The Architecture of the LISA Science Analysis
Creators: name: Teukolsky, Saul A.
name: Vallisneri, Michele
name: Chua, Alvin
name: Akeson, Rachel
name: Archibald, Anne M.
name: Babak, Stanislav
name: Breivik, Katelyn
name: Brown, C. Titus
name: Cornish, Neil J.
name: Cutler, Curt
name: Davidoff, Scott
name: Foucart, Francois
name: Galley, Chad R.
name: Kidder, Lawrence E.
name: Kumar, Prayush
name: Lamberts, Astrid
name: Lovelace, Geoffrey
name: Mahabal, Ashish
name: Corbett Moran, Christine
name: Nuttall, Laura
name: Okounkova, Maria
name: Robson, Travis
name: Scheel, Mark A.
name: Shoemaker, Deirdre
name: Taylor, Stephen
name: Tinto, Massimo
name: Varma, Vijay
name: Vecchio, Alberto
Publisher: name: Keck Institute for Space Studies
Year: 2019

description: The space-based gravitational-wave (henceforth, GW!) observatory LISA (Amaro-Seoane et al., 2017) will o˙er unparalleled science returns, including a view of massive black hole mergers up to high redshifts, precision tests of general relativity and black hole structure, a census of thousands of compact binaries in the Galaxy, and the possibility of detecting stochastic signals from the early Universe. While the Mock LISA Data Challenges (2006–2011) gave us confidence that LISA will be able to fulfill its scientific potential, we still have a rather incomplete idea of what the end-to-end LISA science analysis should look like. The task at hand is substantial: 1) Our data reduction process needs to ensure the phase coherence of GW measurements across data gaps and instrument glitches over multiple years. 2) Our waveform models need to reach part-in-105 accuracy to maximize the science payo˙ of the mission, with suÿcient computational eÿciency to sample parameter space broadly. 3) Our algorithms need to resolve thousands of individual sources of di˙erent types and strengths, all of them superimposed on the same multi-year dataset, while simultaneously characterizing the underlying noise-like stochastic background. 4) Our catalogs need to represent the complex and high-dimensional joint distributions of estimated source parameters for all sources. It is tempting to assume that current algorithms and prototype codes will scale up to this challenge, thanks to the greatly increased computational power that will become available by the time of LISA’s launch in the early 2030s. In reality, harnessing that power will require very di˙erent methods, adapted to future high-performance computational architectures that we can only glimpse now. Thus, we need to begin our exploration at this time, seeking inspiration from other disciplines (e.g., big data processing, computational biology, the most advanced applications in astroinformatics) and learning to pose the same physical questions in di˙erent, future-proof ways—or even daring to imagine questions that will be tractable only with future machines. The broad objective of this study was to imagine how evolved or rethought data analysis algorithms and source-modeling codes will perform the LISA science analysis on the computers of the future, with the hope of guiding LISA science and data analysis research and development in the years to come.
description: K 20191002-102632020