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We determine three independent Population II distance moduli to the Fornaxdwarf spheroidal (dSph) galaxy, using wide-field, ground-based $VI$ imagingacquired with the Magellan-Baade telescope at Las Campanas Observatory. Aftersubtracting foreground stars using Gaia EDR3 proper motions, we measure an$I$-band tip of the red giant branch (TRGB) magnitude of $I_0^\mathrm{TRGB} =16.753 \pm 0.03_\mathrm{stat} \pm 0.037_\mathrm{sys}$ mag, with a calibrationbased in the LMC giving a distance modulus of $\mu_0^\mathrm{TRGB} = 20.80 \pm0.037_\mathrm{stat} \pm 0.057_\mathrm{sys}$ mag. We determine an RR Lyrae (RRL)distance from template mean magnitudes, with periods adopted from theliterature. Adopting a Gaia DR2 calibration of first overtone RRLperiod-luminosity and period-Wesenheit relations, we find $\mu_0^\mathrm{PLZ} =20.74 \pm 0.01_\mathrm{stat} \pm 0.12_\mathrm{sys}$ mag and $\mu_0^\mathrm{PWZ}= 20.68 \pm 0.02_\mathrm{stat} \pm 0.07_\mathrm{sys}$ mag. Finally, wedetermine a distance from Fornax's horizontal branch (HB) and two galacticglobular cluster calibrators, giving $\mu_0^\mathrm{HB} = 20.83 \pm0.03_\mathrm{stat} \pm 0.09_\mathrm{sys}$ mag. These distances are each derivedfrom homogeneous IMACS photometry, are anchored to independent geometriczero-points, and utilize different classes of stars. We therefore average overindependent uncertainties and report the combined distance modulus $\langle\mu_0\rangle = 20.770 \pm 0.042_\mathrm{stat} \pm 0.024_\mathrm{sys}$ mag(corresponding to a distance of $143\pm3$ kpc).

Distances to Local Group Galaxies via Population II, Stellar Distance Indicators. II. The Fornax Dwarf Spheroidal