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"Testing General Relativity with Low-Frequency, Space-Based Gravitational-Wave Detectors"

Jonathan R. Gair and Michele Vallisneri and Shane L. Larson and John G. Baker

	Abstract
1	Introduction
2	The Theory of Gravitation
	2.1	Will’s “standard model” of gravitational theories
	2.2	Alternative theories
	2.3	The black-hole paradigm
3	Space-Based Missions to Detect Gravitational Waves
	3.1	The classic LISA architecture
	3.2	LISA-like observatories
	3.3	Mid-frequency space-based observatories
4	Summary of Low-Frequency Gravitational-Wave Sources
	4.1	Massive black-hole coalescences
	4.2	Extreme-mass-ratio inspirals
	4.3	Galactic binaries
5	Gravitational-Wave Tests of Gravitational Physics
	5.1	The “classic tests” of general relativity with gravitational waves
	5.2	Tests of general relativity with phenomenological inspiral template families
	5.3	Beyond the binary inspiral
6	Tests of the Nature and Structure of Black Holes
	6.1	Current observational status
	6.2	Tests of black-hole structure using EMRIs
	6.3	Tests of black-hole structure using ringdown radiation: black-hole spectroscopy
	6.4	Prospects from gravitational-wave and other observations
7	Discussion
	Acknowledgements
	References
	Footnotes
	Figures
	Tables

“Peeling” refers to the fact that different parts of the metric (specifically the Weyl tensor) fall off at different rates with distance. The dominant monopole component is effectively the mass of the central object, while the next-order component, the current dipole, is effectively the spin or angular momentum of the central black hole. The “peeling” constraints imposed in [458 ] ensured that the mass and spin were not changed by the perturbation. Such changes are already contained within the Kerr metric family and do not represent modifications to GR.