http://arxiv.org/abs/2301.02672
Gravitational waves modulate the apparent frequencies of other periodic signals. We propose to use this effect to detect low-frequency gravitational waves by searching for correlated frequency modulations in a large set of well-resolved gravitational wave signals. We apply our proposed method to the large number of gravitational wave signals from Galactic binary white dwarfs that are expected to be detected with the planned space-based gravitational wave detector LISA. We show that, given current projections for the number and properties of these sources and the sensitivity of the instrument, this method would enable the detection of background gravitational wave strain amplitudes of, e.g., $A\simeq10^{-10}$ at a frequency $F\simeq10^{-8}\,\rm Hz$. When using signals from binary neutron stars such as those expected to be observed with proposed detectors like DECIGO, we expect a sensitivity to gravitational waves competitive with that of current Pulsar Timing Arrays. This would allow the detection of gravitational waves from, e.g., super-massive black hole binaries with chirp masses $M_c\gtrsim10^9\,\rm M_\odot$ at a distance $D\simeq10\,\rm Mpc$. Our results show that gravitational-wave detectors could be sensitive at frequencies outside of their designed bandwidth using the same infrastructure. This has the potential to open up unexplored and otherwise inaccessible parts of the gravitational wave spectrum.
J. Stegmann and S. Vermeulen
Tue, 10 Jan 23
84/93
Comments: 10 pages, 5 figures, 1 table, comments welcome