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Radiative transfer models of two transitional type Ia supernova (SNe Ia) havebeen produced using the abundance stratification technique. These two objects--designated SN 2007on and SN 2011iv-- both exploded in the same galaxy, NGC1404, which allows for a direct comparison. SN 2007on synthesised 0.25$M_{\odot}$ of $^{56}$Ni and was less luminous than SN 2011iv, which produced0.31 $M_{\odot}$ of $^{56}$Ni. SN 2007on had a lower central density($\rho_{c}$) and higher explosion energy ($E_{\rm kin}$ $\sim1.3\pm$0.3$\times10^{51}$erg) than SN 2011iv, and it produced less nuclearstatistical equilibrium (NSE) elements (0.06 $M_{\odot}$). Whereas, SN 2011ivhad a larger $\rho_{c}$, which increased the electron capture rate in thelowest velocity regions, and produced 0.35 $M_{\odot}$ of stable NSE elements.SN 2011iv had an explosion energy of $E_{\rm kin}$ $\sim 0.9\pm$0.2$\times10^{51}$erg. Both objects had an ejecta mass consistent with theChandrasekhar mass (Ch-mass), and their observational properties are welldescribed by predictions from delayed-detonation explosion models. Within thisframework, comparison to the sub-luminous SN 1986G indicates SN 2011iv and SN1986G have different transition densities ($\rho_{tr}$) but similar $\rho_{c}$.Whereas, SN 1986G and SN 2007on had a similar $\rho_{tr}$ but different$\rho_{c}$. Finally, we examine the colour-stretch parameter $s_{BV}$ vs.$L_{max}$ relation and determine that the bulk of SNe Ia (including thesub-luminous ones) are consistent with Ch-mass delayed-detonation explosions,where the main parameter driving the diversity is $\rho_{tr}$. We also find$\rho_{c}$ to be driving the second order scatter observed at the faint end ofthe luminosity-width relationship.

On the type Ia supernovae 2007on and 2011iv: Evidence for Chandrasekhar-mass explosions at the faint end of the luminosity-width relationship