  The distribution of a pure condensible planetary atmosphere in equilibrium
with a surface reservoir is revisited employing the energy budget of the
climate system, emphasizing the atmospheric horizontal latent heat transport.
This configuration is applicable to icy Solar System bodies such as Triton as
well as a range of possible exoplanet atmospheres, including water or
$\mathrm{CO_2}$ iceballs or ocean worlds, and lava planets with mineral vapor
atmospheres. Climate regimes for slowly rotating planets with the hot-spot near
the substellar point, and for rapidly rotating planets with a warm equatorial
belt, are both treated. A non-dimensional parameter controlling the fractional
variation of the surface pressure is derived; it measures whether the pure
condensible atmosphere is global or localized. The global pure condensible
atmosphere with the non-dimensional parameter much less than order of unity is
maintained by the strong horizontal latent heat transport associated with an
"evaporation/sublimation-driven flow" from warm to cold places that compensates
for the incoming differential radiative forcing. We show that the variation of
surface temperature can be estimated in terms of this non-dimensional parameter
if it is not too large. In the case of a pure water-vapor atmosphere with an
ice or liquid surface, we show that the atmosphere is thick enough to maintain
nearly isothermal surface conditions even when the substellar surface
temperature is around the freezing point. Finally, it is proposed that the
evaporation/sublimation-driven flow regime for global atmospheres could be
detected via its effect on the inhomogeneous distribution of minor
non-condensible components in the atmosphere.
