Re-analysis of the ╣ of NH3 in C/2002 LINEAR T7 Using CSHELL at the NASA IRTF

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NH3 is the dominant (observable) nitrogen-containing volatile in comets, present at 1% relative to water. At infrared wavelengths, NH3 (ν1 band) is difficult to detect since it requires a significant geocentric velocity to shift the strongest NH3 emissions (Q-branch) out of the terrestrial atmospheric water absorption. The P- and R- branches are less dependent on geocentric velocity, but since they are generally weaker lines, they are challenging to detect. The 3-micron region is rich in molecular emissions (HCN, OH, H2O, C2H2, NH2, and other minor species), so that for many lines of the P- and R- branches, the ability to resolve these faint emissions from nearby brighter emission lines requires careful spectral registration of images.
Previously, we applied and tested our model of fluorescence efficiency factors for NH3 in C/2002 T7 (LINEAR). The high Doppler shift (- 66 km/s) of C/T7 during early May 2004 made it an excellent target for searching for NH3 through its strongest IR emission lines. While the Q-branch lines were detected with high signal to noise, the sQ33 line of NH3 was on the wing of a deep atmospheric absorption. Other lines were fainter and near brighter emissions or atmospheric absorptions.
The ability to accurately use the sQ33 emission and P- and R-branch lines, we discovered that our atmospheric model and algorithms needed improvement. Upgrades to our algorithms include an improved spectral transmittance model and spectral registration routines (Villanueva et al. 2006). This work will present a re-analysis of the 3-micron region from the high quality data set of C/2002 LINEAR T7 using the improved atmospheric transmittance models and data analysis algorithms from Villanueva et al.
KM-S would like to acknowledge support from the National Science Foundation RUI Program No. 0407052.

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