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

Published online by Cambridge University Press:  05 March 2013

Hun-Dae Kim ,
Ramesh Balasubramanyam  and
Michael G. Burton
Hun-Dae Kim
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia
Ramesh Balasubramanyam
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia
Michael G. Burton
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia 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
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Abstract

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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 regionsISM: individual (IRAS 17470-2853 = G0.55–0.85)ISM: moleculesISM: abundancesstars: formationradio lines: ISM
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 19 , Issue 4 , 2002 , pp. 505 - 514
Copyright
Copyright © Astronomical Society of Australia 2002

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