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It has recently become possible to zoom-in from cosmological to sub-pc scalesin galaxy simulations to follow accretion onto supermassive black holes(SMBHs). However, at some point the approximations used on ISM scales (e.g.optically-thin cooling and stellar-population-integrated star formation [SF]and feedback [FB]) break down. We therefore present the first cosmologicalradiation-magnetohydrodynamic (RMHD) simulation which self-consistentlycombines the FIRE physics (relevant on galactic/ISM scales where SF/FB areensemble-averaged) and STARFORGE physics (relevant on small scales where wetrack individual (proto)stellar formation and evolution), together withexplicit RMHD (including non-ideal MHD and multi-band M1-RHD) whichself-consistently treats both optically-thick and thin regimes. This allows usto span scales from ~100 Mpc down to <100 au (~300 Schwarzschild radii) arounda SMBH at a time where it accretes as a bright quasar, in a single simulation.We show that accretion rates up to $\sim 10-100\,{\rm M_{\odot}\,yr^{-1}}$ canbe sustained into the accretion disk at $\ll 10^{3}\,R_{\rm schw}$, withgravitational torques between stars and gas dominating on sub-kpc scales untilstar formation is shut down on sub-pc scales by a combination of optical depthto cooling and strong magnetic fields. There is an intermediate-scale,flux-frozen disk which is gravitoturbulent and stabilized by magnetic pressuresustaining strong turbulence and inflow with persistent spiral modes. In thispaper we focus on how gas gets into the small-scale disk, and how starformation is efficiently suppressed.

FORGE'd in FIRE: Resolving the End of Star Formation and Structure of AGN Accretion Disks from Cosmological Initial Conditions