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Type IIn SNe show spectral evidence for strong interaction between theirblast wave and dense circumstellar material (CSM) around the progenitor star.SN2010jl was the brightest core-collapse SN in 2010, and it was a Type IInexplosion with strong CSM interaction. Andrews et al. recently reportedevidence for an IR excess in SN2010jl, indicating either new dust formation orthe heating of CSM dust in an IR echo. Here we report multi-epoch spectra ofSN2010jl that reveal the tell-tale signature of new dust formation:emission-line profiles becoming systematically more blueshifted as the red sideof the line is blocked by increasing extinction. The effect is seen clearly inthe intermediate-width (400--4000 km/s) component of H$\alpha$ beginningroughly 30d after explosion. Moreover, we present near-IR spectra demonstratingthat the asymmetry in the hydrogen-line profiles is wavelength dependent,appearing more pronounced at shorter wavelengths. This evidence suggests thatnew dust grains had formed quickly in the post-shock shell of SN 2010jl arisingfrom CSM interaction. Since the observed dust temperature has been attributedto an IR echo and not to new dust, either (1) IR excess emission at $\lambda <5 \mu$m is not a particularly sensitive tracer of new dust formation in SNe, or(2) some assumptions about expected dust temperatures might require furtherstudy. Lastly, we discuss one possible mechanism other than dust that mightlead to increasingly blueshifted line profiles in SNeIIn, although thewavelength dependence of the asymmetry argues against this hypothesis in thecase of SN2010jl.

Systematic Blueshift of Line Profiles in the Type IIn Supernova 2010jl: Evidence for Post-Shock Dust Formation?