Statistical imprints of wave-like dark matter on multiply-imaged galaxies in strong cluster lenses from JWST

Abstract

Wave-like dark matter ($\ddot{I}ˆ$DM) is an elusive dark matter (DM) candidate. The model, often also called fuzzy or ultralight DM, proposes that DM is an extremely light ($m\sim 10^{-22}$ eV) boson and thereby has a kpc-scale de Broglie wavelength. Hence, interference of DM gives rise to sub-galactic density fluctuations that can be studied with strong gravitational lensing. In this paper, we use the residual power spectrum, ${\mathrm{P}}_{\hat{I}}´(k)$, as a probe of $\ddot{I}ˆ$DM, which quantifies deviations from smooth lensing predictions, measured from multiply-imaged galaxies in strong cluster lenses. The key idea is that imprinted in these deviations are lensing distortions from DM substructure, which can be harnessed statistically to distinguish among DM theories. We simulate JWST-quality mock observations of strong gravitational lensing in galaxy clusters, modeling line-of-sight DM substructure within $\ddot{I}ˆ$DM and the standard cold dark matter (CDM) paradigms. Using mock deep observations ($\sim$ 20 hours), we find that ${\mathrm{P}}_{\hat{I}}´(k)$ is sensitive to both $\ddot{I}ˆ$DM particle mass and fluctuation amplitude, and can distinguish $\ddot{I}ˆ$DM fluctuations from CDM subhalos. We demonstrate that ${\mathrm{P}}_{\hat{I}}´(k)$ can be measured directly from data by modeling the smooth lensing with a local Curved Arc Basis formalism. With realistic modeling systematics, we find a statistically significant separation between $\ddot{I}ˆ$DM and CDM across $1\lesssim k\lesssim 11{\mathrm{kpc}}^{-1}$ -- offering an independent probe of the wave-like nature of DM complementary to existing constraints.

19 pages