On the possible detection of C60+ in the interstellar medium

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Presentation transcript:

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

C60+

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

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

- telluric lines - stellar MgII blend

Telluric lines

Telluric lines

Telluric lines

Galazutdinov, G. A. ; Shimansky, V. V. ; Bondar, A. ; Valyavin, G Galazutdinov, G. A.; Shimansky, V. V.; Bondar, A.; Valyavin, G.; Krełowski, J. 2017, MNRAS, 465, 3956

Non-LTE Mg II

Non-LTE Mg II

Mg II

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

No weights!

Weighted fit

After Correction – No weights

After Correction – Weighted

New results

Versus dust

Ti II 3242

NaI 3303

FeI 3860

CN 3876

CaI 4227

CH+ 4232

DIB 5780

DIB 5797

DIB 6196

DIB 6284

DIB 6284

DIB6279

DIB 6284

DIB 6614

Weaker lines

E. K. Campbell, M. Holz, D. Gerlich, J. P E.K.Campbell, M.Holz, D.Gerlich, J.P.Maier, Nature, 2015, 523, 7560, 322 9632.7 0.8 9577.5 1.00 9428.5 0.3 9365.9 0.2 E.K.Campbell, J.P.Maier, 2018, ApJ, 858, 36 9632.1 0.84 9577.0 1.00 9427.8 0.17 9365.2 0.26

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?

Thank you for attention !