SN 2013df, a double-peaked IIb supernova from a compact progenitor and an extended H envelope

Abstract

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 \textit{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 ${}^{56}$Ni in the explosion is $\sim 0.1$ M${}_{\odot }$, while the ejecta mass is $0.8-1.4$ M${}_{\odot }$ and the explosion energy $0.4-1.2\times 10^{51}$erg. In addition, we have estimated a lower limit to the progenitor radius ranging from $64-169$ $R_{\odot }$. The spectral evolution indicates that SN 2013df had a hydrogen envelope similar to SN 1993J ($\sim 0.2$ M${}_{\odot }$). The line profiles in nebular spectra suggest that the explosion was asymmetric with the presence of clumps in the ejecta, while the [O\,{\sc i}] $\lambda$$\lambda$$6300$, $6364$ luminosities, may indicate that the progenitor of SN 2013df was a relatively low mass star ( $\sim 12-13$ M${}_{\odot }$).

18 pages, 11 figures, 9 tables, accepted for publication in MNRAS

References in corpus (10)

• Nucleosynthesis and Remnants in Massive Stars of Solar Metallicity
• Mass loss from hot massive stars
• Empirical Color Transformations Between SDSS Photometry and Other Photometric Systems
• Determining the Type, Redshift, and Age of a Supernova Spectrum
• A Wolf-Rayet-like progenitor of supernova SN 2013cu from spectral observations of a wind
• The Broad-lined Type Ic SN 2003jd
• Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
• The type IIb SN 2008ax: the nature of the progenitor
• The type IIb SN 2008ax: spectral and light curve evolution
• ESC Supernova spectroscopy of non-ESC targets

Cited by in corpus (3)

• Constraints on the Progenitor of SN 2016gkg From Its Shock-Cooling Light Curve
• The progenitor and early evolution of the Type IIb SN 2016gkg
• A likely inverse-Compton emission from the Type IIb SN 2013df