We present F555W ( V ) , F439W ( B ) , and F336W ( U ) photometry of 9507 stars in the central 2 ^ { \prime } of the dense , post core collapse cluster M30 ( NGC 7099 ) derived from Hubble Space Telescope Wide Field/Planetary Camera 2 images . These data are used to study the mix of stellar populations in the central region of the cluster . Forty eight blue straggler stars are identified ; they are found to be strongly concentrated towards the cluster center . The specific frequency of blue stragglers , F _ { BSS } \equiv { N } ( { BSS } ) / N ( V < V _ { HB } +2 ) , is 0.25 \pm 0.05 in the inner region of M30 ( r < 20 ^ { \prime \prime } ) , significantly higher than the frequency found in other clusters : F _ { BSS } = 0.05 \ > – \ > 0.15 . The shape of M30 ’ s blue straggler luminosity function resembles the prediction of the collisional formation model and is inconsistent with the binary merger model , of Bailyn & Pinsonneault ( 1995 , ApJ , 439 , 705 ) . An unusually blue star ( B = 18.6 , B - V = -0.97 ) , possibly a cataclysmic variable based on its color , is found about 1 \farcs 2 from the crowded cluster center . Bright red giant stars ( B < 16.6 ) appear to be depleted by a factor of 2–3 in the inner r < 10 ^ { \prime \prime } relative to fainter giants , subgiants , and main sequence turnoff stars ( 95 % significance ) . We confirm that there is a radial gradient in the color of the overall cluster light , going from B - V \sim 0.82 at r \sim 1 ^ { \prime } to B - V \sim 0.45 in the central 10 ^ { \prime \prime } . The central depletion of the bright red giants is responsible for about half of the observed color gradient ; the rest of the gradient is caused by the relative underabundance of faint red main sequence stars near the cluster center ( presumably a result of mass segregation ) . The luminosity function of M30 ’ s evolved stars does not match the luminosity function shape derived from standard stellar evolutionary models : the ratio of the number of bright giants to the number of turnoff stars in the cluster is 30 % higher than predicted by the model ( 3.8 \sigma effect ) , roughly independent of red giant brightness over the range M _ { V } = -2 to +2 .