Emulator validation described in the note
@@ -369,8 +369,6 @@ The allowed range of cosmological parameters is as follows:
%
Actually, $w_a$ and $w_0$ are constrained jointly to be $0.3\leq (-w_0-w_a)^{1/4}$. Note that \ccl only allows a subregion within this parameter space. For models in which w(z) crosses $-1$ at some given redshift, {\tt CLASS} will crash because this value corresponds to a true cosmological constant, which by definition should have no perturbations.\footnote{We thank Emilio Bellini and Miguel Zumalac\'arregui for clarifying this for us.} The linear matter power spectrum is still obtained from {\tt CLASS} as described in the section above.
-An automated check is in place which compares the \ccl emulator outputs for certain cosmologies to smoothed power spectra from the simulations presented in \citet{Lawrence17}.\footnote{Courtesy of Earl Lawrence and Katrin Heitmann.} The check ensures that the \ccl outputs when calling the emulator are within $3\%$ of the simulation benchmarks at $z=0$ and for the $k$ range of validity of the emulator. This essentially corresponds to a verification of the results presented in Figure 5 and Figure 6 of \citet{Lawrence17}.
-
\subsubsection{Spline parameters \& the INI file}
All spline and grid parameters relevant for computing quantities such as distances, growth functions, power spectra, and halo mass functions are defined in the {\tt ccl$\_$params.ini} file in the {\tt include} folder of the repository. This file allows the user to configure the following constants:
@@ -449,7 +447,7 @@ We have found that changing {\tt N$\_$A} to $200$, or changing the sampling of t
We plan to implement the following power spectrum methods in the future:
\begin{itemize}
\item CAMB,
- \item cosmic emulator for neutrino cosmologies,
+ \item other emulators,
\item Halo model/HOD.
\end{itemize}
@@ -917,6 +915,8 @@ Additionally, independent codes were utilized to test the accuracy of halo mass
\end{equation}
We note that while we maintain the $10^{-4}$ for our evaluations of $\sigma$, the accuracy degrades to a value of $5\times10^{-3}$ for the halo mass function evaluation, primarily at the high halo mass and high redshift domains. We find that this increased error is acceptable, as the level of precision is significantly better than the accuracy of current halo mass function models.
+The implementation of the matter power spectrum emulation code from \citet{Lawrence17} in \ccl has been validated at first instance by comparing the direct output of the original code to \ccl for the best fit cosmology (M000) in the range of wavenumbers spanned by the emulator predictions and confirming that the agreement is within the expectation from numerical errors (fractional difference of $<10^{-5}$). We have also compared the \ccl emulator outputs for certain cosmologies to smoothed power spectra from the simulations presented in \citet{Lawrence17}.\footnote{Courtesy of Earl Lawrence and Katrin Heitmann.} The check ensures that the \ccl outputs when calling the emulator are within $3\%$ of the simulation benchmarks at $z=0$ and for the $k$ range of validity of the emulator. This essentially corresponds to a verification of the results presented in Figure 5 and Figure 6 of \citet{Lawrence17}.
+
Finally, we note that formal tests for predictions in cosmologies with neutrinos are not yet included. The support for neutrino cosmologies in the current release is therefore not yet formally validated, although outputs have been informally compared against other codes where available. Formal validation of this functionality is ongoing.
\ccl has a suite of test routines which, upon compilation, compare its outputs to the benchmarks from code comparison. These are run with {\tt make check}.
