  In this paper, we present a Ly$\alpha$ halo extended to $\sim200$ kpc
identified by stacking $\sim 3300$ Ly$\alpha$ emitters at $z=2.2-2.3$. We carry
out imaging observations and data reduction with Subaru/Hyper Suprime-Cam
(HSC). Our total survey area is $\sim12$ deg$^2$ and imaging depths are
$25.5-27.0$ mag. Using the imaging data, we select 1,240 and 2,101 LAE
candidates at $z=2.2$ and 2.3, respectively. We carry out spectroscopic
observations of our LAE candidates and data reduction with Magellan/IMACS to
estimate the contamination rate of our LAE candidates. We find that the
contamination rate of our sample is low (8%). We stack our LAE candidates with
a median stacking method to identify the Ly$\alpha$ halo at $z=2$. We show that
the Ly$\alpha$ halo is extended to $\sim200$ kpc at a surface brightness level
of $10^{-20}$ erg s$^{-1}$ cm$^{-2}$ arcsec$^{-2}$. Comparing to previous
studies, our Ly$\alpha$ halo is more extended at radii of $\sim25-100$ kpc,
which is not likely caused by the contamination in our sample but by different
redshifts and fields instead. To investigate how central galaxies affect
surrounding LAHs, we divide our LAEs into subsamples based on the Ly$\alpha$
luminosity ($L_{\rm Ly\alpha}$), rest-frame Ly$\alpha$ equivalent width
(EW$_0$), and UV magnitude (M$_{\rm uv}$). We stack the subsamples and find
that higher $L_{\rm Ly\alpha}$, lower EW$_0$, and brighter M$_{\rm uv}$ cause
more extended halos. Our results suggest that more massive LAEs generally have
more extended Ly$\alpha$ halos.
