J. Kaluzny

COLOR-MAGNITUDE DIAGRAM DISTRIBUTION OF THE BULGE RED CLUMP STARS : EVIDENCE FOR THE GALACTIC BAR

The color-magnitude diagrams of

BVRI Observations of the Optical Afterglow of GRB 990510

\sim 5\times 10^5

The First DIRECT Distance Determination to a Detached Eclipsing Binary in M33

stars obtained for 13 fields towards the Galactic bulge with the OGLE project reveal a well-defined population of bulge red clump stars. We find that the distributions of the extinction-adjusted apparent magnitudes of the red clump stars in fields lying at

Are the ogle microlenses in the galactic bar

l=\pm5\deg

DIRECT Distances to Nearby Galaxies Using Detached Eclipsing Binaries and Cepheids. I. Variables in the Field M31B

in galactic longitude differ by

The optical gravitational lensing experiment: Deep photometry of the sagittarius DWARF spheroidal galaxy

0.37\pm0.025\;mag

RR Lyrae Variables in the Globular Cluster M55. The First Evidence for Nonradial Pulsations in RR Lyrae Stars

. Assuming that the intrinsic luminosity distribution of the red clump stars is the same on both sides of the Galactic center, this implies that the distances to the red clump stars in the two fields differ by a factor of

THE CLUSTER AGES EXPERIMENT (CASE). IV. ANALYSIS OF THE ECLIPSING BINARY V69 IN THE GLOBULAR CLUSTER 47 Tuc

1.185\pm0.015

DIRECT Distances to Nearby Galaxies Using Detached Eclipsing Binaries and Cepheids. II. Variables in the Field M31A

. A plausible explanation of the observed difference in the luminosity distribution is that the Galactic bulge is a triaxial structure, or bar, which is inclined to the line of sight by no more than

Cluster AgeS Experiment. Catalog of variable stars in the globular cluster omega Centauri

45\deg