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APOGEE has amassed the largest ever collection of multi-epoch,high-resolution (R~22,500), H-band spectra for B-type emission line (Be) stars.The 128/238 APOGEE Be stars for which emission had never previously beenreported serve to increase the total number of known Be stars by ~6%. We focuson identification of the H-band lines and analysis of the emission peakvelocity separations (v_p) and emission peak intensity ratios (V/R) of theusually double-peaked H I and non-hydrogen emission lines. H I Br11 emission isfound to preferentially form in the circumstellar disks at an average distanceof ~2.2 stellar radii. Increasing v_p toward the weaker Br12--Br20 linessuggests these lines are formed interior to Br11. By contrast, the observed IRFe II emission lines present evidence of having significantly larger formationradii; distinctive phase lags between IR Fe II and H I Brackett emission linesfurther supports that these species arise from different radii in Be disks.Several emission lines have been identified for the first time including~16895, a prominent feature in the spectra for almost a fifth of the sampleand, as inferred from relatively large v_p compared to the Br11-Br20, a tracerof the inner regions of Be disks. Unlike the typical metallic lines observedfor Be stars in the optical, the H-band metallic lines, such as Fe II 16878,never exhibit any evidence of shell absorption, even when the H I lines areclearly shell-dominated. The first known example of a quasi-triple-peaked Br11line profile is reported for HD 253659, one of several stars exhibiting intra-and/or extra-species V/R and radial velocity variation within individualspectra. Br11 profiles are presented for all discussed stars, as are fullAPOGEE spectra for a portion of the sample.

High-resolution, H band Spectroscopy of Be Stars with SDSS-III/APOGEE: I. New Be Stars, Line Identifications, and Line Profiles