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Aims. Supernovae offer the unique possibility to probe diffuse extra-galacticsightlines via observation of the optical transitions of atoms, molecules andthe diffuse interstellar bands (DIBs). Through optical spectroscopy thepresence of (complex) molecules in distant galaxies can be established.  Methods. High resolution optical (3300 -- 6800 Angstrom) spectra of SN2006Xat different phase obtained with UVES on the VLT were reduced and analysed.  Results. In addition to previously detected atomic (NaI and CaII) andmolecular (CN) transitions we present detections of DIBs (6196, 6283 Angstrom),diatomic molecules (CH, CH+) and neutral atoms (CaI) in the spectra of SN2006Xtaken at different phases (at 2 days before and 14 and 61 days after thebrightness maximum). An analysis of the absorption profiles shows no variationbetween phases in the abundance, nor the central velocities (within 3-sigmaerror bars) of the (dense) gas tracers (CH, CH+ and CaI) and the DIBs. This isconsistent with the conclusion in the literature that SN2006X exploded behind adense interstellar cloud (inferred from strong atomic sodium and calcium linesand CN transitions) which caused strong photometric reddening but whosematerial was not directly affected by the supernova explosion. The CH and CNcolumn densities correspond to a reddening of one magnitude following theGalactic correlation derived previously. The 6196 and 6283 lines detected inthe M100 ISM are under-abundant by factor of 2.5 to 3.5 (assuming a visualextinction of ~2 mag) compared to the average Galactic ISM relationship. Upperlimits for 6379 and 6613 DIBs show that these are at least a factor of sevenweaker. Therefore, the Galactic DIB-reddening relation does not seem to hold inM100, although the lower gas-to-dust ratio may further reduce this discrepancy.

Interstellar atoms, molecules and diffuse bands toward SN2006X in M100