Nova Cen 2013 ( V1369 Cen ) is the fourth bright nova observed panchromatically through high resolution UV+optical multi epoch spectroscopy . It is also the nova with the richest set of spectra ( both in terms of data quality and number of epochs ) thanks to its exceptional brightness . Here , we use the late nebular spectra taken between day \sim 250 and day \sim 837 after outburst to derive the physical , geometrical and kinematical properties of the nova . We compare the results with those determined for the other panchromatic studies in this series : T Pyx , V339 Del ( nova Del 2013 ) , and V959 Mon ( nova Mon 2012 ) . From this we conclude that in all these novae the ejecta geometry and phenomenology can be consistently explained by clumpy gas expelled during a single , brief ejection episode and in ballistic expansion , and not by a wind . For V1369 Cen the ejecta mass ( \sim 1 \times 10 ^ { -4 } M \odot ) and filling factor ( 0.1 \leq f \leq 0.2 ) are consistent with those of classical novae but larger ( by at least an order of magnitude ) than those of T Pyx and the recurrent novae . V1369 Cen has an anomalously high relative to solar N/C ratio that is beyond the range currently predicted for a CO nova , and the Ne emission line strengths are dissimilar to those of typical ONe or CO white dwarfs .