http://arxiv.org/abs/2202.04091
Current and upcoming high angular resolution and multi-frequency experiments are well poised to explore the rich landscape of secondary CMB anisotropies. In this context, we compute for the first time, the power spectrum of CMB fluctuations from plasma in a cosmological distribution of evolving lobes of giant radio galaxies. We, also, explicitly take into account the non-thermal electron distribution, as opposed to thermal distribution, which has important implications for the inference of the CMB angular power spectrum. The relativistic particles are fed from the central supermassive blackholes via radio jets leading to radio lobes expanding to megaparsec scales into the intergalactic medium. Using a model of radio galaxy, we model the energetics and the pressure of the non-thermal electrons. We calculate the mean global non-thermal y-distortion, \ynt. For observationally reasonable distribution of the jet luminosities in the range of $10^{45}-10^{47}$ ergs$^{-1}$, we find \ynt to be less than $10^{-5}$, and hence not violating the COBE limit as previously claimed. Using the unique spectral dependence of the non-thermal SZ, we show that a detection of \ynt can be within reach at the level of $\gtrsim 5\sigma$ from a future PIXIE-like experiment. The total non-thermal SZ power spectrum, $C^{NT}\ell$, from the radio lobes is shown to peak at $\ell \sim 3000$ with an amplitude $\sim 1\%$ of thermal SZ power spectrum from galaxy clusters, and is also within the reach for a PIXIE like experiment. Finally, we show that a detection of the $C^{NT}\ell$ with a PIXIE-like experiment can lead to $\sim 5\sigma$ constraint on the mass dependence of the jet luminosity with the constraint becoming, at least, ten times better for the proposed more ambitious CMB-HD survey. This will, further, lead to the tightest constraint on the central black hole mass -to- host halo mass scaling relations.
S. Acharya, S. Majumdar and B. Nath
Thu, 10 Feb 22
41/66
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