http://arxiv.org/abs/1612.02805
Shock-cooling models provide robust predictions for the early time emission from core-collapse SNe. Modern surveys have begun discovering and following SNe shortly after first light—providing first measurements of the rise of Type II SNe. We explore how shock cooling models can constrain the progenitor’s radius, explosion velocity, and local host extinction. We fit synthetic photometry in several realistic observing scenarios and find that ultraviolet observations can constrain the progenitor’s radius to a statistical uncertainty of $\pm10-15\%$, with a systematic uncertainty of $\pm 20\%$. With these observations the local host extinction can be constrained to $\pm0.05$ mag and the velocity to $\pm 5\%$ with a systematic uncertainty of $\pm 10\%$. We also re-analyze the SN light curves presented in Garnavich et al (2016) and find that KSN2011a can be fit by a BSG model with a progenitor radius of $R_s = 10_{-7{\rm (stat)}}^{+37 {\rm (stat)}} \phantom{}_{-1 {\rm (sys)}}^{+8 {\rm (sys)}}$ R$_\odot$, while KSN2011d can be fit with a RSG model with a progenitor radius of $R_s = 140_{-47 {\rm (stat)}}^{+91 {\rm (stat)}} \phantom{}_{-28 {\rm (sys)}}^{+23 {\rm (sys)}}$ R$_\odot$. Our results do not agree with those of Garnavich et al (2016). Moreover, we re-evaluate their claims and find that there is no statistically significant evidence for shock breakout in the light curve of KSN 2011d.
A. Rubin and A. Gal-Yam
Fri, 9 Dec 16
52/62
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