Of the 9096 visible stars -- 90% are how close? I was on a beach on a tropical island one night and, of course, the night sky was magnificent. It got me thinking: 

I want to point to a star and say with $90$% certainty that it is probably $x$ light-years away. What should be $x$?

In other words, in this Sky and Telescope list of 9096 stars, $90$% are within how many light-years?
P.S. I had hoped that the answer would be in the post Demographics of stars visible to the naked eye, but it was not.
 A: Here is an update on (my) answer that your refer to. I have changed the visual threshold to V<6.5 mag (which is what Sky and Telescope have done) and I have used the revised Hipparcos reduction from van Leeuwen (2007) (catalogue available here) to obtain a (almost) complete catalogue of stars with their trigonometric parallaxes. It contains 7892 stars. I am not going to investigate the discrepancy with the Sky and Telecope article which uses the Hoffleit & Jaschek bright star catalogue as their reference.
The distribution of distances is illustrated in the two plots below (labelled in light years, as you wish). The first shows the number of stars as a function of distance. The second shows the cumulative fraction of stars closer than some distance. From this, you can read off, or I can tell you, that 90% of bright stars in the Hipparcos catalogue are closer than  1175 light years.
NB: I don't think 4 significant figures are warranted. There are some tens of bright stars that are so distant that their parallaxes are too small and are garbage (negative in some cases). I'm also not clear about what the status of binary stars are (you can't resolve them, but in many cases Hipparcos could)
 
Number of bright stars versus distance



Normalised cumulative frequency of star distance
A: The post you reference gives the distribution of distances as a histogram. It is based on 6000 visible stars, but it is still basically the answer you want. The peak is at $10^2 = 100$ parsecs. 90% of the stars look to be between $10^{1.5} \approx 30$ and $10^{2.5} \approx 300$ parsecs. 
