Optimizing the third generation of gravitational-wave observatories for Galactic astrophysics

Abstract

Gravitational-wave (GW) astrophysics is a rapidly expanding field, with plans to enhance the global ground-based observatory network through the addition of larger, more sensitive observatories: Einstein Telescope and Cosmic Explorer. These observatories will allow us to peer deeper into the sky, collecting GW events from farther away and earlier in the Universe. Within our own Galaxy, there is a plethora of interesting GW sources, including core-collapse supernovae, phenomena in isolated neutron stars and pulsars, and potentially novel sources. As GW observatories are directionally sensitive, their placement on the globe will affect the observation of Galactic sources. We analyze the performance of one-, two-, and three-observatory networks, both for sources at the Galactic center, as well as a source population distributed over the Galactic disk. We find that, for a single Cosmic Explorer or Einstein Telescope observatory, placement at near-equatorial latitudes provides the most reliable observation of the Galactic center. When a source population distributed over the Galactic disk is considered, the observatory location is less impactful, although equatorial observatories still confer an advantage over observatories at more extreme latitudes. For two-and three-node networks, the longitudes of the observatories additionally become important for consistent observation of the Galaxy.

Quantum signatures in nonlinear gravitational waves

“…Quadruple systems of massive stars, the progenitors of black holes and neutron stars, are actually common, calculated to be ∼ 20% [52], but it appears difficult for all of the stars to form black holes [53] much less merge. A study of double merger systems could be of great value for the optimization of third generation gravitational wave detectors [54] and beyond.…”