Journal
PHYSICAL REVIEW D
Volume 95, Issue 10, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.95.103012
Keywords
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Funding
- Royal Society
- H-MSCA-RISE Grant [StronGrHEP-690904]
- APACHE grant of the French Agence Nationale de la Recherche [ANR-16-CE31-0001]
- NSF [PHY-1607130]
- Fundacao para a Ciencia e a Tecnologia (FCT) [IF/00797/2014/CP1214/CT0012]
- Spanish Ministry of Economy and Competitivity of Spain, MINECO [ESP2013-47637-P, ESP2015-67234-P]
- Science and Technology Facilities Council
- Ramon y Cajal Programme of the Ministry of Economy, Industry and Competitiveness of Spain
- CAS President's International Fellowship Initiative
- Centre National d'Etudes Spatiales
- STFC [ST/N000633/1] Funding Source: UKRI
- Direct For Mathematical & Physical Scien
- Division Of Physics [1607130] Funding Source: National Science Foundation
- Fundação para a Ciência e a Tecnologia [IF/00797/2014/CP1214/CT0012] Funding Source: FCT
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The space-based Laser Interferometer Space Antenna (LISA) will be able to observe the gravitational-wave signals from systems comprised of a massive black hole and a stellar-mass compact object. These systems are known as extreme-mass-ratio inspirals (EMRIs) and are expected to complete similar to 104-105 cycles in band, thus allowing exquisite measurements of their parameters. In this work, we attempt to quantify the astrophysical uncertainties affecting the predictions for the number of EMRIs detectable by LISA, and find that competing astrophysical assumptions produce a variance of about three orders of magnitude in the expected intrinsic EMRI rate. However, we find that irrespective of the astrophysical model, at least a few EMRIs per year should be detectable by the LISA mission, with up to a few thousands per year under the most optimistic astrophysical assumptions. We also investigate the precision with which LISA will be able to extract the parameters of these sources. We find that typical fractional statistical errors with which the intrinsic parameters (redshifted masses, massive black hole spin and orbital eccentricity) can be recovered are similar to 10(-6)-10(-4). Luminosity distance (which is required to infer true masses) is inferred to about 10% precision and sky position is localized to a few square degrees, while tests of the multipolar structure of the Kerr metric can be performed to percent-level precision or better.
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