  Unusual extinction curves of high-redshift QSOs have been taken as evidence
that dust is primarily produced by supernovae at high redshift. In particular,
the 3000 A Todini-Ferrara-Maiolino kink in the extinction curve of the z = 6.20
SDSS J1048+4637 has been attributed to supernova dust. Here we discuss the
challenges in inferring robust extinction curves of high-redshift QSOs and
critically assess previous claims of detection of supernova dust. In
particular, we address the sensitivity to the choice of intrinsic QSO spectrum,
the need for a long wavelength baseline, and the drawbacks in fitting
theoretical extinction curves. In a sample of 21 QSOs at z ~ 6 we detect
significant ultraviolet extinction using existing broad-band optical,
near-infrared, and Spitzer photometry. The median extinction curve is
consistent with a Small Magellanic Cloud curve with A_1450 ~ 0.7 mag and does
not exhibit any conspicuous (restframe) 2175 A or 3000 A features. For two
QSOs, SDSS J1044-0125 at z = 5.78 and SDSS J1030+0524 at z = 6.31, we further
present X-shooter spectra covering the wavelength range 0.9-2.5 um. The
resulting non-parametric extinction curves do not exhibit the 3000 A kink.
Finally, in a re-analysis of literature spectra of SDSS J1048+4637, we do not
find evidence for a conspicuous kink. We conclude that the existing evidence
for a 3000 A feature is weak and that the overall dust properties at high and
low redshift show no significant differences. This, however, does not preclude
supernovae from dominating the dust budget at high redshift.
