We determine three independent Population II distance moduli to the Fornax dwarf spheroidal (dSph) galaxy, using wide-field, ground-based $VI$ imaging acquired with the Magellan-Baade telescope at Las Campanas Observatory. After subtracting 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 calibration based in the LMC giving a distance modulus of $\mu_0^\mathrm{ TRGB} = 20.80 \pm 0.037_\mathrm{ stat} \pm 0.057_\mathrm{ sys}$ mag. We determine an RR Lyrae (RRL) distance from template mean magnitudes, with periods adopted from the literature. Adopting a Gaia DR2 calibration of first overtone RRL period-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, we determine a distance from Fornax's horizontal branch (HB) and two galactic globular cluster calibrators, giving $\mu_0^\mathrm{ HB} = 20.83 \pm 0.03_\mathrm{ stat} \pm 0.09_\mathrm{ sys}$ mag. These distances are each derived from homogeneous IMACS photometry, are anchored to independent geometric zero-points, and utilize different classes of stars. We therefore average over independent 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).
Categories: astro-ph.GA astro-ph.CO