Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime

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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This document introduces the exciting and fundamentally new science and astronomy that the European New Gravitational Wave Observatory (NGO) mission (derived from the previous LISA proposal) will deliver. The mission (which we will refer to by its informal name eLISA ) will survey for the first time the low-frequency gravitational wave band (about 0.1 mHz to 1 Hz), with sufficient sensitivity to detect interesting individual astrophysical sources out to z = 15. The measurements described here will address the basic scientific goals that have been captured in ESA s New Gravitational Wave Observatory Science Requirements Document ; they are presented here so that the wider scientific community can have access to them. The eLISA mission will discover and study a variety of cosmic events and systems with high sensitivity: coalescences of massive black holes binaries, brought together by galaxy mergers; mergers of earlier, less-massive black holes during the epoch of hierarchical galaxy and black-hole growth; stellar-mass black holes and compact stars in orbits just skimming the horizons of massive black holes in galactic nuclei of the present era; extremely compact white dwarf binaries in our Galaxy, a rich source of information about binary evolution and about future Type Ia supernovae; and possibly most interesting of all, the uncertain and unpredicted sources, for example relics of inflation and of the symmetry-breaking epoch directly after the Big Bang. eLISA s measurements will allow detailed studies of these signals with high signal-to-noise ratio, addressing most of the key scientific questions raised by ESA s Cosmic Vision programme in the areas of astrophysics and cosmology. They will also provide stringent tests of general relativity in the strong-field dynamical regime, which cannot be probed in any other way. This document not only describes the science but also gives an overview on the mission design and orbits. LISA s heritage in the eLISA design will be clear to those familiar with the previous proposal, as will its incorporation of key elements of hardware from the LISA Pathfinder mission, scheduled for launch by ESA in 2014. But eLISA is fundamentally a new mission, one that will pioneer the completely new science of low-frequency gravitational wave astronomy. 4 of

Subfields: Astronomy and Astrophysics

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Citations in the corpus

A Population of Short-Period Variable Quasars from PTF as Supermassive Black Hole Binary Candidates (2016, background): “…be detectable by Pulsar Timing Arrays (North American Nanohertz Observatory for Gravitational waves; Jenet et al. 2009, Parkes Pulsar Timing Array; Manchester 2008, European Pulsar Timing Array; Janssen et al. 2008) or future space-based interferometers, such as eLISA (Amaro-Seoane et al. 2013).”
The evolution of massive black holes and their spins in their galactic hosts (2012, background): “…such as the Laser Interferometer Space Antenna (LISA) (Bender et al. 1998; Danzmann Rüdiger 2003; The LISA International Science Team 2011) or a similar mission led by ESA (eLISA/NGO, see Amaro-Seoane et al. (2012); Jennrich et al. (2012)) or NASA (SGO, see The SGO Core Concept Team (2011)).”
Rapid Eccentricity Oscillations and the Mergers of Compact Objects in Hierarchical Triples (2013, background): “EMRIs consist of a binary of stellar-mass objects in orbit around a SMBH (see, e.g., Amaro-Seoane et al. 2007; Amaro-Seoane 2012; Amaro-Seoane et al. 2013a).”
Eccentric Black Hole Gravitational-wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters (2017, background): “…the lower bound of the sensitive frequency band is around ∼1 Hz, for the Einstein Telescope13 (ET, Punturo et al. 2010); for space-based GW observatories, the upper bound of the sensitive frequency band for the Laser Interferometer Space Antenna14 (LISA) is around ∼1 Hz (Amaro-Seoane et al. 2013).”
BINARY BLACK HOLE ACCRETION FROM A CIRCUMBINARY DISK: GAS DYNAMICS INSIDE THE CENTRAL CAVITY (2013, background): “Typical binary BH GW sources detected by a space interferometer at higher frequencies, such as eLISA (Amaro-Seoane et al. 2013), would be well past the decoupling epoch, but the lowest-mass, unequalmass eLISA sources may still be surrounded by a circumbinary disk (Yunes et al. 2011; Kocsis et al.…”
Gravitational-wave sensitivity curves (2014, methodology): “For a review of the GW sources for space-based missions see, for example, Amaro-Seoane et al (2013), Gair et al (2013) or Jennrich et al (2011).”
Observable Spectra of Induced Gravitational Waves from Inflation (2012, methodology): “value and is compatible with instant reheating into a radiation 5We use the detector parameters of the original NASA/ESA experiment which are available, however this is now a European only experiment [63] and the detector speciciations have changed slightly, as dicussed in Appendix (D). { 13 { Figur”