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REFERENCES

  1. Bradford, C. M., Aguirre, J. E., Aikin, R., et al. 2009, ApJ, 705, 112

  2. Canzian, B., Mundy, L. G., & Scoville, N. Z. 1988, ApJ, 333, 157

  3. Cernicharo, J., Goicoechea, J. R., Pardo, J. R., & Asensio-Ramos, A. 2006, ApJ, 642, 940

  4. Costagliola, F. & Aalto, S. 2010, A&A, 515, A71

  5. de Vicente, P., Martín-Pintado, J., Neri, R., & Colom, P. 2000, A&A, 361, 1058

  6. de Vicente, P., Martin-Pintado, J., & Wilson, T. L. 1997, A&A, 320, 957

  7. Gensheimer, P. D., Mauersberger, R., & Wilson, T. L. 1996, A&A, 314, 281

  8. González-Alfonso, E., Smith, H. A., Fischer, J., & Cernicharo, J. 2004, ApJ, 613, 247

  9. Greve, T. R., Papadopoulos, P. P., Gao, Y., & Radford, S. J. E. 2009, ApJ, 692, 1432

  10. Kamenetzky, J., Glenn, J., Maloney, P. R., et al. 2011, ApJ, 731, 83

  11. Krips, M., Neri, R., García-Burillo, S., et al. 2008, ApJ, 677, 262

  12. Lahuis, F., Spoon, H. W. W., Tielens, A. G. G. M., et al. 2007, ApJ, 659, 296

  13. Loenen, A. F., van der Werf, P. P., Güsten, R., et al. 2010, A&A, 521, L2

  14. Martín, S., Krips, M., Martín-Pintado, J., et al. 2011, A&A, 527, A36

  15. Martín, S., Mauersberger, R., Martín-Pintado, J., Henkel, C., & García-Burillo, S. 2006, ApJS, 164, 450

  16. Mauersberger, R. & Henkel, C. 1993, in Reviews in Modern Astronomy, Vol. 6, Reviews in Modern Astronomy, ed. G. Klare, 69-102

  17. Mauersberger, R., Henkel, C., Wielebinski, R., Wiklind, T., & Reuter, H. 1996, A&A, 305, 421

  18. Muller, S., Beelen, A., Guélin, M., et al. 2011, ArXiv e-prints

  19. Naylor, B. J., Bradford, C. M., Aguirre, J. E., et al. 2010, ApJ, 722, 668

  20. Panuzzo, P., Rangwala, N., Rykala, A., et al. 2010, A&A, 518, L37

  21. Sakamoto, K., Aalto, S., Evans, A. S., Wiedner, M. C., & Wilner, D. J. 2010, ApJ, 725, L228

  22. Sakamoto, K., Mao, R.-Q., Matsushita, S., et al. 2011, ArXiv e-prints

  23. Salter, C. J., Ghosh, T., Catinella, B., et al. 2008, AJ, 136, 389

  24. Sawada, T., Hasegawa, T., Handa, T., et al. 2001, ApJS, 136, 189

  25. Snell, R. L., Narayanan, G., Yun, M. S., et al. 2011, AJ, 141, 38

  26. van der Werf, P. P., Isaak, K. G., Meijerink, R., et al. 2010, A&A, 518, L42

  27. Wang, M., Henkel, C., Chin, Y., et al. 2004, A&A, 422, 883

  28. Weliachew, L. 1971, ApJ, 167, L47

Discussion

CASELLI: You talk about "hot core" species. Did you try to compare abundance ratios in Arp 220 with typical "hot core" abundances, to test if we are indeed observing ~ 106 Sgr B2 hot cores?

MARTÍN: Such comparison was performed with the abundances measured towards the starburst galaxy NGC 253, but not yet with Arp 220. However, Arp 220 and NGC 253 show significantly similar abundances but for the vibrational emission observed towards Arp 220. This difference points out towards a "hot core" origin but a closer comparison with Galactic templates is yet to be performed.

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