Distance to the SMC
SMC distance determined with the accuracy of 3% using binary systems composed of giants.
The Araucaria Project. The Distance to the Small Magellanic Cloud from Late-type Eclipsing Binaries
D. Graczyk, G. Pietrzyński, I. Thompson, W. Gieren, B. Pilecki, P. Konorski, A. Udalski, I. Soszyński, S. Villanova, M. Górski, K. Suchomska, P. Karczmarek, R.-P. Kudritzki, F. Bresolin, A. Gallenne
We present a distance determination to the Small Magellanic Cloud (SMC) based on an analysis of four detached, long period, late type eclipsing binaries discovered by the OGLE Survey. The components of the binaries show negligible intrinsic variability. A consistent set of stellar parameters was derived with low statistical and systematic uncertainty. The absolute dimensions of the stars are calculated with a precision of better than 3%. Atmospheric parameters are derived from analysis with the MOOG code.
The surface brightness – infrared color relation was used to derive the distance to each binary. The four systems clump tightly around a distance modulus of (m-M)=18.99 mag with a dispersion of only 0.05 mag. They probably lie in a main body of the galaxy. Combining their distances with our previous published distance to the eclipsing binary OGLE SMC113.3 4007 we obtain a mean distance modulus to the SMC of 18.965 ± 0.025 (stat.) ± 0.048 (syst.) mag. This corresponds to a distance of 62.1 ± 1.9 kpc, where the error includes both uncertainties. The system OGLE SMC113.3 4007 lies in a foreground substructure of the SMC in so called Wing.
Taking into account other recent published determinations of the SMC distance we calculated the distance modulus difference between the SMC and the LMC equal to 0.458 ± 0.068 mag. Finally we advocate distance modulus m-M=18.95 ± 0.07 mag as a new “canonical” value of the distance modulus to this galaxy, where given error is dominated by uncertainties of the galaxy structure, its shape and total line-of-sight geometrical depth.