Low-frequency gravitational-wave science with eLISA/NGO

By P. Amaro-Seoane, S. Aoudia, Stanislav Babak, P. Bin'etruy, Emanuele Berti, A. Boh'e, C. Caprini, M. Colpi, N. Cornish, K. Danzmann and 20 more. 2012

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We review the expected science performance of the New Gravitational-Wave Observatory (NGO, a.k.a. eLISA), a mission under study by the European Space Agency for launch in the early 2020s. eLISA will survey the low-frequency gravitational-wave sky (from 0.1 mHz to 1 Hz), detecting and characterizing a broad variety of systems and events throughout the Universe, including the coalescences of massive black holes brought together by galaxy mergers; the inspirals of stellar-mass black holes and compact stars into central galactic black holes; several millions of ultra-compact binaries, both detached and mass transferring, in the Galaxy; and possibly unforeseen sources such as the relic gravitational-wave radiation from the early Universe. eLISA’s high signal-to-noise measurements will provide new insight into the structure and history of the Universe, and they will test general relativity in its strong-field dynamical regime.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/4230c401ac7f74ce712e4c42383786057264d420

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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, methodology): “For eLISA, this method has the advantage of exploiting not only MBHBs as standard sirens, but also extreme mass ratio inspirals (EMRIs), which should be detected in large numbers (see [104] and references therein).”
RESONANT POST-NEWTONIAN ECCENTRICITY EXCITATION IN HIERARCHICAL THREE-BODY SYSTEMS (2012, background): “…might be detectable using LIGO5 and VIRGO6 (e.g., Wen 2003 but see Mandel et al. 2008 and O’Leary et al. 2006), pulsar timing arrays (e.g., Finn & Lommen 2010; Amaro-Seoane et al. 2010; Kocsis et al. 2012), and future space-based GW observatories, such as eLISA/NGO (Amaro-Seoane et al. 2012a,b)7.”
INTO THE LAIR: GRAVITATIONAL-WAVE SIGNATURES OF DARK MATTER (2013, methodology): “The late-time inspiral of this system is of interest to future space-based GW detectors (Amaro-Seoane et al. 2012a,b).”
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].”
Supernova Type Ia progenitors from merging double white dwarfs - Using a new population synthesis model (2012, background): “The DWDs are expected to be the dominant source (Evans et al. 1987; Nelemans et al. 2001a) of gravitational waves for the future space-born gravitational wave observatories such as eLISA (Amaro-Seoane et al. 2012a,b).”
Search for New Physics with Atoms and Molecules (2017, methodology): “, 2011) and Evolved-LISA (eLISA) (Amaro-Seoane et al., 2012)] and both terrestrial and space based matter-wave”
Models of low-mass helium white dwarfs including gravitational settling, thermal and chemical diffusion, and rotational mixing (2016, background): “Moreover, they are expected to be excellent sources of gravitational waves (Hermes et al. 2012a; Kilic et al. 2013) and verification sources for gravitational detectors such as eLISA (Amaro-Seoane et al. 2012).”
Prospects for detection of detached double white dwarf binaries with Gaia, LSST and LISA (2017, background): “…surveys such as Gaia (Gaia Collabora- E-mail: korol@strw.leidenuniv.nl tion et al. 2016) and the Large Synoptic Survey Telescope (LSST) (LSST Science Collaboration et al. 2009), and in gravitational waves (GWs) with the Laser Interferometer Space Antenna (LISA) mission (Amaro-Seoane et al. 2012).”
Supermassive black holes and their feedback effects in the IllustrisTNG simulation (2017, background): “These differences in merger rates at black hole masses up to 107.5 M imply that future space-based gravitational wave detectors such as eLisa (Amaro-Seoane et al. 2012) will be able to differentiate between different models for the SMBH growth.”