01725nas a2200277   4500000000100000000000100001008004100002100001900043700001900062700001700081700002100098700002500119700001800144700002200162700001800184700001900202700002000221700002200241700001900263700002500282700002200307245007500329856004500404490000800449520099000457       2022                            d1 aGeorge N. Wong1 aBen S. Prather1 aVedant Dhruv1 aBenjamin R. Ryan1 aMonika Mościbrodzka1 aChi-Kwan Chan1 aAbhishek V. Joshi1 aRicardo Yarza1 aAngelo Ricarte1 aHotaka Shiokawa1 aJoshua C. Dolence1 aScott C. Noble1 aJonathan C. McKinney1 aCharles F. Gammie00aPATOKA: Simulating Electromagnetic Observables of Black Hole Accretion  uhttps://doi.org/10.3847/1538-4365/ac582e0 v2593 aThe Event Horizon Telescope (EHT) has released analyses of reconstructed images of horizon-scale millimeter emission near the supermassive black hole at the center of the M87 galaxy. Parts of the analyses made use of a large library of synthetic black hole images and spectra, which were produced using numerical general relativistic magnetohydrodynamics fluid simulations and polarized ray tracing. In this article, we describe the PATOKA pipeline, which was used to generate the Illinois contribution to the EHT simulation library. We begin by describing the relevant accretion systems and radiative processes. We then describe the details of the three numerical codes we use, iharm, ipole, and igrmonty, paying particular attention to differences between the current generation of the codes and the originally published versions. Finally, we provide a brief overview of simulated data as produced by PATOKA and conclude with a discussion of limitations and future directions.