MI volunteers
+
%
\RequirePackage{docswitch}
\setjournal{\flag}
@@ -135,7 +136,7 @@ and $a(\chi)$, the inverse of $\chi(a)$.
%-------------------------------------------------------------------------------
\subsection{Growth of perturbations}
-\vol{?}
+\vol{Mustapha Ishak}
To compute the growth function, $D(a)$, the growth factor of matter perturbations, \ccl solves the following differential equation:
\begin{equation}
@@ -394,8 +395,8 @@ where $h_{\rm P}$ is Planck's constant and $h$ is $H_0/100$ with $H_0$ in units
\section{Implementation of high-accuracy cosmological functions}
%-------------------------------------------------------------------------------
-\subsection{Background functions}
-\vol{?}
+\subsection{Background functions \& growth of perturbations}
+\vol{Mustapha Ishak}
\cont{Initial conditions. Normalization. Units and sensitivity to physical constants (G, c etc).}
@@ -403,6 +404,7 @@ Including/excluding radiation in the computation of the comoving distances and t
The value of the gravitational constant, $G$, enters into the critical density. We found that failure to define $G$ with sufficient precision would result in lack of convergence at the $10^{-4}$ level between the different submissions. Importantly, note that CAMB barely has $10^{-4}$ precision in $G$ (and similarly, there might be other constants within CAMB/CLASS for which one should check the precision level). For \ccl, we are using the value from the Particle Physics Handbook.
+
%-------------------------------------------------------------------------------
\subsection{Matter power spectrum}
\vol{Elisa Chisari, who else?}
