HRS CCDs, distributed in 73 spectral orders. This configuration provides a large number of these features from which we derive precise radial velocities. The HET queue-based observing mode allows for the spectrograph configuration to change multiple times throughout a single night as targeting requests from different observers are carried out. Standard sequences of calibration frames, including *biases*, *flats*, and *ThAr* wavelength references, are typically obtained at the end of the observing session. The echelle and cross-disperser positions are not precisely repeatable at the sub-pixel level, so the standard HET operations introduce a discontinuity between the *target* and the *ThAr* observations, which can result in RV shifts of several hundred m s$^{-1}$. To avoid this, we obtain additional *ThAr* frames immediately before or after each target observation, without altering the instrument configuration. We do not obtain extra *flats* because the telescope overhead would be severe and our experience has shown that the misalignment inherent in the standard queue procedures is usually small enough to prevent fringing in reduced images.

To efficiently and uniformly reduce the large HRS data set generated by our [*Kepler*]{} EB program, we created a semi-automated data handling pipeline for the HRS. This pipeline is written in the 