  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 ~250 and day ~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 (about 1E-4 solar masses) and filling factor (0.1<=f<=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.
