The period–luminosity relation for Mira variables in the Milky Way using Gaia DR3: a further distance anchor for <i>H</i>0

ABSTRACT Gaia DR3 parallaxes are used to calibrate preliminary period–luminosity relations of O-rich Mira variables in the 2MASS J, H, and Ks bands using a probabilistic model accounting for variations parallax zero-point underestimation uncertainties. The derived compared those measured Large Small Magellanic Clouds, Sagittarius dwarf spheroidal galaxy, globular cluster members, subset Milky Way with VLBI parallaxes. linear JHKs slightly steeper thus fainter at short period than corresponding LMC relations, suggesting population effects near-infrared perhaps larger previous observational works have claimed. Models astrometry suggest that, despite intrinsic photocentre wobble use mean photometry astrometric solution current data reduction, recovered should be on average unbiased but underestimated uncertainties nearest stars. recommended EDR3 corrections evaluated $\nu _\mathrm{eff}=1.25\, \mu \mathrm{m}^{-1}$ require minimal ($\lesssim 5\, \mathrm{as}$) redder five-parameter sources, overcorrect six-parameter most by factor ∼1.6 $G\approx 12.5\, \mathrm{mag}$. as anchors Type Ia host galaxy NGC 1559 find $H_0=(73.7\pm 4.4)\, \mathrm{km\, s}^{-1}\, \mathrm{Mpc}^{-1}$.