Padova-Asiago Supernova Group
Highlights
SN 2013df, a double-peaked IIb supernova from a compact progenitor and an extended H envelope
Morales-Garoffolo, A. et al. 2014, MNRAS 445, 1467 (link to pdf)
Optical observations of the type IIb SN 2013df from a few days to about 250 days after explosion are presented. These observations are complemented with UV photometry taken by SWIFT up to 60 days post-explosion. The double-peak optical light curve is similar to those of SNe 1993J and 2011fu although with different decline and rise rates. From the modelling of the bolometric light curve, we have estimated that the total mass of synthesised Ni56 in the explosion is ~0.1 Msun, while the ejecta mass is 0.8-1.4 Msun and the explosion energy 0.4-1.2x10^51erg. In addition, we have estimated a lower limit to the progenitor radius ranging from 64-169 Rsun. The spectral evolution indicates that SN 2013df had a hydrogen envelope similar to SN 1993J (~0.2 Msun). The line profiles in nebular spectra suggest that the explosion was asymmetric with the presence of clumps in the ejecta, while the [OI] lambda 6300, 6364 luminosities, may indicate that the progenitor of SN 2013df was a relatively low mass star ( ~12-13 Msun). 20
Morales-Garoffolo, A. et al. 2014, MNRAS 445, 1467 (link to pdf)
Optical observations of the type IIb SN 2013df from a few days to about 250 days after explosion are presented. These observations are complemented with UV photometry taken by SWIFT up to 60 days post-explosion. The double-peak optical light curve is similar to those of SNe 1993J and 2011fu although with different decline and rise rates. From the modelling of the bolometric light curve, we have estimated that the total mass of synthesised Ni56 in the explosion is ~0.1 Msun, while the ejecta mass is 0.8-1.4 Msun and the explosion energy 0.4-1.2x10^51erg. In addition, we have estimated a lower limit to the progenitor radius ranging from 64-169 Rsun. The spectral evolution indicates that SN 2013df had a hydrogen envelope similar to SN 1993J (~0.2 Msun). The line profiles in nebular spectra suggest that the explosion was asymmetric with the presence of clumps in the ejecta, while the [OI] lambda 6300, 6364 luminosities, may indicate that the progenitor of SN 2013df was a relatively low mass star ( ~12-13 Msun). 20
