\\ Species Tag:        &   18005 & Name:&  H2O           
\\ Version:            &       4 & & Water
\\ Date:       &  Nov. 2005      & & 1$^{st}$ 4 vibrations
\\ Contributor:&  B. J. Drouin   & &
\\             &  J. C. Pearson  & &
\\             &  H. M. Pickett  & &
\\ Lines Listed:       &   28832 & Q(300.0)=&      178.120
\\ Freq. (GHz) $<$     &   29799 & Q(225.0)=&      116.019
\\ Max. J:             &      23 & Q(150.0)=&       63.677
\\ LOGSTR0=            &  -999.0 & Q(75.00)=&       23.170
\\ LOGSTR1=            &  -999.0 & Q(37.50)=&        8.580
\\ Isotope Corr.:      &     0.0 & Q(18.75)=&        3.033
\\ Egy. (cm$^{-1}$) $>$&     0.0 & Q(9.375)=&        1.257
\\ $\mu_a$ = &                   & A=& 835840.3
\\ $\mu_b$ = & see below         & B=& 435351.7
\\ $\mu_c$ = &                   & C=& 278138.7
\headend 

\begin{center}
\begin{tabular*}{7cm}{@{\extracolsep{\fill}}rrr}
\hline
v & state & $\mu_b$\\
\hline
 1 & $\nu_2$  & -1.82332\\
 2 & 2$\nu_2$ & -1.79166\\
 3 & $\nu_1$  & -1.86006\\
 4 & $\nu_3$  & -1.87744\\
\hline
\end{tabular*}
\end{center}
\vspace{10pt}
The frequency analysis includes the ground state and first four excited
vibrations and is based on H.M. Pickett, J.C. Pearson, C.E. Miller, 
2005, Journal of Molecular Spectroscopy {\bf 233}, 174-179.
The data set used in this fit includes all the microwave measurements
reviewed in J. C. Pearson, T. Anderson, E. Herbst, F. C. De Lucia and 
P. Helminger, 1991, Astrophys J. {\bf 379}, L41, additional measurements 
were used from J. C. Pearson, 1995, Ph.D. Thesis Duke University, S. 
Belov, 1996, Private Communication, F. Matsushima, H. Odashima, 
T. Iwasaki, S. Tsunekawa, K. Takagi, 1995, J. Mol.\ Struct.\ {\bf 352}, 353-371,
and P. Chen, J.C. Pearson, S. Matsuura, H.M. Pickett, G.A. Blake, 2000, 
Astrophys. J. Suppl. {\bf 128}, 371-385, K.V. Chance, K. Park, K.M. Evenson, 
1998, J. Quant. Spectrosc.Radiat. Transfer {\bf 59} 687-688.  FTIR rotational 
data was taken from J. Kauppinen, T. Karkkainen and E. Kyro, 1978, J. Mol.\ Spectrosc.\ {\bf 71}, 
15, J. W. C. Johns, 1985, J. Opt.\ Soc.\ Am.\ {\bf B2}, 1340, R. Paso and V. M.
Horneman, 1995, J. Opt.\ Soc.\ Am.\ {\bf B12}, 1813 and R.A. Toth, 1999, J. 
Mol. Spectros. {\bf 194} 28-42.

FTIR band transitions were taken from R.A. Toth, 1999, J. 
Mol. Spectros. {\bf 194} 28-42, P. De Natale, L. Lorini, M. Inguscio, I.G. Nolt, J.H. Park, G.DiLonardo, 
L. Fusina, P.R.A. Ade, A.G. Murray, 1997, Appl. Opt. {\bf 36}, 8526-8532. D.B. 
Peterson, C.I. Frum, H.M. Pickett (JPL data at 1000 K, 190-340 cm$^{-1}$), 
unpublished. M.P. Esplin, R.B. Wattson, M.L. Hoke, L.S. Rothman, 1998, J. 
Quant.Spectrosc. Radiat. Transfer {\bf 60}, 711-738. S.N. Mikhailenko, V.G. 
Tyuterev, K.A. Keppler, B.P. Winnewisser,M. Winnewisser, G. Mellau, S. Klee, 
K.N. Rao, 1997, J. Mol.Spectrosc. {\bf 184}, 330-349. O.L. Polyansky, J.R. 
Busler, B. Guo, K. Zhang, P.F. Bernath, 1996, J.Mol. Spectrosc. {\bf 176}, 
305-315. O.L. Polyansky, J. Tennyson, P.F. Bernath, 1997, J. Mol. Spectrosc. 
{\bf 186}, 213-221. O.L. Polyansky, N.F. Zobov, J. Tennyson, J.A. Lotoski, 
P.F. Bernath, 1997, J. Mol. Spectrosc. {\bf 184} 35-50.R.A. Toth, 1993, J. 
Opt. Soc. Am. B {\bf 10}, 1526-1544. R.A. Toth, L.R. Brown, C. Plymate, 1998, 
J. Quant. Spectrosc. Radiat.Transfer {\bf 59}, 529-562. N.F. Zobov, O.L. 
Polyansky, J. Tennyson, J.A. Lotoski, P.Colarusso, K.-Q. Zhang, P.F. Bernath, 
1999, J. Mol. Spectrosc. {\bf 193}, 118-136. Energy Levels are taken from R. A. Toth, 1998, 
J. Mol.\ Spectrosc.\ {\bf 190}, 379 and O. L. Polyansky, N. Zobov, S. Viti, 
J. Tennyson, P. Bernath and L. Wallace, 1997, J. Mol.\ Spectrosc.\ {\bf 186}, 
422.

The fit results in a reduced RMS of 9.5 obtained for a combination of the the five states.
This catalog entry represents the excited state portion only.

The intensities calculation follows the method in C. Camy-Peyret 
{\it et al.}, 1985, J. Mol.\ Spectrosc.\ {\bf 113}, 208.  The values of 
$\mu_b$ listed above are from S. L. Shostak and J. S. Muenter, 1991, J. Chem
Phys. {\bf 94}, 5883-5890, these were used as well as second order Herman Wallis terms
determined for the ground state. 
The Herman Wallis terms were determined using SPCAT to match an intensity
prediction based on a fully perturbed ground state as described by H. M. Pickett, 
\lq\lq Centrifugal Corrections to Rotational Intensities", Lecture TF10, 45$^{th}$ 
Symposium on Molecular Spectroscopy, Columbus, OH, 1990.
The partition function includes the ground, $\nu_2$, $2\nu_2$, $\nu_1$ and $\nu_3$ states.  
Classical corrections for higher temperatures are given in P. Chen {\it et al.}.