  We present a study of a sample of 45 spectroscopically confirmed, UV luminous
galaxies at $z\sim 6$. They were selected as bright Lyman-break galaxies (LBGs)
using deep multi-band optical images in more than 2 deg$^2$ of the sky, and
subsequently identified via their strong Ly$\alpha$ emission. The majority of
these LBGs span an absolute UV magnitude range from $-22.0$ to $-20.5$ mag with
Ly$\alpha$ equivalent width (EW) between $\sim$10 and $\sim$200 \AA,
representing the most luminous galaxies at $z\sim 6$ in terms of both UV
continuum emission and Ly$\alpha$ line emission. We model the SEDs of 10 LBGs
that have deep infrared observations from HST, JWST, and/or Spitzer, and find
that they have a wide range of stellar masses and ages. They also have high
star-formation rates ranging from a few tens to a few hundreds of Solar mass
per year. Five of the LBGs have JWST or HST images and four of them show
compact morphology in these images, including one that is roughly consistent
with a point source, suggesting that UV luminous galaxies at this redshift are
generally compact. The fraction of our photometrically selected LBGs with
strong Ly$\alpha$ emission ($\mathrm{EW}>25$ \AA) is about $0.2$, which is
consistent with previous results and supports a moderate evolution of the IGM
opacity at the end of cosmic reionization. Using deep X-ray images, we do not
find evidence of strong AGN activity in these galaxies, but our constraint is
loose and we are not able to rule out the possibility of any weak AGN activity.
