  We present photometry, spectroscopy, and host-galaxy integral-field
spectroscopy of the Type II supernova (SN) 2016esw in CGCG~229-009 from the
first day after the explosion up to 120 days. Its light-curve shape is similar
to that of a typical SN II; however, SN 2016esw is near the high-luminosity end
of the SN II distribution, with a peak of $M^{\rm max}_{V}=-18.36$ mag. The
$V$-band light curve exhibits a long recombination phase for a SN II (similar
to the long-lived plateau of SN 2004et). Considering the well-known relation
between the luminosity and the plateau decline rate, SN 2016esw should have a
$V$-band slope of $\sim 2.10$ mag (100 days)$^{-1}$; however, SN 2016esw has a
substantially flatter plateau with a slope of $1.01\pm 0.26$ mag (100
days)$^{-1}$, perhaps indicating that interacting Type II supernovae are not
useful for cosmology. At 19.5 days post-explosion, the spectrum presents a boxy
H$\alpha$ emission line with flat absorption profiles, suggesting interaction
between the ejecta and circumstellar matter. Finally, based on the spectral
properties, SN 2016esw shows similarities with the luminous and interacting SN
2007pk at early epochs, particularly in terms of observable line features and
their evolution.
