LISA Symposium 2026 - Plenary 9 @LISAcommunity

Uploaded August 2026 | Updated September 2026, 2 hours ago

(Recorded on June 26, 2026)

Welcome to the ninth plenary session for the 16th LISA Symposium!

Presentations in this session:
00:00:18 - Consortium Overview & Update - Niels Warburton
00:32:20 - Gaps and Glitches in LISA Data - Jean-Baptiste Bayle
01:03:00 - Probing symmetry breaking in the early universe with LISA - Bogumiła Świeżewska
01:33:00 - Gravitational wave observatories from the ground to pulsar timing arrays - Joey Shapiro Key

Session Chair: Neil Cornish

LISA Symposium XIV Parallel B Multi-Messenger Astrophysics and SMBHs Part 2

Predicting GW signals from compact binary population of a Milky Way like galaxy for LISA

LECSTalks! Writing Research & Teaching Statements for Faculty/Postdoc Positions by Lance Cooper

Progress of the investigation for thermal effect in space GW detection mission TianQin

$AMIGO: Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Astrodynamical middle-frequency interferometric gravitational wave observatory Wei-Tou Ni, Gang Wang and An-Ming Wu AMIGO is a first-generation Astrodynamical Middle-frequency Interferometric GW Observatory. The scientific goals of AMIGO are: to bridge the spectra gap between first-generation high-frequency and low-frequency GW sensitivities; to detect intermediate mass BH coalescence; to detect inspiral phase and predict time of binary black hole coalescence together with neutron star coalescence for ground interferometers; to detect compact binary inspirals for studying stellar evolution and galactic population. The mission concept is to use time delay interferometry for a nearly triangular formation of 3 drag-free spacecraft with nominal arm length 10,000 km, emitting laser power 2-10 W and telescope diameter 300-500 mm. The design GW sensitivity in the middle frequency band is 3 x 10^(-21) Hz^(-1/2). Both heliocentric and geocentric orbits are under study. All options have LISA-like formations, that is the triangular formation is 60 deg inclined to the orbit plane. For AMIGO, the first-generation time delay interferometry is good enough for the laser frequency noise suppression. We also investigate for each options of orbits under study, whether constant equal-arm implementation is feasible. For the solar-orbit option, the acceleration to maintain the formation can be designed to be less than 15 nm/s2 with the thruster requirement in the 15 {mu}N range. AMIGO would be a good place to implement the constant equal-arm option. Fuel requirement, thruster noise requirement and test mass acceleration actuation requirement are briefly considered. From the orbit study, the solar orbit option is the first mission orbit choice. We study the deployment for this orbit option. A last-stage launch from 300 km LEO (Low Earth Orbit) to an appropriate 2-degree-behind-the-Earth AMIGO formation in 95 days requires only a {delta}v of 75 m/s.$

Resolving Galactic binaries using a network of space-borne gravitational wave detectors

Highlighting a milestone for LISA: Our understanding and long-term results of LPF interferometry