Probing Fundamental Physics with Gravitational Waves: The Next Generation. (arXiv:2010.09010v2 [gr-qc] UPDATED)
<a href="http://arxiv.org/find/gr-qc/1/au:+Perkins_S/0/1/0/all/0/1">Scott E. Perkins</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Yunes_N/0/1/0/all/0/1">Nicolás Yunes</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Berti_E/0/1/0/all/0/1">Emanuele Berti</a>
Gravitational wave observations of compact binary mergers are already
providing stringent tests of general relativity and constraints on modified
gravity. Ground-based interferometric detectors will soon reach design
sensitivity and they will be followed by third-generation upgrades, possibly
operating in conjunction with space-based detectors. How will these
improvements affect our ability to investigate fundamental physics with
gravitational waves? The answer depends on the timeline for the sensitivity
upgrades of the instruments, but also on astrophysical compact binary
population uncertainties, which determine the number and signal-to-noise ratio
of the observed sources. We consider several scenarios for the proposed
timeline of detector upgrades and various astrophysical population models.
Using a stacked Fisher matrix analysis of binary black hole merger
observations, we thoroughly investigate future theory-agnostic bounds on
modifications of general relativity, as well as bounds on specific theories.
For theory-agnostic bounds, we find that ground-based observations of
stellar-mass black holes and LISA observations of massive black holes can each
lead to improvements of 2-4 orders of magnitude with respect to present
gravitational wave constraints, while multiband observations can yield
improvements of 1-6 orders of magnitude. We also clarify how the relation
between theory-agnostic and theory-specific bounds depends on the source
properties.
Gravitational wave observations of compact binary mergers are already
providing stringent tests of general relativity and constraints on modified
gravity. Ground-based interferometric detectors will soon reach design
sensitivity and they will be followed by third-generation upgrades, possibly
operating in conjunction with space-based detectors. How will these
improvements affect our ability to investigate fundamental physics with
gravitational waves? The answer depends on the timeline for the sensitivity
upgrades of the instruments, but also on astrophysical compact binary
population uncertainties, which determine the number and signal-to-noise ratio
of the observed sources. We consider several scenarios for the proposed
timeline of detector upgrades and various astrophysical population models.
Using a stacked Fisher matrix analysis of binary black hole merger
observations, we thoroughly investigate future theory-agnostic bounds on
modifications of general relativity, as well as bounds on specific theories.
For theory-agnostic bounds, we find that ground-based observations of
stellar-mass black holes and LISA observations of massive black holes can each
lead to improvements of 2-4 orders of magnitude with respect to present
gravitational wave constraints, while multiband observations can yield
improvements of 1-6 orders of magnitude. We also clarify how the relation
between theory-agnostic and theory-specific bounds depends on the source
properties.
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