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Nebular Spectroscopy of Kepler’s Brightest Supernova

• Authors: G. Dimitriadis, C. Rojas-Bravo, C.D. Kilpatrick, R.J. Foley, A.L. Piro, J.S. Brown, P. Guhathakurta, A.C.N. Quirk, A. Rest, G.M. Strampelli, B.E. Tucker, and A. Villar

2019 The Astrophysical Journal Letters 870 L14.

• Provider: AAS Journals

Caption: Figure 5.

DEIMOS spectrum of SN 2018oh zoomed in to show Hα (top panel), He I λ5875 (middle panel), and He I λ6678 (bottom panel). The flux is adjusted to what would have been seen 200 days after maximum brightness. The underlying continuum, which we approximate with a Savitsky–Golay smoothed (with a 180 Å filter) version of the spectrum, is displayed as blue solid lines. The gray-shaded region corresponds the ±22 Å (roughly 1000 km s−1) region around the rest wavelength of each line. In red, we insert a feature at the rest-wavelength of each line with a FWHM of 1000 km s−1 and a height corresponding to our 3σ detection limit above the smoothed continuum. With a dashed black line, we also show how such a feature would look in the data. For each feature, we also display the residuals relative to the continuum.