3 Conclusion

With the presentation of absolute transition probabilities of Co II, we hope to provide data that allow for a better understanding of such objects as Co-stars and late-type supernovae; in the latter case, time evolution of Fe, Co and Ni lines provides a test of explosive nucleosynthesis models.

To avoid typing errors, all tables containing transition probabilities are computer processed. Complete results of the fits of both the odd and even energy system, as well as the corresponding complete transition arrays (without lower limits to the gf- and A-values or restriction of the configurations) can be found in our database (anonymous ftp) at ftp://nucleus.phys.uva.nl in the directory pub/orth/co2.

Acknowledgements

It is a pleasure to thank Dr. J.E. Lawler for sharing his results with us in advance of the publication.