LPF - A Space Saga Part 1 @LISAcommunity

Uploaded January 2021 | Updated September 2026, 2 hours ago

5 years ago on this day… It is January 13, 2016. The laser on board the LISA Pathfinder spacecraft lights up for the first time. Tension back home on Earth is mounting. The spacecraft is already more than a million kilometers away and carries a delicate experiment. Decades of research have culminated in this mission, but so many things could still go wrong ...
Find out more at lisamission.org/news/top-news/laser-light-lisa-pathfinder.

LISA Symposium XIV Parallel D EMRIs part 2

Status of the LISA Enhanced Temperature Subsystem (LETS)

Prospects for Detecting Exoplanets around Double White Dwarfs with LISA and Taiji

LISA Symposium XIV Parallel A Beyond LISA Part 2

$Numerical Relativity Surrogate model for eccentric binary black hole gravitational waveform Numerical Relativity Surrogate model for eccentric binary black hole gravitational waveform Tousif Islam, Vijay Varma, Jacqueline Lodman, Scott Field and Gaurav Khanna Though Numerical Relativity (NR) simulations provide the most accurate gravitational waveforms for binary black holes (BBHs), they are computationally expensive, taking days to weeks to generate one single waveform. NR surrogate waveform models are computationally cheaper without sacrificing accuracy. While surrogate models for non-spinning, aligned spin and precessing BBHs are quite reliable, efforts to build an eccentric NR surrogate model are still at an early stage. We provide detailed data decomposition and parameterization strategies to build an effective NR surrogate for eccentric BBHs waveforms. Based on the proposed framework, we then present a time domain, inspiral-merger-ringdown NR surrogate model for eccentric binary black holes for mass ratio $q=1$. We call it NRSur2dq1Ecc. The model includes the (l=2,m=2), (l=3,m=2) and (l=4,m=4) spin-weighted spherical harmonic modes. The odd $m$ modes are zero due to the symmetry of the system. We parameterize the effect of eccentricity via eccentric parameter $e_w$ and mean anomaly $l_w$. This model has been trained against 41 NR waveforms with mass ratio $q=1$, $e_wlt0.175$ and $0ltl_wlt2pi$ (as estimated at a reference time of $t_{ref} 4200M$); and uses Gaussian Process Regression to build the fits across parameter space. We show that our model can accurately predict NR waveforms with mismatches $approx 10^{-3}$ and can recover subtle effects like mode-mixing in the ringdown signal. The method proposed here would pave the way forward for constructing any future surrogate waveform model with eccentric binaries.$

IfoCAD simulations for TTL noise analyses in LISA

LISA Symposium XIV Parallel A LISA Instrumentation 3 Part 2

Experimental backscatter measurement rig for LISA beam dumps and FIOS characterisation

About the modes and tones of Black Hole Ringdowns

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