Group d is from 2013-09-30 to 2014-11-17, and represents a new detector and detector electronics installed in the APOLLO apparatus. This group should be appended to the latest versions of groups a, b, and c (note the update to c). We recommend using different range biases for the four sets, labeled a, b, c, and d. Each group should acquire a different bias. We also have explored error scalings, and believe that scaling our statistical uncertainties (as represented in the normal point files) could be accomplished by one of the following choices: Group factor for scaling OR RSS term a 2.0 17 ps b 6.0 60 ps c 2.5 20 ps d 1.0 0 ps Thus the point: 5120101030123810000000024392228766593170610236 141648B 73152 8948 5320A 251A which has a reported uncertainty of 14.1 ps would become 28.2 ps under scaling, or 22.1 ps if applying the RSS value. Batch data reduction using: Common treatment: threshhold = 1 (excluding all shots with > 1 photon received) no first photon bias no DAC correction 10 ps RSS term to account for DAC channel offsets applied throughout, based on windowed time periods Different treatment: Group b uses the lun-fid correlation technique to form normal points. Groups a, c, and d use a functional fit method, except in cases where the fit failed, in which case the correlation technique was substituted. An extensive comparison between the two techniques revealed no net bias, at the few picosecond level.