Minor changes, fix one equation, removed boldface comment
@@ -264,7 +264,7 @@ This is a list of some power spectrum methods that we would like to implement in
\subsubsection{Normalization of the power spectrum}
\label{sec:PSnorm}
-There are two alternative schemes for normalization of the matter power spectrum. The first one is to specify the value of $A_s$, the amplitude of the primordial power spectrum, which is passed directly to {\tt CLASS}. This option is available in the case of the linear/nonlinear matter power spectrum implementation. For these, as well as for BBKS, there is the additional option to set the normalization of the matter power spectrum by specifying $\sigma_8$, the RMS density constrast averaged over spheres of radius $8h^{-1}$Mpc. {\bf make sure we document how to use each option.} The computation of $\sigma_8$ is described in Section \ref{sec:hmf}
+There are two alternative schemes for normalization of the matter power spectrum. The first one is to specify the value of $A_s$, the amplitude of the primordial power spectrum, which is passed directly to {\tt CLASS}. This option is available in the case of the linear/nonlinear matter power spectrum implementation. For these, as well as for BBKS, there is the additional option to set the normalization of the matter power spectrum by specifying $\sigma_8$, the RMS density constrast averaged over spheres of radius $8h^{-1}$Mpc. The computation of $\sigma_8$ is described in Section \ref{sec:hmf}
\subsection{Angular power spectra}
\label{sec:cl}
@@ -422,7 +422,7 @@ This function is directly implemented in {\tt CCL} as well as a specific $\sigma
The \citet{Tinker2010} model parameterizes both the halo mass function and the halo bias in terms of the peak height, $\nu = \delta_c / \sigma(M)$, where $\delta_c$ is the critical density for collapse and is chosen to be $1.686$ for this particular parameterization. We can then parameterize the halo function and halo bias as
\begin{equation}
\b(\nu) = 1 - A\frac{\nu^a}{\nu^a + {\delta_c}^a} + B\nu^b+C\nu^c,
- \f(\nu) = \alpha[1+(\beta\nu)^{-2\phi}]\nu^{2\eta}e(-\gamma\nu^2/2).
+ f(\nu) = \alpha[1+(\beta\nu)^{-2\phi}]\nu^{2\eta}e(-\gamma\nu^2/2).
\end{equation}
The currently implemented model in {\tt CCL} does not account for changes in halo definition, though this remains an area of active work to improve upon.
