Publications of the Astronomical Society of Australia

Research Article

A Spectral Line Survey of IRAS 17470-2853 from 86.1 to 92.1 GHz

Hun-Dae Kima1, Ramesh Balasubramanyama1 and Michael G. Burtona1a2

a1 School of Physics, University of New South Wales, Sydney, NSW 2052, Australia

a2 School of Physics, University of New South Wales, Sydney, NSW 2052, Australia. School of Cosmic Physics, Dublin Institute of Advanced Studies, 5 Merrion Square, Dublin 2, Ireland


We present results from a spectral line survey of the young stellar object IRAS 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 m radio telescope in the frequency range from 86.1 to 92.1 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 80–115 GHz and 330–360 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 ˜5 km s−1 indicates relatively quiet or quasi-thermal emission. On the other hand, a significant difference in T A* (HNC)/T A*(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 (υ=0, J=2–1), ˜9 km s−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.

(Received September 15 2001)

(Accepted October 06 2002)


  • HII regions;
  • ISM: individual (IRAS 17470-2853 = G0.55–0.85);
  • ISM: molecules;
  • ISM: abundances;
  • stars: formation;
  • radio lines: ISM