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We reanalyze the multi-epoch direct detections of HD 88133 b and ups And bthat were published in Piskorz et al. 2016 and Piskorz et al. 2017,respectively. Using simulations to attempt to reproduce the detections, we findthat with the 6 and 7 $L$ band Keck/NIRSPEC epochs analyzed in the originalworks, the planets would not have been detectable unless they had unreasonablylarge radii. HD88133 and ups And both have fairly large stellar radii, whichcontributed to the difficulty in detecting the planets. We take thisopportunity to consider how these planets may have been detectable with thesmall number of epochs originally presented by running simulations both withthe upgraded NIRSPEC instrument and with near-zero primary velocities, asrecommended by Buzard et al. 2021. While 7 $L$ band NIRSPEC2.0 epochs withnear-zero primary velocities would have allowed a strong ($10.8\sigma$)detection of ups And b, many more than 6 $L$ band epochs would have beenrequired for a strong detection of HD88133b, which could be due in part to boththis system's large stellar radius and low stellar temperature. This workstresses the importance of careful analytic procedures and the usefulness ofsimulations in understanding the expected sensitivity of high-resolutionspectroscopic data.

Reinvestigation of the Multi-Epoch Direct Detections of HD 88133 b and Upsilon Andromedae b