CSIRO Publishing blank image blank image blank image blank imageBooksblank image blank image blank image blank imageJournalsblank image blank image blank image blank imageAbout Usblank image blank image blank image blank imageShopping Cartblank image blank image blank image You are here: Journals > PASA   
  Publications of the Astronomical Society of Australia
blank image Search
blank image blank image
blank image
  Advanced Search

Journal Home
Current Issue
All Issues
Special Issues
Research Fronts


Article << Previous     |     Next >>   Contents Vol 19(4)

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

Hun-Dae Kim, Ramesh Balasubramanyam and Michael G. Burton

Publications of the Astronomical Society of Australia 19(4) 505 - 514
Published: 20 December 2002


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 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 (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.

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

Full text doi:10.1071/AS01094

© ASA 2002

blank image
 PDF (335 KB)
 Export Citation
Legal & Privacy | Contact Us | Help


© CSIRO 1996-2016