\\ Species Tag:        &   97002 & Name:&  Cl-35-ONO2      
\\ Version:            &       2 & & Chlorine nitrate
\\ Date:       &  Oct. 1996      & & $^{35}$Cl isotope
\\ Contributor:&  H. S. P. M\"uller  & & 
\\             &                 & & 
\\ Lines Listed:       &   78323 & Q(300.0)=&   614310.627 
\\ Freq. (GHz) $<$     &    1000 & Q(225.0)=&   372267.704 
\\ Max. J:             &      99 & Q(150.0)=&   181443.199 
\\ LOGSTR0=            &   -10.0 & Q(75.00)=&    54099.169 
\\ LOGSTR1=            &    -7.3 & Q(37.50)=&    17894.505 
\\ Isotope Corr.:      &  -0.122 & Q(18.75)=&     6296.771 
\\ Egy. (cm$^{-1}$) $>$&         & Q(9.375)=&     2230.345 
\\ $\mu_a$ = &  0.72             & A=& 12105.78
\\ $\mu_b$ = &  0.28             & B=&  2777.001
\\ $\mu_c$ = &                   & C=&  2258.151
\headend 

	The frequencies are taken from 
(1) R. D. Suenram and D. R. Johnson, 1977, J. Mol. Spectrosc. {\bf 65}, 239;
(2) R. D. Suenram and F. J. Lovas, 1984, J. Mol. Spectrosc. {\bf 105}, 351; 
and (3) H. S. P. M\"uller, P. Helminger, and S. H. Young, 
1997, J. Mol. Spectrosc. {\bf 181}, 363. 

The data for both isotopomers ($^{35}$Cl and $^{37}$Cl) in the $v$ = 0 and 
$v_9$ = 1 states has been fit simultaneously as described in (3). 
Lines outside four times the experimental uncertainties were omitted and 
have not been merged. A fit of similar qualtity is achieved when only 
lines of this species are used. While the data for this species is archived 
in the usual way, the combined fit is archived as clg.*.

Because $^{35}$Cl hyperfine splittings were important in the fit, the catalog 
entry presented includes these splittings even though they are in general much 
smaller than the width of stratospheric lines.

The dipole moment is from (1). The partition function takes into account the 
torsional mode at $ca.$ 120 cm$^{-1}$. Because of the small rotational 
constants the partition function has been calculated up to $J$ = 150. 
Transitions with $J$ $>$ 99 are not included because at stratospheric temperatures 
their intensity is expected to be very small, even though some of them may 
be stronger than listed low $J$ lines at room temperature.