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Central Compact Objects (CCOs), neutron stars found near the centre of someSupernova Remnants (SNRs), have been almost exclusively studied in X-rays andare 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 thelocation 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 nebuladetected at optical wavelengths, whose exact nature remains uncertain. New MUSEintegral field spectroscopy data confirm that the nebula, shaped like a smoothblob extending 8" in diameter, is dominated by [N II]$\lambda\lambda$6548,6583emission. The data reveals a distinct and previously unobserved morphology ofthe H$\alpha$ emission, exhibiting an arc-like shape reminiscent of a bow shocknebula. We observe a significantly strong [N II] emission relative toH$\alpha$, with the [N II]$\lambda\lambda$6548,6583 up to 34 times theintensity of the H$\alpha$ emission within the optical nebula environment.Notably, the [N II] and H$\alpha$ structures are not spatially coincident, withthe [N II] nebula concentrated to the south of the CCO and delimited by theH$\alpha$ arc-like structure. We detect additional emission in [N I], He I, [SII], [Ar III], [Fe II], and [S III]. We discuss our findings in the light of aphotoionization or Wolf-Rayet nebula, pointing to a very massive progenitor andfurther suggesting that very massive stars do not necessarily make black holes.

MUSE observations of the optical nebula surrounding the central compact object in the Vela Junior Supernova Remnant