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Optical observations of the type IIb SN 2013df from a few days to about 250days after explosion are presented. These observations are complemented with UVphotometry taken by \textit{SWIFT} up to 60 days post-explosion. Thedouble-peak optical light curve is similar to those of SNe 1993J and 2011fualthough with different decline and rise rates. From the modelling of thebolometric light curve, we have estimated that the total mass of synthesised$^{56}$Ni in the explosion is $\sim0.1$ 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. Inaddition, we have estimated a lower limit to the progenitor radius ranging from$64-169$ $R_{\odot}$. The spectral evolution indicates that SN 2013df had ahydrogen envelope similar to SN 1993J ($\sim 0.2$ M$_{\odot}$). The lineprofiles in nebular spectra suggest that the explosion was asymmetric with thepresence of clumps in the ejecta, while the [O\,{\sc i}]$\lambda$$\lambda$$6300$, $6364$ luminosities, may indicate that the progenitorof SN 2013df was a relatively low mass star ( $\sim 12-13 $ M$_{\odot}$).

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