Science with the space-based interferometer eLISA: Supermassive black hole binaries

By A. Klein, E. Barausse, A. Sesana, A. Petiteau, Emanuele Berti, Stanislav Babak, Jonathan R. Gair, S. Aoudia, Ian Hinder, Frank Ohme and 1 more. 2015

340 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/900eca41c2ac6ddd327b51c116ac271337c29a49

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Citations in the corpus

Science with the space-based interferometer eLISA. III: probing the expansion of the universe using gravitational wave standard sirens (2016, background): “The first paper of this series [16] has dealt with the cosmological evolution of MBHBs.”
Testing modified gravity at cosmological distances with LISA standard sirens (2019, methodology): “es and they are expected to be observed in dierent redshift ranges. In particular, stellar mass BHBs will mainly be detected at 0:01 . z. 0:1 [166], EMRIs at 0:1 . z. 2 3 [167] and MBHBs at z& 1 [168], implying that LISA will constitute a cosmological probe able to map the expansion of the unive”
Probing the theory of gravity with gravitational lensing of gravitational waves and galaxy surveys (2019, methodology): “Along with the ground-based gravitational wave detectors, spacebased gravitational wave experiment such as LISA (Laser Interferometer Space Antenna) Klein et al. (2016); AmaroSeoane et al. (2017) are going to measure the gravitational wave signal emitted from supermassive binary black holes in the…”
Science with the space-based interferometer eLISA. II: gravitational waves from cosmological phase transitions (2015, background): “For a more detailed discussion on the status of the eLISA mission and its possible designs, we refer the reader to the first paper of this series [3].”
Science with the space-based interferometer LISA. IV: probing inflation with gravitational waves (2016, background): “The first paper of this series dealt with the GW signal from massive black hole binaries [65], the second paper with the stochastic background from first order phase transitions occurring in the early Universe [39], and the third one with the use of massive black hole binaries as standard sirens to ”
THE FINAL SPIN FROM BINARY BLACK HOLES IN QUASI-CIRCULAR ORBITS (2016, background): “More massive BH binaries are targeted by existing pulsar-timing arrays (in the mass range 108 − 1010M ; Manchester & IPTA 2013) and by future space-borne interferometers such as eLISA (in the mass range 104 − 107M ; Klein et al. 2016).”
Unveiling the gravitational universe at μ-Hz frequencies (2019, background): “out their geometric structure; and pierce through the cosmic microwave background (CMB) to probe the physics of the early Universe [14, 23, 34, 68, 155, 160, 252].”
Improved reconstruction of a stochastic gravitational wave background with LISA (2020, background): “Depending on the astrophysical formation scenarios [8–12], LISA is going to detect few hundreds of massive (∼ 104–107M ) black hole binary mergers with Signal-to-Noise Ratio (SNR) up to thousand.”
Superradiance (2015, methodology): “[128], LISA will have the ability to measure BH masses and spins with a very good precision [641], in a range of masses largely complementary to the ones coming from ground-based GW detector and EM observations.”
Multi-messenger astrophysics (2019, methodology): “110]. In order to study the merger of the much larger (106 to 108M ) \supermassive" black holes located at the center of galaxies, the EU is planning a large space-based GW detector called eLISA [112], consisting of an interferometer using three small satellites in Solar orbit. A dierent techni”
Constraining the mass of dark photons and axion-like particles through black-hole superradiance (2018, methodology): “The arrows denote the range of projected LISA measurements using three different population models for supermassive BH growth (popIII, Q3 and Q3-nod from [81], cf.”
A Review of Gravitational Waves from Cosmic Domain Walls (2017, background): “Space-borne interferometers such as eLISA [128,129] and DECIGO [130] are planned to be launched in the future, and they will enable us to explore lower frequency ranges, which cannot be probed in the ground-based experiments.”