Journal
PHYSICAL REVIEW D
Volume 93, Issue 2, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.93.024003
Keywords
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Funding
- European Union's Seventh Framework Programme (FP7/PEOPLE-2011-CIG) through Marie Curie Career Integration Grant [GALFORMBHS PCIG11-GA-2012-321608]
- H2020-MSCA-RISE-2015 [StronGrHEP-690904]
- NSF CAREER [PHY-1055103]
- FCT [IF/00797/2014/CP1214/CT0012]
- European Research Council Consolidator Grant [647839]
- University Research Fellowship of the Royal Society
- Irish Research Council under the National Development Plan for Ireland
- DFG [SFB/Transregio 7]
- European Research Council (ERC) [647839] Funding Source: European Research Council (ERC)
- Division Of Physics
- Direct For Mathematical & Physical Scien [1055103] Funding Source: National Science Foundation
- STFC [ST/K000845/1] Funding Source: UKRI
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We compare the science capabilities of different eLISA mission designs, including four-link (two-arm) and six-link (three-arm) configurations with different arm lengths, low-frequency noise sensitivities and mission durations. For each of these configurations we consider a few representative massive black hole formation scenarios. These scenarios are chosen to explore two physical mechanisms that greatly affect eLISA rates, namely (i) black hole seeding, and (ii) the delays between the merger of two galaxies and the merger of the black holes hosted by those galaxies. We assess the eLISA parameter estimation accuracy using a Fisher matrix analysis with spin-precessing, inspiral-only waveforms. We quantify the information present in the merger and ringdown by rescaling the inspiral-only Fisher matrix estimates using the signal-to-noise ratio from nonprecessing inspiral-merger-ringdown phenomenological waveforms, and from a reduced set of precessing numerical relativity/post-Newtonian hybrid waveforms. We find that all of the eLISA configurations considered in our study should detect some massive black hole binaries. However, configurations with six links and better low-frequency noise will provide much more information on the origin of black holes at high redshifts and on their accretion history, and they may allow the identification of electromagnetic counterparts to massive black hole mergers.
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