Abstract
We investigate the imprint of dark energy on the kinetic Sunyaev–Zel'dovich (kSZ) angular power spectrum on scales of ℓ=1000 to 10000, and find that the kSZ signal is sensitive to the dark energy parameter. For example, varying the constant w by 20% around w=−1 results in a ≳10% change on the kSZ spectrum; changing the dark energy dynamics parametrized by wa by ±0.5, a 30% change on the kSZ spectrum is expected. We discuss the observational aspects and develop a fitting formula for the kSZ power spectrum. Finally, we discuss how the precise modeling of the post-reionization signal would help the constraints on patchy reionization signal, which is crucial for measuring the duration of reionization.
Highlights
Dark energy (DE), the energy source that drives our Universe accelerating, has remained a mystery since it was discovered in 1998 [1,2]
The nature of dark energy is a mystery in modern cosmology, and its property is characterized by its equation of state (EoS) parameter
Current CMB space-mission such as WMAP and Planck, ground-based CMB experiments such as Atacama Cosmology Telescope (ACT) and South Pole Telescope (SPT), as well as baryon acoustic oscillation experiments from SDSS can set up tight constraints on w parameter if assuming that w is a constant
Summary
Dark energy (DE), the energy source that drives our Universe accelerating, has remained a mystery since it was discovered in 1998 [1,2]. In models of inhomogeneous reionization (or “patchy reionization”), where different regions of the Universe were ionized at different times, the bulk motion of bubbles of free electrons around the UV emitting sources may cause the temperature anisotropy on the CMB [15,16,17,18,21,22,23,24] It has been demonstrated [23,21] that the magnitude of the kSZ power from patchy reionization is related to the duration of reionization. Providing such an investigation on how much dark energy effect on kSZ signal is the main aim of this paper Such detail modeling of post-reionization signal is meaningful as more precise CMB observations are measuring the arcmin scale fluctuations. This set of parameter was derived using a joint dataset of WMAP9 + SPT + ACT + BAO + H0 [3]
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