  We present the first results from a CARMA high-resolution $^{12}$CO(1-0),
$^{13}$CO(1-0), and C$^{18}$O(1-0) molecular line survey of the North America
and Pelican (NAP) Nebulae. CARMA observations have been combined with
single-dish data from the Purple Mountain 13.7m telescope to add short spacings
and produce high-dynamic-range images. We find that the molecular gas is
predominantly shaped by the W80 HII bubble that is driven by an O star. Several
bright rims are probably remnant molecular clouds heated and stripped by the
massive star. Matching these rims in molecular lines and optical images, we
construct a model of the three-dimensional structure of the NAP complex. Two
groups of molecular clumps/filaments are on the near side of the bubble, one
being pushed toward us, whereas the other is moving toward the bubble. Another
group is on the far side of the bubble and moving away. The young stellar
objects in the Gulf region reside in three different clusters, each hosted by a
cloud from one of the three molecular clump groups. Although all gas content in
the NAP is impacted by feedback from the central O star, some regions show no
signs of star formation, while other areas clearly exhibit star formation
activity. Other molecular gas being carved by feedback includes the cometary
structures in the Pelican Head region and the boomerang features at the
boundary of the Gulf region. The results show that the NAP complex is an ideal
place for the study of feedback effects on star formation.
