Left: Near‐IR emission lines detected at Keck using the NIRSPEC instrument on UT 2005 March 17. The exposure time was 2400 s, and used the moderate resolution setting with a 0﹩\farcs﹩76 slit. To improve the signal‐to‐noise ratio, the spectrum is smoothed to 0.02 μm bins. Vertical lines denote the positions expected for Hα and the flanking [N II] lines at ﹩z=1.325﹩. Right: Keck‐DEIMOS spectra of MIPS J142824.0+352619, smoothed to highlight several absorption features which suggest the presence of a ﹩z=1.034\pm 0.002﹩ foreground galaxy. The thick line at 7400 Å denotes the divide between the red and blue arms on the spectrometer. The A‐ and B‐band telluric lines are denoted by the symbol ﹩\oplus ﹩. We also indicate where [O II] would appear at ﹩z=1.325﹩. Although this does appear to coincide with an emission line nearby, the difficulty in removing atmospheric lines at the red end renders it inconclusive.