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We present the discovery of J22564-5910, a new type of hot subdwarf (sdB)which shows evidence of gas present in the system and has shallow, multi-peakedhydrogen and helium lines which vary in shape over time. All observationalevidence points towards J22564-5910 being observed very shortly after themerger phase that formed it. Using high-resolution, high signal-to-noisespectroscopy, combined with multi-band photometry, Gaia astrometry, and TESSlight curves, we aim to interpret these unusual spectral features. Thephotometry, spectra and light curves are all analyzed, and their results arecombined in order to support our interpretation of the observations: the likelypresence of a magnetic field combined with gas features around the sdB. Basedon the triple-peaked H lines, the magnetic field strength is estimated and, byusing the shellspec code, qualitative models of gas configurations are fittedto the observations. All observations can either be explained by a magneticfield of ~650 kG which enables the formation of a centrifugal magnetosphere, ora non-magnetic hot subdwarf surrounded by a circumstellar gas disk/torus. Bothscenarios are not mutually exclusive and both can be explained by a recentmerger. J22564-5910 is the first object of its kind. It is a rapidly spinningsdB with gas still present in the system. It is the first post-merger starobserved this early after the merger event, and as such is very valuable systemto test merger theories. If the magnetic field can be confirmed, it is not onlythe first magnetic sdB, but it hosts the strongest magnetic field ever found ina pre-white dwarf object. Thus, it could represent the long-sought forimmediate ancestor of strongly magnetic WDs.

Looking into the cradle of the grave: J22564-5910, a young post-merger hot subdwarf?