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	Figure 1: The original and smoothed spectra of SN 2002ej (Sect. 5). The spectra are in the parent galaxy restframe. The number near smoothed spectra are the corresponding box sizes.
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In the text

	Figure 2: The graphical output of GELATO for the cases of SN 2002an and SN 2005bs from our sample. The spectra are in the parent galaxy rest frame. The black lines are the input spectra and the gray ones the best fitting template spectra, divided in bins and scaled in flux to match the input spectra in the respective bins.
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In the text

	Figure 3: The phase distribution of the template SN spectra. Typically, the phases are relative to the B-maximum for SNe Ia and Ib/c and to the explosion epoch for SNe II.
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In the text

	Figure 4: The phases determined with GELATO compared to the phases from photometry for a sample of type-Ia SNe. In the bottom panel are the residuals.
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In the text

	Figure 5: The phases derived with GELATO compared to the phases obtained from photometry for a sample of type-II (black dots) and type-Ib/c (gray dots) SNe. In the bottom panel are the residuals.
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In the text

	Figure 6: The comparison of the ESC SN spectra of non-ESC targets with their best fitting templates. The spectra are in the parent galaxy restframe and not corrected for extinction. The black lines are the ESC spectra, while the gray ones display template spectra.
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In the text

	Figure 7: Same as Fig. 6.
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In the text

	Figure 8: Same as Fig. 6.
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In the text

	Figure 9: Same as Fig. 6.
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In the text