UK ATC)

Decelerated sphere as inertial reference sensor for future missions

Thermodynamics of rotating black hole clusters

Effect and Mitigation of LPF Glitches on Simulated LISA TDI Data