  The Keck Planet Imager and Characterizer (KPIC) is a purpose-built instrument
for high-dispersion coronagraphy in the K and L bands on Keck. This instrument
will provide the first high resolution (R$>$30,000) spectra of known directly
imaged exoplanets and low-mass brown dwarf companions visible in the northern
hemisphere.
  KPIC is developed in phases. Phase I is currently at Keck in the early
operations stage, and the phase II upgrade will deploy in late 2021. The goal
of phase II is to maximize the throughput for planet light and minimize the
stellar leakage, hence reducing the exposure time needed to acquire spectra
with a given signal-to-noise ratio. To achieve this, KPIC phase II exploits
several innovative technologies that have not been combined this way before.
These include a 1000-element deformable mirror for wavefront correction and
speckle control, a set of lossless beam shaping optics to maximize coupling
into the fiber, a pupil apodizer to suppress unwanted starlight, a pupil plane
vortex mask to enable the acquisition of spectra at and within the diffraction
limit, and an atmospheric dispersion compensator. These modules, when combined
with the active fiber injection unit present in phase I, will make for a highly
efficient exoplanet characterization platform.
  In this paper, we will present the final design of the optics and
opto-mechanics and highlight some innovative solutions we implemented to
facilitate all the new capabilities. We will provide an overview of the
assembly and laboratory testing of the sub-modules and some of the results.
Finally, we will outline the deployment timeline.
