Small change to description of neutrinos tests.
@@ -862,7 +862,7 @@ The accuracy of this approximation is shown in Figure \ref{fig:NLextrapol} for r
With the implementation described above, the power spectrum splines are initialized up to {\tt K$\_$MAX$\_$SPLINE}. This is also true for the linear matter power spectrum, which is used within \ccl in particular to obtain $\sigma_8$ (see Eq. \ref{eq:sigR}). We have tested how this procedure affects the convergence of the linear matter power spectrum. We compare the fiducial \ccl output to the case where we set {\tt K$\_$MAX$\_$SPLINE}~$=5\times 10^3/$Mpc. The result is shown in Figure \ref{fig:NLextrapol}. For some applications that use the linear power spectrum, the user might need to increase the value of {\tt K$\_$MAX$\_$SPLINE}. While \ccl adopts certain fiducial values of the number of scale factor and wavenumber values to use in the interpolation, we have tested that increasing the sampling does not change the results presented in Figures \ref{fig:NLextrapol}.
-In addition to the above tests in $\Lambda$CDM cosmologies without massive neutrinos, we have checked the impact of using splines at low and high $k$ in cosmologies CCL7, CCL8, and CCL9 with massive neutrinos, defined in Table \ref{tab:cosmologies_nu}. We compare the linear and nonlinear matter power spectrum as computed directly via {\tt CLASS} to that computed using {\tt CLASS} via \ccl (i.e. using splines at high and low k). We find that for $k$ between {\tt K$\_$MIN} and {\tt K$\_$MIN$\_$SPLINE}, the two power spectra agree to better than $10^{-4}$ in all models. For $k$ between {\tt K$\_$MAX$\_$SPLINE} and {\tt K$\_$MAX}, agreement is better than $10^{-3}$, which we deem sufficient given the significant uncertainties introduced at these small scales, e.g. baryonic effects. The fractional difference between the two power spectra is plotted in Figure \ref{fig:power_nu}. \todo{Are we okay with this? -DL}
+In addition to the above tests in $\Lambda$CDM cosmologies without massive neutrinos, we have checked the impact of using splines at low and high $k$ in cosmologies CCL7, CCL8, and CCL9 with massive neutrinos, defined in Table \ref{tab:cosmologies_nu}. We compare the linear and nonlinear matter power spectrum as computed directly via {\tt CLASS} to that computed using {\tt CLASS} via \ccl (i.e. using splines at high and low k). We find that for $k$ between {\tt K$\_$MIN} and {\tt K$\_$MIN$\_$SPLINE}, the two power spectra agree to better than $10^{-4}$ in all models. For $k$ between {\tt K$\_$MAX$\_$SPLINE} and {\tt K$\_$MAX}, agreement is better than $10^{-3}$, which we deem sufficient given the significant uncertainties introduced at these small scales, e.g. baryonic effects. The fractional difference between the two nonlinear power spectra is plotted in Figure \ref{fig:power_nu}; the test with linear power spectra yields very similar results. \todo{Are we okay with this? -DL}
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