  Central Compact Objects (CCOs), neutron stars found near the centre of some
Supernova Remnants (SNRs), have been almost exclusively studied in X-rays and
are thought to lack the wind nebulae typically seen around young,
rotation-powered pulsars. We present the first, spatially-resolved,
morphological and spectroscopic study of the optical nebula observed at the
location of CXOU J085201.4-461753, the CCO in the heart of the Vela Junior SNR.
It is currently the only Galactic CCO with a spatially coincident nebula
detected at optical wavelengths, whose exact nature remains uncertain. New MUSE
integral field spectroscopy data confirm that the nebula, shaped like a smooth
blob extending 8" in diameter, is dominated by [N II]$\lambda\lambda$6548,6583
emission. The data reveals a distinct and previously unobserved morphology of
the H$\alpha$ emission, exhibiting an arc-like shape reminiscent of a bow shock
nebula. We observe a significantly strong [N II] emission relative to
H$\alpha$, with the [N II]$\lambda\lambda$6548,6583 up to 34 times the
intensity of the H$\alpha$ emission within the optical nebula environment.
Notably, the [N II] and H$\alpha$ structures are not spatially coincident, with
the [N II] nebula concentrated to the south of the CCO and delimited by the
H$\alpha$ arc-like structure. We detect additional emission in [N I], He I, [S
II], [Ar III], [Fe II], and [S III]. We discuss our findings in the light of a
photoionization or Wolf-Rayet nebula, pointing to a very massive progenitor and
further suggesting that very massive stars do not necessarily make black holes.
