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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/2517

Title: A spectral line survey of IRAS 17470-2853 from 86.1 to 92.1 GHz
Authors: Kim, Hun-Dae
Balasubramanyam, R.
Burton, M.G.
Keywords: HII regions
ISM: individual (IRAS 17470-2853 = G0.55– 0.85)
ISM: molecules
ISM: abundances
stars: formation
radio lines: ISM
Issue Date: 2002
Publisher: Astronomical Society of Australia
Citation: Publications of the Astronomical Society of Australia, 2002, Vol.19, p505-514
Abstract: We present results from a spectral line survey of the young stellar object IRAS17470-2853, undertaken to examine chemical changes during the evolution from hot molecular cores to ultracompact HII regions. Observations were carried out with the Mopra 22m radio telescope in the frequency range from 86.1 to 92.1GHz. 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 80-115GHz and 330-360GHz 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 ~5kms-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 (υv=0, J=2-1), ~9kms-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.
Description: Restricted Access. Please click on the alternative location for the open-access full text.
URI: http://hdl.handle.net/2289/2517
ISSN: 1323-3580
Alternative Location: http://adsabs.harvard.edu/cgi-bin/bib_query?2002PASA...19..505K
http://dx.doi.org/10.1071/AS01094
Copyright: 2002 Astronomical Society of Australia
Appears in Collections:Research Papers (A&A)

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