  Previous studies have shown strong evidence that the Sun is crossing an
outflow originating from the Sco-Cen OB association. Understanding this
outflow's origin and structure illuminates how massive star formation shapes
the interstellar medium (ISM) and helps predict future Galactic conditions
affecting our Solar System. We analysed H I emission and optical ISM absorption
lines towards 47 early-type stars around the Upper Sco region to refine the map
of the Sco-Cen outflow. Combined with data for nearby stars, we find that the
outflow has at least two components: a faster, low-density component traced by
Ca II, and a slower, possibly lower-density component traced by Mg II and Fe II
in the UV that is passing through the Earth. A constant flow model successfully
describes both components with $(l,b,|\vec{v}|) = (335.4^{\circ}, -6.8^{\circ},
14.0 \,\,\textrm{km}\,\textrm{s}^{-1})$ and $(305.5^{\circ}, +17.6^{\circ},
21.2\,\,\textrm{km}\,\textrm{s}^{-1})$, respectively. The origin of the faster
component points towards the Sco-Cen 15 Myr population, which is consistent
with the origin of the slower component within 2 $\sigma$. A simple model
comparison indicates that a constant flow is favoured over a spherical flow
geometry, implying an extended distribution of feedback sources within Sco-Cen.
We also found that a poorly studied 25 pc long H I cloud at a distance of 107
pc belongs to the established Sco-Cen flow.
