tokens: which was managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The fits had an average rms residual of 0.15 km s −1 and an average maximum residual of 0.3 km s −1 . Two observations have larger uncertainties. The signal-to-noise ratio (S/N) for the 814 cm −1 setting from 2007 was too low to use telluric lines in the GV Tau N spectrum. Instead, the dispersion function was fit to lines in the telluric standard (rms 0.06 km s −1 ), and this solution was applied to GV Tau N. Three measurable telluric lines in the GV Tau N spectrum were used to assign a zero-point (wavelength shift) uncertainty of 0.5 km s −1 . The 932 cm −1 setting from 2007 only contains three telluric lines; hence, an independent dispersion solution was not possible. In this case, the pipeline wavelength scale was retained, with an assumed uncertainty of 1 km s −1 . Model telluric transmission spectra were utilized for a few of the settings. Because the S/N for the 780 cm −1 setting was degraded as a result of insufficient S/N in the telluric calibrator, corrections for atmospheric lines were made using the software package TERRASPEC (Bender 2010 ). TERRASPEC was also used to improve the correction for telluric water lines in the 767 and 807 cm −1 settings. For all of the observations, additional continuum normalization was carried out for each order of interest by fitting a low-order polynomial to the continuum outside the intervals of absorption from known molecular transitions in GV Tau N. 3. Analysis In the TEXES spectra we detect numerous absorption lines of NH 3 , HCN, and C 2 H 2 ; a few lines of H 2 O in absorption; and H 2 in emission (Table 2 ). The H 2 emission from GV Tau was previously reported in Bitner et al. ( 2008 ) and is not discussed further here. Most of the HCN and C 2 H 2 lines were measured in 2006, with additional lines measured in 2007. The unexpected detection in 2006 of numerous NH 3 absorption lines was followed up in 2007 with grating settings that probed lower-energy NH 3 transitions. Weak absorption lines of water were also detected in the 2007 spectra. The entire set of pipeline-reduced spectra for GV Tau N is shown in Figure A1 . The positions and identifications of the detected lines are indicated. Table 2 All Lines Notes. a *: detection; x: nondetection; ...: not covered; t: telluric line; e: order edge/roll-off; u: high uncertainty; d: blended with other line. b ν 4 + ν 5 – ν 4 band, i.e., absorption out of the ν 4 level. c The 813.85 cm −1 ortho- and 813.83 cm −1 para-H 2 O lines were treated as a single line with combined g l . While the H 2 O lines are pure rotational transitions within the ground vibrational state, the NH 3 , HCN, and C 2 H 2 absorption lines are predominantly rovibrational transitions out of the ground vibrational state to a higher vibrational state; the C 2 H 2 ν 4 + ν 5 – ν 4 line is an exception (see Section 3.1 ). The HCN ν 2
ner_tags: O O O O O B-Organization I-Organization I-Organization I-Organization I-Organization I-Organization I-Organization B-Organization O O O O O O B-Organization I-Organization I-Organization O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O B-Software B-Citation I-Citation O B-Software O O O O O O O O O O O O O B-Wavelength O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject O O O O B-Instrument O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O