OPTICAL GRAVITATIONAL LENSING EXPERIMENT - DISTANCE TO THE MAGELLANICCLOUDS WITH THE RED CLUMP STARS - ARE THE MAGELLANIC CLOUDS 15-PERCENT CLOSER THAN GENERALLY ACCEPTED

We present a new distance determination to the Large and Small Magella nic Clouds using the newly developed red clump stars method (Paczynski and Stanek 1998). This new, single-step, Hipparcos calibrated method seems to be one of the most precise techniques of distance determinati on with very small statistical error due to large number of red clump stars usually available. The distances were determined independently a long four lines-of-sight located at opposite sides of each Magellanic Cloud. The results for each line-of-sight are very consistent. For the SMC we obtain the distance modulus: m - M = 18.56 +/- 0.03 +/- 0.06 m ag (statistical and systematic errors, respectively) and for the LMC: m - M = 18.08 +/- 0.03 +/- 0.12 mag where systematic errors are mostly due to uncertainty in reddening estimates. Both distances will be ref ined and systematic errors reduced when accurate reddening maps for ou r fields are available. Distance moduli to bath Magellanic Clouds are approximate to 0.4 mag smaller than generally accepted values. The mod ulus to the LMC is in good agreement with the recent determinations fr om RR Lyrae type stars and upper limit resulting from the SN1987A echo . We suspect that the distance to the LMC and SMC Is shorter by about 15% than previously assumed: 42 kpc and 52 kpc, respectively. Calibrat ions of the period-luminosity relation for Cepheids which give overest imated distances to the LMC and SMC are probably incorrect and require urgent reanalysis. We also present our color-magnitude diagrams aroun d the red clump for the LMC and SMC. We identify vertical red clump, f irst noted by Zaritsky and Lin (1997), in the color-magnitude diagram of both Magellanic Clouds and we interpret it as an evolutionary featu re rather than unknown stellar population between the LMC and our Gala xy.