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Pan, Y.-C; Foley, R. J; Kromer, M; Fox, O. D; Zheng, W; Challis, P; Clubb, K. I; Filippenko, A. V; Folatelli, G; Graham, M. L; Hillebrandt, W; Kirshner, R. P; Lee, W. H; Pakmor, R; Patat, F; Phillips, M. M; Pignata, G; Röpke, F; Seitenzahl, I; Silverman, J. M; Simon, J. D; Sternberg, A; Stritzinger, M. D; Taubenberger, S; Vinko, J; Wheeler, J. C
Monthly notices of the Royal Astronomical Society, 10/2015, Volume: 452, Issue: 4Journal Article
SN 2013dy is a Type Ia supernova (SN Ia) for which we have compiled an extraordinary data set spanning from 0.1 to ∼ 500 d after explosion. We present 10 epochs of ultraviolet (UV) through near-infrared (NIR) spectra with Hubble Space Telescope/Space Telescope Imaging Spectrograph, 47 epochs of optical spectra (15 of them having high resolution), and more than 500 photometric observations in the BVrRiIZYJH bands. SN 2013dy has a broad and slowly declining light curve (Δm 15(B) = 0.92 mag), shallow $\mathrm{Si}\,\small {II}\,\lambda 6355$ absorption, and a low velocity gradient. We detect strong C ii in our earliest spectra, probing unburned progenitor material in the outermost layers of the SN ejecta, but this feature fades within a few days. The UV continuum of SN 2013dy, which is strongly affected by the metal abundance of the progenitor star, suggests that SN 2013dy had a relatively high-metallicity progenitor. Examining one of the largest single set of high-resolution spectra for an SN Ia, we find no evidence of variable absorption from circumstellar material. Combining our UV spectra, NIR photometry, and high-cadence optical photometry, we construct a bolometric light curve, showing that SN 2013dy had a maximum luminosity of $10.0^{+4.8}_{-3.8} \times 10^{42}$ erg s−1. We compare the synthetic light curves and spectra of several models to SN 2013dy, finding that SN 2013dy is in good agreement with a solar-metallicity W7 model.
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