  We reanalyze the multi-epoch direct detections of HD 88133 b and ups And b
that were published in Piskorz et al. 2016 and Piskorz et al. 2017,
respectively. Using simulations to attempt to reproduce the detections, we find
that with the 6 and 7 $L$ band Keck/NIRSPEC epochs analyzed in the original
works, the planets would not have been detectable unless they had unreasonably
large radii. HD88133 and ups And both have fairly large stellar radii, which
contributed to the difficulty in detecting the planets. We take this
opportunity to consider how these planets may have been detectable with the
small number of epochs originally presented by running simulations both with
the upgraded NIRSPEC instrument and with near-zero primary velocities, as
recommended by Buzard et al. 2021. While 7 $L$ band NIRSPEC2.0 epochs with
near-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 been
required for a strong detection of HD88133b, which could be due in part to both
this system's large stellar radius and low stellar temperature. This work
stresses the importance of careful analytic procedures and the usefulness of
simulations in understanding the expected sensitivity of high-resolution
spectroscopic data.
