submitted

paper/paper.tex

@@ -613,7 +613,7 @@ \subsection{Multiphase ISM}
 These results certainly open up the path to future searches to
 construct new models.} 
 
-Qualitatively this result can be understood as follows.
+The results from this model can be qualitatively explained as follows.
 Due to the large fraction of \lya photons being emitted within the
 moving clumps ($P_{\rm cl}\sim 1$) the `intrinsic' profile closely follows 
 the clump kinematics. 
@@ -625,8 +625,8 @@ \subsection{Multiphase ISM}
 sight, $0.8<f_{\mathrm{cl}}<8$, combined with the high velocity dispersion
 of the clumps implies existence of low-density inter-clump 
 regions where \lya photons can freely propagate.
-This gives result to an emergent spectrum close to the intrinsic one, explaining the high
-flux at the line's center.  
+This gives result to an emergent spectrum close to the intrinsic one,
+explaining the high flux at the line's center.    
 
 Because the width of the observable spectrum is hence set primarily by
 $\sigma_{\rm cl}$, a lower velocity dispersion would produce a
@@ -720,11 +720,11 @@ \section{Discussion}
 These results disfavor the high rotational velocity of $V_{m}\sim350$
 \kms\  that we find in the pure rotation model. 
 On the other hand the results from the multiphase model yield a
-velocity dispersion $\sigma_{\rm cl}=$\sigmaclump, consistent with observed
-values in other CDGs, favoring the multiphase model.
-In this case we can  estimate a value for the dynamical
-mass using the constraints for the velocity dispersion, $\sigma$,  in
-a spherical system localized in a region of size $r$    
+velocity dispersion $\sigma_{\rm cl}=$\sigmaclump, consistent with
+other observations.
+We can now estimate a value for the dynamical mass using the
+constraints for the velocity dispersion, $\sigma$,  in a spherical
+system localized in a region of size $r$     
 
 \begin{equation}
 M_{\rm dyn} = 3 \frac{\sigma ^{2}r}{G} = 3.48\times10^{9}
@@ -734,12 +734,12 @@ \section{Discussion}
 
 Assuming that the \lya emission is entirely powered by star formation 
 we use the 3D half-light radius $r_s=2.25$ kpc as the typical size
-for the HI region and that  $\sigma=\sigma_{\rm{cl}}=$\sigmaclump, we
-obtain a dynamical mass of  $M_{\rm dyn}=2.31\pm0.04 \times 10^{9}$
-$M_{\odot}$, which is ten times the estimated baryonic mass in
-\tol. 
+for the HI region. 
+With $\sigma=\sigma_{\rm{cl}}=$\sigmaclump we obtain a dynamical mass
+of  $M_{\rm dyn}=2.31\pm0.04 \times 10^{9}$ $M_{\odot}$, which is ten
+times the estimated baryonic mass in \tol. 
 
-A larger dynamical mass estimate over its baryonic mass is a hint that
+A larger dynamical mass estimate over its baryonic mass hints that
 \tol\ is dark matter dominated.  
 Following the methodology of \citet{2011ApJ...726..108T} we estimate
 that a dark matter halo with a virial mass $\sim 6\times 10^{11}$

paper/referee.md

@@ -33,17 +33,17 @@ conclusions.
 Reply. The quoted values for the chi^2 are correct. The low
 statistical value means that the two distributions (observed and
 simulated) are indeed not the same. But we don't expect them to be the
-same because we don't expect reality to have the same simplified
+same because we don't expect this galaxy to have the same simplified
 description that we have in our models.
 
 The value of these fits does not lie on the basis of its statistical
 significance, but in it's ability to reproduce for the first time the
 broad features of the observed galaxy. Their value is in the
 physical insight they provide into the physical processes shaping the
-Lyalpha line.
+Lyalpha line. 
 
 This was succintly put by George Box when he wrote that "All models
-are wrong but some are useful", or in a more extended quote from him
+are wrong but some are useful", or in a more extended quote from him:
 "Now it would be very remarkable if any system existing in the real
 world could be exactly represented by any simple model. However,
 cunningly chosen parsimonious models often do provide remarkably
@@ -59,6 +59,9 @@ useful?"."
 
 (full source can be found in wikipedia https://en.wikipedia.org/wiki/All_models_are_wrong)
 
+In this context the chi^2 quantification is useful to decide between
+parameters within the same model or between different models.
+
 We have included a comment along these lines in the corresponding
 section. The conclusions and discussion remain unchanged.