\\ Species Tag:        &   17002 & Name:&  NH$_3$
\\ Version:            &       4 & & Ammonia hyperfine lines
\\ Date:       & Oct. 2009       & & GS, $\nu_2$ = 1
\\ Contributor:&  S. Yu, B. Drouin and J. Pearson & &
\\ Lines Listed:       &  110577 & Q(300.0)=&   1766.3358
\\ Freq. (GHz) $<$     &   39999 & Q(225.0)=&   1140.9789
\\ Max. J:             &      20 & Q(150.0)=&   623.7662
\\ LOGSTR0=            &   -20.0 & Q(75.00)=&   225.4150
\\ LOGSTR1=            &   -20.0 & Q(37.50)=&    84.0965
\\ Isotope Corr.:      &     0.0 & Q(18.75)=&    34.7977
\\ Egy. (cm$^{-1}$) $>$&     0.0 & Q(9.375)=&    17.2096
\\ $\mu_a$ = &                   & A=& 331411.77
\\ $\mu_b$ = &                   & B=& A
\\ $\mu_c$ = & 1.471932          & C=& 186836.77

\headend

The two inversion states of the ground state and the $\nu_2$ = 1 state are included in this analysis. The vibrational designations are as the following: 0 for $0^+$; 1 for $0^-$; 2 for $\nu_2^+$, 3 for $\nu_2^-$. Seven quanta were used to describe each level: J, K, V, F1, F2, I$_{tot}$, F (F1 = J + I$_N$; F = F1 + I$_{tot}$; F2 = 4 for K = 1, 4 or 7 etc.; F2 = 2 for K = 2, 5 or 8 etc.; F2 = 0 for K = 0, 3, 6 etc.)

The hyperfine lines in the ground state were reported by Kukolich, Phys. Rev. {\bf 156}, 83 (1967); Kukolich et al, J. Chem. Phys. {\bf 52}, 5477(1970); Kukolich et al, Phys. Rev. A {\bf 138}, 1323 (1965); Ruben et al, J. Chem. Phys. {\bf 61}, 3780 (1974); Cazzoli et al, Astron. Astrophys. 2009 (submitted). Both the N and H hyperfine splittings are resolved in these studies.

The hyperfine lines in the $\nu_2$ = 1 state were reported by Belov et al, J. Mol. Spectrosc. {\bf 189}, 1 (1998); Urban et al, J. Mol. Spectrosc. {\bf 2000}, 280 (2000); Fichoux et al, J. Mol. Spectrosc. {\bf 192}, 169 (1998). Only the N hyperfine splittings are resolved in these studies.

The microwave lines without hyperfine splittings were reported by Poynter et al, APJS {\bf 29}, 87 (1975); Belov et al, J. Mol. Spectrosc. {\bf 84}, 288 (1980); Minguzzi et al, J. Mol. Spectrosc. {\bf 96}, 294 (1982); Siemsen et al, Optics Lett. {\bf 10}, 594 (1985); Sasada et al, J. Mol. Spectrosc. {\bf 117}, 317 (1986);  Tanaka et al, Chem. Phys. Lett. {\bf 146}, 165 (1988); Winnewisser et al, Naturforsch. {\bf 51a}, 200 (1996); Belov et al, J. Mol. Spectrosc. {\bf 189}, 1 (1998); Chen et al, J. Mol. Spectrosc. {\bf 236}, 116 (2006);

The infrared and far-infrared lines without hyperfine splittings were reported by Freund and Oka, Phys Rev. A {\bf 13}, 2178 (1976); Laughton et al, J. Mol. Spectrosc. {\bf 62}, 263 (1976); Hillman et al, Optics Lett. {\bf 1}, 81 (1977);  Sattler et al, J. Mol. Spectrosc. {\bf 88}, 347 (1981); Shoja-Chagherv et al, J. Mol. Spectrosc. {\bf 97}, 287 (1983); Poynter and Margolis, Mol. Phys. {\bf 48}, 401 (1983); Urban et al, J. Mol. Spectrosc. {\bf 101}, 1 (1983); Poynter and Marglis, Mol. Phys. {\bf 51}, 393 (1984); Brown and Toth, J. Opt. Soc. Am. B {\bf 2}, 842 (1985); Hermanussen et al, J. Mol. Spectrosc. {\bf 119}, 291 (1986); Urban et al, J. Mol. Spectrosc. {\bf 118}, 298 (1986); Fusina et al, J. Mol. Spectrosc. {\bf 141}, 23 (1990); Chu et al, JQSRT {\bf 51}, 591 (1994); Fabian et al, J. Mol. Spectrosc. {\bf 173}, 591 (1995); Krupnov et al, J. Mol. Spectrosc. {\bf 176}, 442 (1996).

The rotational dipoles and their J and K dependences for both ground and $\nu_2$ = 1 state from Ueda and Iwahori (J. Mol. Spectrosc. {\bf 116} 191 (1986)) were used along with the $\nu_2$-band dipoles, and their Herman-Wallis constants reported by Fabian and Yamada (J. Mol. Spectrosc. {\bf 198} 191(1999)). 

The partition function includes contributions from the $\nu_2$ = 1 state and $J$ up to 20.  This entry is a prediction of ground state rotation-inversion transitions only.