I Fourier transform of the density fluctuation

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The discussion centers on the Fourier transform of density fluctuations in cosmology, specifically the equation governing the evolution of these fluctuations. The equation presented is a second-order differential equation that describes the dynamics of the density fluctuation, δ, in terms of the scale factor H and matter density Ω_m. The Fourier transform of the density fluctuation is defined, leading to a similar differential equation for δ_k, the Fourier-transformed fluctuation. The participants express confusion about the solution to this equation, suggesting that a Gaussian function may be the only viable solution. The textbook referenced is "Introduction to Cosmology" by Barbara Ryden, which provides the relevant equations and context.
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Computing the Fourier transform of the density fluctuation.
There is a Fourier transform that I don't really understand in my textbook.

I have the following equation:
##\ddot{\delta} + 2H\dot{\delta} -\frac{3}{2} \Omega_m H^2 \delta = 0##

Then using the Fourier transform:
##\delta_{\vec{k}} = \frac{1}{V} \int \delta(\vec{r}) e^{i \vec{k} \cdot \vec{r}} d^3 r##

Where ##\delta(\vec{r})## is the density fluctuation.

We get
##\ddot{\delta_{\vec{k}}} + 2H\dot{\delta_{\vec{k}}} -\frac{3}{2} \Omega_m H^2 \delta_{\vec{k}} = 0##


The only function that does that is a gaussian function, I guess. I don't understand the process here.

Thank you
 
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PeterDonis said:
Which textbook?
Introduction to Cosmology second edition by Barbara Ryden (p.215-219)
 
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https://en.wikipedia.org/wiki/Recombination_(cosmology) Was a matter density right after the decoupling low enough to consider the vacuum as the actual vacuum, and not the medium through which the light propagates with the speed lower than ##({\epsilon_0\mu_0})^{-1/2}##? I'm asking this in context of the calculation of the observable universe radius, where the time integral of the inverse of the scale factor is multiplied by the constant speed of light ##c##.

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