Rees-Sciama signatures from evolving dark matter halos in the cosmic microwave background

Photons in the cosmic microwave background (CMB) radiation receive an extra blueshift in their energies as they traverse slowly-growing dark matter halos. This Rees-Sciama effect arises from the time-dependent gravitational potentials generated by the subsequent accretion of dark matter flows onto collapsed halo cores. Studies of the Rees-Sciama contributions to the stochastic anisotropies in the CMB from large scale linear or quasi-linear perturbations have been previously conducted, but in this work we focus on non-perturbative, collapsed halos. We calculate the magnitude of this effect for a spherical symmetric halo model of self-similarity, and demonstrate a projected profile of this signature on the sky as a function of the impact parameter of the line of sight. Its typical angular size is larger than that of the halo's virialized core, which provides a possible avenue to separate Rees-Sciama signatures from scattering signatures of Sunyaev-Zeldovich effects. We argue that this effect can be potentially utilized not only to probe the dynamics of dark matter halos, but also to measure cosmological parameters such as $H(z)$ and $\Omega_{\Lambda}(z)$.