\\ Species Tag:        &   19004 & Name:&  H$_3$O$^+$
\\ Version:            &       2 & & Hydronium ion,
\\ Date:       & Nov. 2008       & & GS, $\nu_2$ = 1
\\ Contributor:&  S. Yu & &
\\             &  B. J. Drouin & &
\\ Lines Listed:       &     304 & Q(300.0)=&   520.1678
\\ Freq. (GHz) $<$     &   10000 & Q(225.0)=&   326.8681
\\ Max. J:             &      20 & Q(150.0)=&   174.0742
\\ LOGSTR0=            &    -5.0 & Q(75.00)=&    62.5579
\\ LOGSTR1=            &    -5.0 & Q(37.50)=&    26.6647
\\ Isotope Corr.:      &     0.0 & Q(18.75)=&    15.9161
\\ Egy. (cm$^{-1}$) $>$&     0.0 & Q(9.375)=&    11.6139
\\ $\mu_a$ = &                   & A=& 331411.77
\\ $\mu_b$ = &                   & B=& A
\\ $\mu_c$ = & 1.438             & C=& 186836.77

\headend

The two inversion states of the ground state, $\nu_1$ = 1, $\nu_2$ = 1, $\nu_3$ = 1, $\nu_4$ = 1 states  are included in this calculation.
The vibrational designations are as the following: 00 for $0^-$; 01 for $0^+$; 02 for $\nu_2^-$, 03 for $\nu_2^+$, 04 for $\nu_1^-$, 05 for 
$\nu_1^+$, 06 for $\nu_3^-$, $l$ = 1; 07 for $\nu_3^-$, $l$ = -1; 08 for $\nu_3^+$, $l$ = 1; 09 for $\nu_3^+$, $l$ = -1; 10 for $\nu_4^-$, 
$l$ = 1; 11 for $\nu_4^-$, $l$ = -1; 12 for $\nu_4^+$, $l$ = 1; 13 for $\nu_4^+$, $l$ = -1; The experimental measurements were reported by 
Plummer et al., 1985, J. Chem.\ Phys.\ {\bf 83}, 1428; Bogey et al., 1985, Astron.\ Astrophys.\ {\bf 148}, L11; Verhoeve et al., 1988, 
Chem.\ Phys.\ Lett., {\bf 143}, 501; Verhoeve et al., 1989, Chem. Phys. Lett., {\bf 161}, 195; Liu and Oka, 1985, Phys.\ Rev.\ Lett.\ {\bf 
54}, 1787; Liu et al., 1985, J. Chem.\ Phys.\ {\bf 82}, 5368; Liu et al.,1986, J. Chem. Phys., {\bf 84}, 1312; Davies et al., 1985, J. Opt. 
Soc. Am. B, {\bf 2}, 794; Haese and Oka, 1984, J. Chem. Phys., {\bf 80 }, 572; Lemoine and Destombes, 1984, Chem. Phys. Lett., {\bf 111}, 
284; Zheng et al., 2007, Chin. Phys. Lett., {\bf 24}, 2569; Tang and Oka, 1999, J. Mol. Spectrosc., {\bf 196}, 120; Stahn et al., 1987, Mol. 
Phys. {\bf 60}, 121; Ho al., 1991, J. Mol. Spectrosc., {\bf 149}, 530; Gruebele et al., 1987 J. Chem. Phys., {\bf 87}, 3347; Yu et al., 
2008, Astrophys. J. Supp. (in press).


The dipole moments for the inversion transitions, $\nu_1$ and $\nu_2$ were taken from the results from Botschwina et al. 1984, Chem.\ Phys.\ 
Lett.\ {\bf 102}, 299; the dipole moments for $\nu_3$ and $\nu_4$ are not available and were estimated based on the available infrared 
intensity ratios (Colvin et al. 1983, J.\ Chem.\ Phys.\ {\bf 79}, 1551 ) with the assumption that infrared intensities are proportional to 
the square of dipole moments.