We present late-time spectra of eight Type Ia supernovae (SNe Ia) obtained at >200 days after peak brightness using the Gemini South and Keck telescopes. All of the SNe Ia in our sample were nearby, well separated from their host galaxy's light, and have early-time photometry and spectroscopy from the Las Cumbres Observatory (LCO). Parameters are derived from the light curves and spectra such as peak brightness, decline rate, photospheric velocity, and the widths and velocities of the forbidden nebular emission lines. We discuss the physical interpretations of these parameters for the individual SNe Ia and the sample in general, including comparisons to well-observed SNe Ia from the literature. There are possible correlations between early-time and late-time spectral features that may indicate an asymmetric explosion, so we discuss our sample of SNe within the context of models for an offset ignition and/or white dwarf collisions. A subset of our late-time spectra are uncontaminated by host emission, and we statistically evaluate our nondetections of Hα emission to limit the amount of hydrogen in these systems. Finally, we consider the late-time evolution of the iron emission lines, finding that not all of our SNe follow the established trend of a redward migration at >200 days after maximum brightness.
@article{arxiv.1708.07799,
title = {Nebular-Phase Spectra of Nearby Type Ia Supernovae},
author = {Melissa L. Graham and Sahana Kumar and Griffin Hosseinzadeh and Daichi Hiramatsu and Iair Arcavi and D. Andrew Howell and Stefano Valenti and David J. Sand and Jerod T. Parrent and Curtis McCully and Alexei V. Filippenko},
journal= {arXiv preprint arXiv:1708.07799},
year = {2017}
}