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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
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.

Type
Research Article
Copyright
Copyright © Astronomical Society of Australia 2002

References

Baudry, A., Combes, M., Perault, M., & Dickman, R. 1980, A&A, 85, 244 Google Scholar
Blake, G. A., Sutton, E. C., Masson, C. R., & Phillips, T. G. 1986, ApJS, 60, 357 CrossRefGoogle Scholar
Blake, G. A., Sutton, E. C., Masson, C. R., & Phillips, T. G. 1987, ApJ, 315, 621 CrossRefGoogle Scholar
Blake, G. A., Mundy, L. G., Carlstrom, J. E., Padin, S., Scott, S. L., Scoville, N. Z., & Woody, D. P. 1996, ApJ, 472, 49 CrossRefGoogle Scholar
Brown, R. D., Burden, F. R., & Cuno, A. 1989, ApJ, 347, 855 CrossRefGoogle Scholar
Cernicharo, J., Castets, A., Duvert, G., & Guilloteau, S. 1984, A&A, 139, L13 Google Scholar
Charnley, S. B., Kress, M. E., Tielens, A. G. G. M., & Millar, T. J. 1995, ApJ, 448, 232 CrossRefGoogle Scholar
Cummins, S. E., Linke, R. A., & Thaddeus, P. 1986, APJ, 60, 819 CrossRefGoogle Scholar
Forster, J. R., & Caswell, J. L. 1999, A&AS, 137, 43 Google ScholarPubMed
Garwood, R. W., & McMullin, J. P. 1999, AIPS++ NOTE 225–Using Dish: The AIPS++ Single Dish Analysis Environment, http://aips2.nrao.edu/docs/aips++.html Google Scholar
Goldsmith, F. P., Langer, W. D., Ellder, J., Irvine, W., & Kollberg, E. 1981, ApJ, 249, 524 CrossRefGoogle Scholar
Henkel, C., Mauersberger, R., Wilson, T. L., Snyder, L. E., Menten, K., & Wouterloot, J. G. A. 1987, A&A, 182, 299 Google ScholarPubMed
Herbst, E., Adams, N. G., & Smith, D. 1987, ApJ, 312, 351 CrossRefGoogle Scholar
Herbst, E., & Leung, C. M. 1990, A&A, 233, 177 Google Scholar
Huntress, W. T. 1977, ApJS, 33, 495 CrossRefGoogle Scholar
Huttemeister, S., Henkel, C., Mauersberger, R., Brouillet, N., Wiklind, T., & Millar, T. J. 1995, A&A, 295, 571 Google Scholar
Irvine, W. I., & Schloerb, F. P. 1984, ApJ, 282, 516 CrossRefGoogle Scholar
Jewell, P. R., Hollis, J. M., Lovas, F. J., & Snyder, L. E. 1989, ApJS, 70, 833 CrossRefGoogle Scholar
Johansson, L. E. B., et al. 1984, A&A, 130, 227 Google ScholarPubMed
Kim, H.-D., Cho, S.-H., Chung, H.-S., Kim, H.-R., Roh, D.-G., Kim, H.-G., Minh, Y. C., & Minn, Y.-K. 2000, ApJS, 131, 483 CrossRefGoogle Scholar
Loren, R. B., & Mundy, L. G. 1984, ApJ, 286, 232 CrossRefGoogle Scholar
Lovas, F. J. 1992, JPCRD, 21, 181 Google Scholar
Macdonald, G. H., Gibb, A. G., Harbing, R. J., & Millar, T. J. 1996, A&AS, 119, 333 Google ScholarPubMed
Mauersberger, R., Henkel, C., Walmsley, C. M., Sage, L. J., & Wiklind, T. 1991, A&A, 247, 307 Google Scholar
Millar, T. J., Herbst, E., & Charnley, S. B. 1991, A&A, 369, 147 Google Scholar
Millar, T. J., Macdonald, G. H., & Gibb, A. G. 1997, A&A, 325, 1163 Google Scholar
Olmi, L., Cesaroni, R., & Walmsley, C. M. 1993, A&A, 276, 489 Google Scholar
Schilke, P., Walmsley, C. M., Pineau des Forets, G., Roueff, E., Flower, D. R., & Guilloteau, G. 1992, A&A, 256, 595 Google Scholar
Schilke, P., Groesbeck, T. D., Blake, G. A., & Phillips, T. G. 1997, ApJS, 108, 301 CrossRefGoogle Scholar
Sutton, E. C., Jaminet, P. A., Danchi, W. C., & Blake, G. A. 1991, ApJS, 77, 255 CrossRefGoogle Scholar
Takano, S., et al. 1998, A&A, 329, 1156 Google Scholar
Turner, B. E. 1989, ApJS, 70, 539 CrossRefGoogle Scholar
Turner, B. E. 1991, ApJS, 76, 617 CrossRefGoogle Scholar
Ulich, B. L., & Haas, R. W. 1976, ApJS, 30, 247 CrossRefGoogle Scholar
Walmsley, C. M., Hersen, W., Henkel, C., Mauersberger, R., & Wilson, T. L. 1987, A&A, 172, 311 Google ScholarPubMed
Walsh, A. J., Hyland, A. R., Robinson, G., & Burton, M. G. 1997, A&A, 291, 261 Google ScholarPubMed
Walsh, A. J., Burton, M. G., Hyland, A. R., & Robinson, G. 1998, A&A, 301, 640 Google ScholarPubMed
Walsh, A. J., Macdonald, G. H., Alvey, N. P. S., Burton, M. G., & Lee, J.-K. 2002, A&A, submittedGoogle Scholar
Wootten, A., Evans II, N. J., Snell, R., & Vanden Bout, P. 1978, ApJ, 225, L143 CrossRefGoogle Scholar
Wootten, A., Bozyan, E. P., & Garrett, D. B. 1980, ApJ, 239, 844 CrossRefGoogle Scholar
Ziurys, L. M., & McGonagle, D. 1993, ApJS, 89, 155 CrossRefGoogle Scholar
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A Spectral Line Survey of IRAS 17470-2853 from 86.1 to 92.1 GHz
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