Auxiliary Information

Online material related to the H.E.S.S. and multiwavelength data published in

H.E.S.S. Collaboration et al., Very high energy γ-ray emission from two blazars of unknown redshift and upper limits on their distance

Figure 2, left panel: KUV 00311-1938 H.E.S.S. observed spectra: [DAT]
The <E> column is the mean energy of the bin, and the dFlux column is the flux point, with the other colmuns being the respective uncertainties

Figure 2, right panel: PKS 1440-389 H.E.S.S. observed spectra: [DAT]
The <E> column is the mean energy of the bin, and the dFlux column is the flux point, with the other colmuns being the respective uncertainties

Figure 3, upper panel: KUV 00311-1938 MWL SED points: [CSV]
Because the H.E.S.S spectrum is integrated over a very long time period, each point comes with a MJD start and stop date.

Figure 3, lower panel: PKS 1440-389 MWL SED points: [CSV]
Since the H.E.S.S observations happened over a very short time period, there are no start and stop dates.