Notes. All observations were obtained at the VLT using the 300 line/mm grism (“GRIS_300V”) along with the “GG435” order-sorting filter to prevent second-order contamination. This resulted in a useable spectral range of 4350 Å–9200 Å. All observations were made through a 1.′′0 slit, which delivered a resolution of ~12 Å, as derived from the FWHM of night-sky lines. The flux standard used for all observations was BD+26°2606 (Oke & Gunn 1983), observed on the same nights as the science observations. All observations were made with the position angle of the spectrograph slit set to 0 deg, which often differed significantly from the parallactic angle (Filippenko 1982); when coupled with the relatively narrow slit used, the potential for differential light loss – and, hence, inaccurate relative flux calibration – is significant. ^(a) Day since estimated explosion date of 2012-03-16.09 UT = MJD 56002.09 = JD 2456002.09; Bose et al. 2013). ^(b) yyyy-mm-dd, calculated as the midpoint of all of the individual exposures. ^(c)Modified Julian Date(Julian Date – 2400000.5), at the midpoint of all of the individual exposures. ^(d) Total exposure time in seconds, with the number of complete sets of four waveplate positions obtained shown in parenthesis. ^(e) Air mass range for each set of observations. ^(f)Average value of theFWHM of the spatial profile for each epoch, rounded to the nearest 0.′′ 1.