Abstract
Context. The method of distance determination of eclipsing binaries consists in combining the radii of both components determined from spectro-photometric observations with their respective angular diameters derived from the surface brightness-color relation (SBC). However, the largest limitation of the method comes from the uncertainty on the SBC relation: about 2% for late-type stars (or 0.04 magnitude) and more than 10% for early-type stars (or 0.2 mag).
Highlights
The distance measurements to extragalactic targets in the last century revolutionized our understanding of the distance scale of the universe
For γ Ori, our angular diameter is consistent with the value derived from the Narrabri Stellar Intensity
Taking advantage of the unique Visible spEctroGraph and polArimeter (VEGA)/Center for High Angular Resolution Astronomy (CHARA) capabilities in terms of spatial resolution, we determined the angular diameters of eight bright early-type stars in the visible with a precision of about 1.5%
Summary
The distance measurements to extragalactic targets in the last century revolutionized our understanding of the distance scale of the universe. The main goal of the long term program called the Araucaria project is to significantly improve the calibration of the cosmic distance scale based on observations of several distance indicators in nearby galaxies (Gieren et al 2005). Thirteen long period systems composed of late-type giants were analyzed in the Magellanic Clouds so far: eight in the Large Magellanic Cloud (Pietrzynski et al 2009, 2013), and five in the Small Magellanic Cloud (Graczyk et al 2012, 2014).
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