Abstract
We show how the temperature and the polarization of the cosmic microwave background are affected by bulk rotation of clusters of galaxies owing to the kinetic Sunyaev-Zeldovich effect. The main effects of rotation are (i) a shift of the position of the peak of the temperature fluctuation relative to the center of the cluster by a few percent of the core radius and (ii) a tilt of the direction of the plane of linear polarization by several degrees.
Highlights
Several effects lead to anisotropies of the cosmic microwave background (CMB): primary effects, imprinted on the surface of last scattering, and secondary effects, arising after hydrogenrecombination or after reionization has taken place.Among the secondary effects, the thermal SunyaevZeldovich effect, which is due to inverse Compton scattering of the CMB photons off the hot intracluster medium (ICM) (Zeldovich & Sunyaev 1969), and the kinetic SunyaevZeldovich effect (k-SZE), which arises from the peculiar motion of the cluster in the rest frame of the CMB (Sunyaev & Zeldovich 1980), are most important
The thermal SunyaevZeldovich effect, which is due to inverse Compton scattering of the CMB photons off the hot intracluster medium (ICM) (Zeldovich & Sunyaev 1969), and the kinetic SunyaevZeldovich effect (k-SZE), which arises from the peculiar motion of the cluster in the rest frame of the CMB (Sunyaev & Zeldovich 1980), are most important
Kinetic Sunyaev-Zeldovich effect from cluster rotation In Fig. 1 the relative change of intensity of the CMB due to the rotational kinetic Sunyaev-Zeldovich effect (rk-SZE) is shown for an edge on (i = π/2) view of an oblate cluster (ι = 1.1) with a cutoff radius R = 10 rc and γ = 1.125 corresponding to β = 3/4
Summary
Several effects lead to anisotropies of the cosmic microwave background (CMB): primary effects, imprinted on the surface of last scattering, and secondary effects, arising after hydrogenrecombination or after reionization has taken place (for references see White & Cohn 2002). In their work the rk-SZE was discussed for a gas density profile following from hydrostatic equilibrium of the gas in the Navarro-Frenk-White dark matter density field within a halo (Navarro et al 1996; Makino et al 1998). Assuming isothermality this gas density profile is very well approximated by the commonly used isothermal β-model (Cavaliere & Fusco-Femiano 1976), which is better applicable to analytical calculations. 2 we state the model assumptions for the rotating cluster of galaxies and derive analytic formulae describing the rk-SZE.
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