  Coronal condensation and rain are a crucial part of the mass cycle between
the corona and chromosphere. In some cases, condensation and subsequent rain
originate in the magnetic dips formed during magnetic reconnection. This
provides a new and alternative formation mechanism for coronal rain. Until now,
only off-limb, rather than on-disk, condensation events during reconnection
have been reported. In this paper, employing extreme-ultraviolet (EUV) images
of the Solar Terrestrial Relations Observatory (STEREO) and Solar Dynamics
Observatory (SDO), we investigate the condensations facilitated by reconnection
from 2011 July 14 to 15, when STEREO was in quadrature with respect to the
Sun-Earth line. Above the limb, in STEREO/EUV Imager (EUVI) 171 \AA~images,
higher-lying open structures move downward, reconnect with the lower-lying
closed loops, and form dips. Two sets of newly reconnected structures then
form. In the dips, bright condensations occur in EUVI 304 \AA~images repeatedly
which then flow downward to the surface. In the on-disk observations by
SDO/Atmospheric Imaging Assembly (AIA) in the 171 \AA~channel, these magnetic
structures are difficult to identify. Dark condensations appear in AIA 304
\AA~images, and then move to the surface as on-disk coronal rain. The cooling
and condensation of coronal plasma is revealed by the EUV light curves. If only
the on-disk observations would be available, the relation between the
condensations and reconnection, shown clearly by the off-limb observations,
would not be identified. Thus, we suggest that some on-disk condensation events
seen in transition region and chromospheric lines may be facilitated by
reconnection.
