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The Galactic Center (GC) has been long known to host gamma-ray emissiondetected to >10 TeV. HESS data now points to two plausible origins: thesupermassive black hole (perhaps with >PeV cosmic rays and neutrinos) orhigh-energy electrons from the putative X-ray pulsar wind nebula G359.95-0.04observed by Chandra and NuSTAR. We show that if the magnetic field experiencedby PWN electrons is near the several mG ambient field strength suggested byradio observations of the nearby GC magnetar SGR J1745-29, synchrotron lossesconstrain the TeV gamma-ray output to be far below the data. Accounting for thepeculiar geometry of GC infrared emission, we also find that the requisite TeVflux could be reached if the PWN is ~1 pc from Sgr A* and the magnetic field istwo orders of magnitude weaker, a scenario that we discuss in relation torecent data and theoretical developments. Otherwise, Sgr A* is left, whichwould then be a PeV link to other AGN.

A Tale of Two Pulsars and the Origin of TeV Gamma Rays from the Galactic Center