  The study of the elusive hot component ($T \gtrsim 10^7$ K) of the Milky Way
circumgalactic medium (CGM) is a novel topic to understand Galactic formation
and evolution. In this work, we use the stacking technique through 46 lines of
sight with Chandra ACIS-S HETG totaling over 10Ms of exposure time and 9 lines
of sight with ACIS-S LETG observations totaling over 1Ms of exposure time, to
study in absorption the presence of highly ionized metals arising from the
super-virial temperature phase of the CGM. Focusing in the spectral range $4 -
8$ $\r{A}$, we were able to confirm the presence of this hot phase with high
significance. We detected transitions of Si XIV K$\alpha$ (with total
significance of 6.0$\sigma$) and, for the first time, SXVI K (total
significance 4.8$\sigma$) in the rest frame of our own Galaxy. For S XVI
K$\alpha$ we found a column density of $1.50^{+0.44}_{-0.38} \times 10^{16}
\mathrm{cm}^{-2}$. For Si XIV K$\alpha$ we measured a column density of
$0.87\pm{0.16} \times 10^{16} \mathrm{cm}^{-2}$. The lines of sight used in
this work are spread across the sky, probing widely separated regions of the
CGM. Therefore, our results indicate that this newly discovered hot medium
extends throughout the halo, and is not related only to the Galactic Bubbles.
The hot gas location, distribution, and covering factor, however, remain
unknown. This component might contribute significantly to the missing baryons
and metals in the Milky Way.
