We present new BVI ground-based photometry and VI space-based photometry for the globular cluster M92 ( NGC 6341 ) and examine luminosity functions in B , V , and I containing over 50,000 stars ranging from the tip of the red giant branch to several magnitudes below the main sequence turn off .
Once corrected for completeness , the observed luminosity functions agree very well with theoretical models and do not show stellar excesses in any region of the luminosity function .
Using reduced- \chi ^ { 2 } fitting , the new M92 luminosity function is shown to be an excellent match to the previously published luminosity function for M30 .
These points combine to establish that the “ subgiant excess ” found in previously published luminosity functions of Galactic globular clusters are due to deficiencies in the stellar models used at that time .
Using up to date stellar models results in good agreement between observations and theory .

Several statistical methods are presented to best determine the age of M92 .
These methods prove to be insensitive to the exact choice of metallicity within the published range .
Using [ Fe/H ] = -2.17 to match recent studies we find an age of 14.2 \pm 1.2 Gyr for the cluster .