The Spectacular Ultraviolet Flash From the Peculiar Type Ia Supernova 2019yvq

Abstract

Early observations of Type Ia supernovae (SNeIa) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN2019yvq, the second observed SNIa, after iPTF14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for an SNIa ($M_g\approx -18.5$mag at peak) yet featured very high absorption velocities ($v\approx 15,000{\mathrm{km}\mathrm{s}}^{-1}$ for Si II $\lambda$6355 at peak). We find that many of the observational features of SN2019yvq, aside from the flash, can be explained if the explosive yield of radioactive ${}^{56}\mathrm{Ni}$ is relatively low (we measure $M_{{}^{56}\mathrm{Ni}}=0.31\pm 0.05M_{\odot }$) and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of ${}^{56}\mathrm{Ni}$ in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations; it is clear additional tuning is required to better match SN2019yvq. In closing, we predict that the nebular spectra of SN2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca II] emission, if it was a double detonation, or narrow [O I] emission, if it was due to a violent merger.

arXiv comment27 pages, 14 figures, accepted in ApJ

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