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We investigate clustering properties of Lyman-break galaxies (LBGs) at z~3based on deep multi-waveband imaging data from optical to near-infraredwavelengths in the Subaru/XMM-Newton Deep Field. The LBGs are selected by U-Vand V-z' colors in one contiguous area of 561 arcmin^2 down to z'=25.5. Westudy the dependence of the clustering strength on rest-frame UV and opticalmagnitudes, which can be indicators of star formation rate and stellar mass,respectively. The correlation length is found to be a strong function of bothUV and optical magnitudes with brighter galaxies being more clustered thanfaint ones in both cases. Furthermore, the correlation length is dependent on acombination of UV and optical magnitudes in the sense that galaxies bright inoptical magnitude have large correlation lengths irrespective of UV magnitude,while galaxies faint in optical magnitude have correlation lengths decreasingwith decreasing UV brightness. These results suggest that galaxies with largestellar masses always belong to massive halos in which they can have variousstar formation rates, while galaxies with small stellar masses reside in lessmassive halos only if they have low star formation rates. There appears to bean upper limit to the stellar mass and the star formation rate which isdetermined by the mass of hosting dark halos.

The Subaru/XMM-Newton Deep Survey (SXDS) -VII. Clustering Segregation with Ultraviolet and Optical Luminosities of Lyman-Break Galaxies at z~3