Constraining axion stimulated emission using the CMB power spectra measurements and the interplay with current CMB constraints on the reionization epo

我的目标是约束轴子的受激发射的CMB功率谱使用宇宙学玻尔兹曼代码，CLASS，并比较普朗克的测量，以约束允许的参数空间的轴子受激发射使用马尔可夫链-蒙特-卡罗分析代码，MontePython。轴子的受激发射提供了额外的能量来源，可以重新加热，激发或加热星系际介质（IGM）。任何注入IGM的能量源都可能导致产生更多的电子，这增加了CMB光子和电子通过汤姆逊散射相互作用的可能性。这导致了CMB各向异性的整体阻尼，更具体地说，偏振（EE）CMB功率spectrum.The再电离光学深度从CMB偏振光谱获得有利于再电离在更高的红移比什么是约束的Gunn-Peterson槽的类星体在z~6的测量。这可能会在早期星星形成的再电离时代的当前模型和来自轴子的额外再电离源之间呈现出有趣的相互作用。我目前正在比较轴子受激发射的光学深度和普朗克从CMB EE功率谱测量得出的光学深度。由此，我应该能够从再电离光学深度的边界导出允许的参数空间。我也在调查，如果有一个红移依赖于能量注入一个给定的光学深度的EE功率谱将改变。这个练习将有助于确定我是否需要在分析中使用CLASS和Montepython。

I aim to constrain the stimulated emission of axions from the CMB power spectra using a cosmological Boltzmann code, CLASS, and comparing to the measurements made by Planck in order to constrain the allowed parameter space for axion stimulated emission using the Markov-Chain-Monte-Carlo analysis code, MontePython. The stimulated emission of axions provides an additional source of energy that can reheat, excite or ionize the Intergalactic Medium (IGM). Any source of energy injection into the IGM could lead to the production of more electrons, which increases the probability of the CMB photons and electrons interacting via Thomson Scattering. This leads to an overall dampening of the CMB anisotropies and more specifically, the polarization (EE) CMB power spectrum.The reionization optical depth obtained from the CMB polarization spectra favours reionization at higher redshifts than what is constrained by the measurement of the Gunn-Peterson trough of a Quasar at z~6. This could present an interesting interplay between the current model of the reionization epoch from early star formation and additional reionization sources from axions. I am currently comparing the optical depth from axion stimulated emission to the optical depth derived from the CMB EE power spectra measurements by Planck. From this, I should be able to derive the allowed parameter space derived from the bound on the reionization optical depth. I am also investigating if the EE power spectrum will change if there is a redshift dependence on the energy injection for a given optical depth. This exercise will help to determine if I need to use CLASS and MontePython in the analysis.