removed before aperture extraction. Spectra were extracted with variance weighting (to reduce cosmic ray contamination), and wavelength calibrated using a standard thorium-argon lamp. The telluric standards were reduced by the same methods, and divided into the science spectra to remove atmospheric features. The sky fibre on the HRS was not used because our science targets are quite bright.

Samples of the final spectra are shown in Fig. \[fig:mgspectra\]. Radial velocities were calculated using the IRAF task *fxcor*, and cross-correlating the heliocentric-corrected spectrum of Arcturus [@b26]. These values are listed in Table \[table:obs\]. The velocities in NGC 5466 are in excellent agreement with those calculated per star by [@b21] this cluster shows a significant dispersion (Shetrone et al. 2012 finds a velocity dispersion of $\sim$17 km/s from 67 stars).

Post-pipeline processed APOGEE spectra are available in the SDSS DR10 database, where they have been reduced and coadded when multiple exposures were taken, and then continuum normalized. We took and additional step and shifted these spectra from the vacuum rest frame to the air rest frame.

![Sample spectral regions in the optical (blue chip, top), and infrared (bottom) showing magnesium, scandium, and iron lines that were used in the abundance analysis.[]{data-label="fig:mgspectra"}](opticalspectra.pdf "fig:"){width="50.00000%"} 