Atomic gravitational wave interferometric sensor

TLDR

The authors propose terrestrial and satellite atom‑interferometer gravitational‑wave detectors based on the Stanford 10 m interferometer and analyze background control methods. The detectors employ two widely separated atom interferometers driven by common lasers, with signal scaling with baseline length; a terrestrial ~1 km baseline achieves ~10⁻¹⁹ /√Hz sensitivity in 1–10 Hz, while a satellite ~1000 km baseline reaches ~10⁻²⁰ /√Hz, and ballistic atoms reduce vibration systematics and spacecraft control needs. The terrestrial detector can reach strain sensitivity ~10⁻¹⁹ /√Hz in 1–10 Hz and detect solar‑mass binaries out to megaparsec distances, while the satellite detector can probe the LISA band with ~10⁻²⁰ /√Hz sensitivity.

Abstract

We propose two distinct atom interferometer gravitational wave detectors, one terrestrial and another satellite based, utilizing the core technology of the Stanford 10 m atom interferometer presently under construction. Each configuration compares two widely separated atom interferometers run using common lasers. The signal scales with the distance between the interferometers, which can be large since only the light travels over this distance, not the atoms. The terrestrial experiment with two $\ensuremath{\sim}10\text{ }\text{ }\mathrm{m}$ atom interferometers separated by a $\ensuremath{\sim}1\text{ }\text{ }\mathrm{km}$ baseline can operate with strain sensitivity $\ensuremath{\sim}\frac{{10}^{\ensuremath{-}19}}{\sqrt{\mathrm{Hz}}}$ in the 1 Hz--10 Hz band, inaccessible to LIGO, and can detect gravitational waves from solar mass binaries out to megaparsec distances. The satellite experiment with two atom interferometers separated by a $\ensuremath{\sim}1000\text{ }\text{ }\mathrm{km}$ baseline can probe the same frequency spectrum as LISA with comparable strain sensitivity $\ensuremath{\sim}\frac{{10}^{\ensuremath{-}20}}{\sqrt{\mathrm{Hz}}}$. The use of ballistic atoms (instead of mirrors) as inertial test masses improves systematics coming from vibrations and acceleration noise, and significantly reduces spacecraft control requirements. We analyze the backgrounds in this configuration and discuss methods for controlling them to the required levels.