
%0 Journal Article
%A Kim, Hun-Dae 
%A Balasubramanyam, Ramesh 
%A Burton, Michael G. 
%T A Spectral Line Survey of IRAS 17470-2853 from 86.1 to 92.1 GHz
%J Publications of the Astronomical Society of Australia
%D 2002/12/11
%V 19
%N 4
%P 505-514
%K HII regions &#8212; ISM: individual (IRAS 17470-2853 = G0.55&#8211;0.85) &#8212; ISM: molecules &#8212; ISM: abundances &#8212; stars: formation &#8212; radio lines: ISM
%R https://doi.org/10.1071/AS01094
%U https://www.publish.csiro.au/paper/AS01094 
%X We present results from a spectral line survey of the young stellar object IRAS&#32;17470-2853, undertaken to examine chemical changes during the evolution from hot molecular cores to ultracompact HII regions. Observations were carried out with the Mopra 22&#32;m radio telescope in the frequency range from 86.1 to 92.1&#32;GHz. A total of 21 lines from 9 molecules were detected. Except for CH3CN they are all simple molecules. We compare the results to the ultracompact HII region G34.3+0.15, where spectral line surveys in the frequency range 80&#8211;115&#32;GHz and 330&#8211;360&#32;GHz have been performed. While the molecular lines detected are similar, their widths and intensities are somewhat narrower and lower, respectively, in IRAS 17470-2853. The typical line width of &#126;5&#32;km&#32;s&#8211;1 indicates relatively quiet or quasi-thermal emission. On the other hand, a significant difference in TA* (HNC)/TA*(HCN) has been found: 0.8 for IRAS 17470-2853 compared to 2.6 for G34.3+0.15. The broad line width of SiO (&#965;=0, J=2&#8211;1), &#126;9&#32;km&#32;s&#8211;1, suggests that IRAS 17470-2853 is experiencing a shock generated by the embedded object. Column densities, or lower limits to them, are derived for observed molecules. 
