All Tables

Table 1: Observational log for SN2006X with UVES. The phase is given in days with respect to the B-band maximum light (February 20, 2006). The UVES setting simultaneously covered three wavelength ranges (3290-4500 Å, 4780-5740 Å and 5830-6800 Å) with a FWHM resolution of $\sim$ 7 km $\ensuremath {\rm {s}^{-1}}$ .
Table 2: Heliocentric corrected radial velocities v (km $\ensuremath {\rm {s}^{-1}}$ ), Doppler widths b (km $\ensuremath {\rm {s}^{-1}}$ ) and column densities N (cm^-2) have been derived with VPFIT for Ca I, CH⁺ and CH transitions toward SN2006X. 1 $\sigma$ rms-errors are given in parenthesis. CH at phase +61 is not well constrained (low S/N) but consistent with earlier phases. Contamination in CH⁺ (4232 Å) at phase -2 and strong noise in CH⁺ (3957 Å) at phase +14 made it impossible to properly constrain fits to this lines. Straightforward peak velocity and strength measurements do however agree with the other two transitions. For the CN R(0) transitions v is 1645 and 1647 km $\ensuremath {\rm {s}^{-1}}$ at phase -2 and +14, respectively.
Table 3: Radial heliocentric velocities and equivalent widths for $\lambda \lambda$ 6196 and 6283 ( $1\sigma$ rms-error in parenthesis). 3 $\sigma$ (=3.0 FWHM $\sigma _{\rm noise}$ ) upper limits for $\lambda \lambda$ 6379 and 6613. Uncertainties in $\lambda$ 6283 central velocity are of the order of 10 to 20 km $\ensuremath {\rm {s}^{-1}}$ .
Table 4: Comparison of DIB strengths (in mÅ) toward SN2006X in M 100, the Galaxy and LMC. Upper limits for $\lambda \lambda$ 6379 and 6613 obtained from weight averaged spectra at phase -2 and +14. Equivalent widths for DIBs toward $\beta ^1$ Sco and $\rho$ Oph from Sollerman et al. (2005) and for Sk-69 223 from Cox et al. (2006). Taurus dark cloud toward HD 283809 from Adamson et al. (1991).