The interstellar medium surrounding the Scorpius-Centaurus association revisited

Aims. We want to make a large-scale study of the morphology, kinematics, and origin of the HI, which surrounds the Sco-Cen association. Methods. We combine our high-sensitivity southern HI survey with the Leiden/Dwingeloo Survey, considering l = 240 degrees-400 degrees, b = -60 degrees to +60 degrees, and radial velocities of V = -41.8 to +40.8 km s(-1). We point out the main HI branches surrounding the association and derive their kinematics. Kinematical H I-maps were compared with spatial maps of interstellar (IS) Na I from the literature. Upper limits for distances d were derived from optical IS absorption components from the literature. Models of expanding spherical H I shells were fitted around each stellar subgroup. Results. The expanding ring of HI associated with the Gould Belt (GB) is very prominent. At each 1, its radial velocity shifts similar to-7 km s(-1) within an interval Delta b similar to 10 degrees-25 degrees. On the sky, the shifts occur within a narrow stripe extending between l, b similar to 250 degrees, -18 degrees and 400 degrees, +50 degrees. The ranges of distances and radial thicknesses of most HI branches are nearly 70-160 pc and 40-90 pc, respectively. The shell-models fit the main branches. Interactions between the shells built a large expanding bubble with a transverse diameter of nearly 250 pc around the association. The near face is approaching with a mean velocity (V) over bar similar to -6.6 km s(-1) at d <= 76 pc from the Sun, covering about 102 degrees x 65 degrees (l, b), forming an H I-wall. There are streamers at (V) over bar similar to -15 to 35 km s(-1), as well as gas presumably overshot into Galactic Quadrant II. The receding gas is more tenuous. Conclusions. The association is traversing the ring since a time comparable to its age producing a significant disturbance on the expanding GB-ring of gas. The latter was almost totally shocked by the association, northerly of the stripe of velocity shifts. Southerly there are large amounts of preshocked gas, as well as smaller more localized shocked regions. Hot gas within the bubble produces most of the 1/4 keV radiation detected toward it by ROSAT. The total mass of the GB gas embedding the Sco-Cen association is estimated at M-1 similar to 368 000 M-circle dot +/- 60%, including similar to 34 000 M-circle dot of associated H-2 and 30% of He. About 39% of the embedding gas was shocked by the association. At vertical bar b vertical bar >= 35 degrees, a comparison of the observations with test points moving on ballistic orbits is consistent with the formation of the Sco-Cen association within the gas ring of the GB and the presumable explosive origin of the latter. The rotation of the ring is assumed.