Contents Previous

REFERENCES

  1. Biller, S. D., et al. 1995, ApJ, 445, 227
  2. Ciliegi, P., McMahon, R. G., & Miley, G. 1999, MNRAS, 302, 222
  3. Dole, H. 2000, PhD thesis, Paris XI University
  4. Dole, H., et al. 2001, to be submitted
  5. Dole, H., Gispert, R., Lagache, G., et al., 2000, in ``ISO Surveys of a Dusty Universe'', Lecture Notes in Physics, eds. D. Lemke, M. Stickel, K. Wilke, Springer
  6. Falgarone, E. 1998, in Starbursts: Triggers, Nature and Evolution, Les Houches School, eds. B. Guiderdoni & A. Kembhavi
  7. Finkbeiner, D. P., Davies, M., & Schlegel, D. J. 2000, ApJ, 544, 81
  8. Fixsen, D. J., et al. 1998, ApJ, 508, 123
  9. Franceschini, A., Andreani, P., & Danese, L. 1998, MNRAS, 296, 709
  10. Gautier, T. N. III, Boulanger, F., Pérault, M., & Puget, J. L. 1992, AJ, 103, 1313
  11. Guiderdoni, B., Hivon, E., Bouchet, F., & Maffei, B. 1998, MNRAS, 295, 877
  12. Guiderdoni, B., Bouchet, B., Puget, J. L., et al. 1997, Nature, 390, 257
  13. Haiman, Z., Knox, L. 2000, ApJ, 530, 124
  14. Hauser, M. G., et al. 1998, ApJ, 508, 25
  15. Herbstmeier, U., et al. 1998, A&A, 332, 739
  16. Kawara, K., Sato, Y., & Matsuhara, H. 1998, A&A, 336, 9
  17. Kelsall, T., Weiland, J. L., & Franz, B. A. 1998, ApJ, 508, 44
  18. Kessler, M. F., et al. 1996, A&A, 315, L27
  19. Kogut, A., et al. 1996, ApJ, 460, 1
  20. Lagache, G., et al. 1999, A&A, 344, 322
  21. Lagache, G., et al. 2000 A&A, 354, 247
  22. Lagache, G. & Dole, H. 2001, to be submitted
  23. Lagache, G., & Puget, J-L. 2000, A&A, 355, 17
  24. Lemke, D., et al. 1996, A&A, 315, L64
  25. Matsuhara, H., Kawara, K., & Sato, Y. 2000, A&A, 361, 407
  26. Miville-Deschênes, M. A. 1999, PhD thesis, Paris XI University
  27. Oliver, S., Rowan-Robinson, M., & Alexander, D. M. 2000, MNRAS, 316, 749
  28. Puget, J. L., et al. 1996, A&A, 308, L5
  29. Puget, J. L., et al. 1999, A&A, 354, 29
  30. Reynolds, R. J., et al. 1998, PASA, 15, 14
  31. Schlegel, D. J., Finkbeiner, D. P., & Davis, M., 1998, ApJ, 500, 525
  32. Wright, E. L. 1998, ApJ, 496, 1
  33. Wright, E. L. 2000, astro-ph/0004192

Discussion

Martin Harwit: While the SCUBA sources might be predominantly at high redshifts, and cannot be ruled out as being at high z, the background is so low there that these galaxies are not major factors as far as production of heavy elements or massive star formation is concerned. Otherwise the abundance of chemical elements at high redshifts would be seen to be much higher.

Jean-Loup Puget: Yes. In the model I presented the bulk of the energy comes from redshifts around z = 1, as do the heavy elements.

Ray Norris: At higher redshift, metallicity will decrease, so presumably the dust fraction will decrease. To what extent can this account for your observed luminosity evolution?

Puget: The luminosity function I showed is a purely empirical one fitting both the background and the counts at 15, 170, and 850 µm. The dust contribution, which should decrease at large z, has to be combined with morphology of the galaxies. Local starbursts show much larger extinction than the average one.

Contents Previous