1. On the possible detection of C60+ in the interstellar medium
Gazinur Galazutdinov
Universidad Católica del Norte
Antofagasta, Chile
Pulkovo Observatory, Russia
Special Astrophysical Observatory, Russia

2. C60+

3. Lab spectrum of C60 cation (blue line) compared to the spectrum of heavily reddened BD +40o 4220 (red line)

4. Laboratory gas-phase spectrum of C60+ by J.P. Maier & Co

6. - telluric lines
- stellar MgII blend

8. Telluric lines

9. Telluric lines

10. Telluric lines

11. Galazutdinov, G. A. ; Shimansky, V. V. ; Bondar, A. ; Valyavin, G
Galazutdinov, G. A.; Shimansky, V. V.; Bondar, A.; Valyavin, G.; Krełowski, J , MNRAS, 465, 3956

12. Non-LTE Mg II

13. Non-LTE Mg II

15. Mg II

16. R. Lallement et al., 2018, A&A, 614, A28

17. No weights!

18. Weighted fit

19. After Correction – No weights

20. After Correction – Weighted

22. New results

24. Versus dust

25. Ti II 3242

26. NaI 3303

27. FeI 3860

28. CN 3876

29. CaI 4227

30. CH

31. DIB 5780

32. DIB 5797

33. DIB 6196

34. DIB 6284

35. DIB 6284

36. DIB6279

37. DIB 6284

38. DIB 6614

41. Weaker lines

42. E. K. Campbell, M. Holz, D. Gerlich, J. P
E.K.Campbell, M.Holz, D.Gerlich, J.P.Maier, Nature, 2015, 523, 7560, 322
E.K.Campbell, J.P.Maier, 2018, ApJ, 858, 36

44. Conclusions
There are no (or poor) correlations with dust & molecules & atomic gas
Poor correlation of 9633 with anything → 9633 is a blend of DIBs ?
9577 correlates with 6196, 6614, broad DIBs
Both DIBs are weak in “zeta” clouds → the effect of low E(B-V) or
UV flux irradiation is needed?

45. Thank you for attention !