deletions | additions       diff --git a/In_fact_Figrefhrdvel_provides.tex b/In_fact_Figrefhrdvel_provides.tex  index 7e3ebc5..4da8360 100644  --- a/In_fact_Figrefhrdvel_provides.tex  +++ b/In_fact_Figrefhrdvel_provides.tex 
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As the latter trends toward the upper right corner of the   HR diagram for lower metallicity, the metallicity dependence is also confirmed  by the empirical data.   Interestingly, they found significant microturbulent velocities (i.e., clearly above 5$\kms$) in the mass  range 7...11$\mso$ for stars with a relative age on the main sequence of $t/\tau_{\rm MS} > 0.8$,  and in the range 12...19$\mso$ for $t/\tau_{\rm MS} > 0.25$, but only insignificant  microturbulent velocities for younger or less massive stars.   Again, these results appear to agree with Fig.~\ref{fig:hrdvel} up to a remarkable   quantitative level.   In summary, our comparison provides evidence for a physical connection   of microturbulence in hot star photospheres with the existence and strength of a sub-photospheric  FeCZ.