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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 4.

Rest-frame nebular-phase (+236, middle panel, and 264, bottom panel, days form B-band maximum) spectra of SN 2018oh. We show the 3.5 Å binned spectra with gray and the 100 Å smoothed with black solid lines, respectively. We compare the spectra with the +230 days SN 2011fe spectrum (red; Graham et al. 2015) and the +286 days SN 2017cbv spectrum (blue; Sand et al. 2018). All spectra are normalized to the flux of SN 2018oh in the r-band of the Swope telescope at its corresponding phase, for which we plot the response functions of its broadband filters at the top panel. We also mark four iron-peak elements’ nebular-phase lines (vertical dashed black lines) and the three zero-velocity positions of the expected interaction lines from hydrogen and helium in the interaction scenario (vertical dashed orange lines). The data used to create this figure are available.

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