We have observed the dwarf galaxy IC 1613 , at multiple epochs in the mid–infrared using Spitzer and contemporaneously in the near–infrared using the new FourStar near-IR camera on Magellan .
We have constructed Cepheid period–luminosity relations in the J , H , K _ { s } , [ 3.6 ] and [ 4.5 ] bands and have used the run of their apparent distance moduli as a function of wavelength to derive the line–of–sight reddening and distance to IC 1613 .
Using a nine–band fit , we find E ( B - V ) = 0.05 \pm 0.01 mag and an extinction–corrected distance modulus of \mu _ { 0 } = 24.29 \pm 0.03 _ { statistical } \pm 0.03 _ { systematic } mag .
By comparing our multi–band and [ 3.6 ] distance moduli to results from the tip of the red giant branch and red clump distance indicators , we find that metallicity has no measurable effect on Cepheid distances at 3.6 \mu m in the metallicity range -1.0 \leq [ Fe / H ] \leq 0.2 , hence derivations of the Hubble constant at this wavelength require no correction for metallicity .