2020/07/31 by Paolo Campeti, Eiichiro Komatsu, Davide Poletti +1
Physics and Astronomy · #Advanced Frequency and Time Standards #Astronomical interferometer #Cosmic background radiation #Cosmic microwave background #Cosmology and Gravitation Theories #Einstein Telescope #Gravitational wave #Gravitational wave background #Gravitational-wave observatory #LIGO #Observatory #Pulsar #Pulsars and Gravitational Waves Research #astro-ph.CO #gr-qc
paper · pdf · doi:10.1088/1475-7516/2021/01/012
Accepted in JCAP. Improved treatment of foregrounds for interferometers and more realistic analytical formula for $Ω_{GW}$. Python code to reproduce figures is available at the link https://github.com/pcampeti/SGWBProbe
openalex created_date 2020/07/16 · arxiv created 2020/11/16 · openalex publication_date 2021/01/08 · arxiv updated 2021/01/20 · openalex updated_date 2026/08/05
We investigate the possibility of measuring the primordial gravitational wave (GW) signal across 21 decades in frequencies, using the cosmic microwave background (CMB), pulsar timing arrays (PTA), and laser and atomic interferometers. For the CMB and PTA experiments we consider the LiteBIRD mission and the Square Kilometer Array (SKA), respectively. For the interferometers we consider space mission proposals including the Laser Interferometer Space Antenna (LISA), the Big Bang Observer (BBO), the Deci-hertz Interferometer Gravitational wave Observatory (DECIGO), the μAres experiment, the Decihertz Observatory (DO), and the Atomic Experiment for Dark Matter and Gravity Exploration in Space (AEDGE), as well as the ground-based Einstein Telescope (ET) proposal. We implement the mathematics needed to compute sensitivities for both CMB and interferometers, and derive the response functions for the latter from the first principles. We also evaluate the effect of the astrophysical foreground contamination in each experiment. We present binned sensitivity curves and error bars on the energy density parameter, Ω GW h 2 , as a function of frequency for two representative classes of models for the stochastic background of primordial GW: the quantum vacuum fluctuation in the metric from single-field slow-roll inflation, and the source-induced tensor perturbation from the spectator axion-SU(2) inflation models. We find excellent prospects for joint measurements of the GW spectrum by CMB and space-borne interferometers mission proposals.