MUSE sneaks a peek at extreme ram‐pressure events III. Tomography of UGC 6697, a massive galaxy falling into Abell 1367

International audienceWe present the MUSE observations of UGC 6697, a giant (M‐* approximate to 10(10) M‐circle dot) spiral galaxy infalling in the nearby cluster Abell 1367. During its high‐velocity transit through the intracluster medium (ICM), the hydrodynamical interactions with the ICM produce a approximate to 100 kpc tail of ionized gas that we map with a mosaic of five MUSE pointings up to 60 kpc from the galaxy. CGCG 97087N, a small companion that lies at few arcminutes in projection from UGC 6697, is also showing signs of the hydrodynamic action of the ICM of the cluster. Along the whole extent of the tail, we detect diffuse H alpha emission, and to a lesser extent, H beta, [OIII] lambda 5007, and [OI] lambda 6300. By comparing the kinematics and distribution of gas and stars (as traced by the CaII triplet) for both galaxies, we separate the ionized gas, as traced by the H alpha line, into a component that is still bound to the galaxy and a component that is stripped. We find that the bound component shows a low‐velocity dispersion and line ratios consistent with photoionization by hot stars. The stripped gas is more turbulent, with velocity dispersions up to greater than or similar to 100 km s(‐1), and is excited by shocks, as traced by high values of [OI]/H alpha and [NII]/H alpha ratio. In the tail of UGC 6697, we identify numerous bright compact knots with line ratios typical of HII regions. These are distributed along the only streams of stripped gas that retain low‐velocity dispersions (less than or similar to 35 km s(‐1)). Despite being in the stripped gas, their physical properties are not different from normal HII regions in galactic disks. We find evidence of a past fast encounter between the two galaxies in the form of a double tail emerging from CGCG 97087N that connects with UGC 6697. This encounter might have increased the efficiency of the stripping process, leaving the stellar distribution and kinematics unaltered