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Key information about the progenitor system and the explosion mechanism ofType Ia supernovae (SNe~Ia) can be obtained from early observations, within afew days from explosion. iPTF16abc was discovered as a young SN~Ia withexcellent early time data. Here, we present photometry and spectroscopy of theSN in the nebular phase. A comparison of the early time data with a sample ofSNe~Ia shows distinct features, differing from normal SNe~Ia at early phasesbut similar to normal SNe~Ia at a few weeks after maximum light (i.e. thetransitional phase) and well into the nebular phase. The transparencytimescales ($t_0$) for this sample of SNe~Ia range between $\sim$ 25 and 41days indicating a diversity in the ejecta masses. $t_0$ also weakly correlateswith the peak bolometric luminosity, consistent with the interpretation thatSNe with higher ejecta masses would produce more $^{56}$Ni. Comparing the $t_0$and the maximum luminosity, L$_{max}$\, distribution of a sample of SNe~Ia topredictions from a wide range of explosion models we find an indication thatthe sub-Chandrasekhar mass models span the range of observed values. However,the bright end of the distribution can be better explained by Chandrasekharmass delayed detonation models, hinting at multiple progenitor channels toexplain the observed bolometric properties of SNe~Ia. iPTF16abc appears to beconsistent with the predictions from the M$_{ch}$ models.

iPTF16abc and the population of Type Ia supernovae: Comparing the photospheric, transitional and nebular phases