16th LISA Symposium - Plenary Session 10 @LISAcommunity

Uploaded June 2026 | Updated September 2026, 59 minutes ago

Welcome to the tenth plenary session for the 16th LISA Symposium! This is the final plenary session of the meeting.

Presentations in this session:
1) Ten Years After LISA Pathfinder: From Experimental Demonstration to LISA and Beyond - Daniele Vetrugno
2) Tests of fundamental physics with LISA - Emanuele Berti
3) Massive Black Hole Binary waveforms for the Mojito Mock Data Challenge - Antoni Ramos-Buades

16th LISA Symposium - Plenary Session 10

ANALYSIS OF THE GRABBING POSITIONING AND RELEASE MECHANISM PERFORMANCE SENSITIVITY TO ALIGNMENT

Modeling LISA In-band Test Mass Forces Induced by Eddy Currents

Covariant and coordinate punctures for 2nd-order gravitational self-force in a highly regular gauge

LISA Symposium XIV Parallel C LISA Data Analysis 2 part 2

A testbed for Tilt-To-Length coupling and Differential-Wavefront-Sensing performance in LISA

$Evaluating a phenomenological approach to spin precession in current gravitational wave events. Unlike in Newtonian dynamics, if two gravitationally bound objects are individually spinning in general relativity, their spins will interact and their orbit will precess. This spin precession leaves an imprint on the gravitational wave signal. The catalog of gravitational wave events has already been investigated for spin precession, described using the two effective parameters $chi_{rm eff}$ and $chi_{P}$ (focussing on the spin precession of binary black holes). Here, we repeat the investigation but with a geometrical approach. Spin precession is characterised as the spin precession of the orbital plane, split into its azimuthal motion (its precession) and its polar motion (its nutation). Looking for these effects, and understanding what binary parameters influence them, is non-trivial. We use sequential prior conditioning to resolve this. Prior conditioning is performed by combining prior distributions with posterior distributions of the parameters were conditioning our priors on. We find that nutation, given its small expected amplitudes, is difficult to constrain. Precession, on the other hand, is clearly constrained, especially for events with highly unequal masses and relatively high signal to noise ratios. We also construct a synthetic binary that we would expect to have a high nutational amplitude, and show that with the future detector sensitivities of ground based gravitational wave observatories, these events are detectable and their nutation can be constrained to be non-zero. Authors: Daria Gangardt, Davide Gerosa, Michael Kesden, Viola De Renzis, Nathan Steinle Presenter: Daria Gangardt$

Null channel formalism of triangular GW interferometers with non-identical & correlated noise

Experimental studies of fiber phase dynamics in the scope of the LISA backlink