Best-fitting stellar model in the pre-flare spectrum. The grey shades label the emission lines identified by us. These are: 1. O III λλ3121,3132; 2. He I λ3189; 3. [Ne V] λ3346; 4. [Ne V] λ3426; 5. [Fe VII] λ3586; 6. [O II] λλ3726,3729; 7. [Fe VII] λ3759; 8. [Ne III] λ3869 + He I λ3889; 9. [Ne III] λ3968 + Hϵ; 10. [S II] λ4076 + Hδ; 11. Hγ + [O III] λ4363; 12. He I λ4471; 13. N III λ4640 + He II λ4686; 14. Hβ; 15. [O III] λλ4959,5007; 16. [N I] λ5199; 17. [Fe VII] λ5722 + [Fe II]λ5750??; 18. He I λ5876; 19. [Fe VII] λ6087; 20. [O I] λ6300; 21. [O I] λ6364 + [Fe X] λ6376; 22. Hα + [N II] λ6548,6583; 23. He I λ6679 + [S II] λλ6716,6731; 24. He I λ7065; 25. [Ar III] λ7136; 26. [O II] λλ7320,7330. The dark grey shades label the regions affected by strong telluric absorption lines, which were not included in the fitting.