Top: an example 1D spectrum of a low-mass galaxy (﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\approx 8.3)﹩) in the EGS field. The blue shows the coadded spectrum of all 1D extractions, and the green shows the continuum-subtracted spectrum, though the observed difference between the two is small, as the estimated continuum (orange line) is quite small for such a low-mass galaxy. The redshift routine searched the continuum-subtracted spectrum for significant residual flux peaks in order to identify emission lines. The error spectrum is shown in purple, generally only visible when coinciding with stronger skylines, which are more common at the redder wavelengths. The vertical dotted red lines show common strong skylines that were excluded from the emission-line detections. Vertical dashed black lines show common strong emission lines (e.g., [O III]4959,5007; Hβ; [O II]3727,3729). Green vertical dashed lines show the locations of weak emission lines that may serve as metallicity indicators ([Ne III] and [O III]4363), and dashed blue lines indicate typically weak helium lines. Magenta dashed lines indicate the locations of the Ca H and K absorption lines, typically only seen in higher-mass galaxies with stronger continua and older stellar populations. Middle: an example spectrum for a high-mass galaxy (﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\approx 10.4)﹩) in EGS that nonetheless exhibits some indicators of star formation, with detectable [O II]3727,3729 emission and Hβ and Hγ Balmer lines. This galaxy lies outside primary CANDELS photometric coverage, and so lacks some photometric and color information. Bottom: another massive galaxy (log(M_⋆/M_⊙ ) ≈ 10.5)) in EGS that is quiescent, with no visible Balmer emission. This galaxy’s redshift is determined via the Ca H and K absorption lines.