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The authors find that the number of observed eclipsing binaries scales directly with the input frequency of short-period orbits. For example although typically less than 1\% of eclipsing FG systems show 1.5 mag eclipses, the ratio at the shortest periods is closer to 20\%. The situation is more complex for higher mass sytems although the authors find humps with high probability of deep eclipses at about 2 day and 0.4 day orbital periods.   \paragraph{}     Along the main sequence, the authors also find no significant difference between their parallel S+S binaries and the full BSE run as long as there is no mass-transfer between the components. However there are difference in oribital evolution when a large fraction of mass is lost in the giant stage. In general, going up the main sequence, the differences between S+S and the BSE code increase and only BSE can create deeply eclipsing Algol systems.   \paragraph{}   Because the authors assume that most eclipsing binaries with periods in the 0.2 to 20 day range and eclipse-depths greater than 0.1 magnitude were detected by Hipparcos photometry they performed a crude comparison at galactic latitudes lower than 30 degrees. They found reasonable agreement although the software predicted more short-period pairs than were observed by Hipparcos.