斯巴鲁/XMM-牛顿深度调查（SXDS）- VII。Lyman-Break半导体在z~3处的紫外和光学亮度与聚簇分离
The Subaru/XMM-Newton Deep Survey (SXDS) -VII. Clustering Segregation with Ultraviolet and Optical Luminosities of Lyman-Break Galaxies at z~3
摘要：
利用Subaru/XMM-Newton Deep Field的光学到近红外波段的深空多波段成像数据，研究了z~3处的Lyman-break星系（LBG）的成团特性.在561弧分^2至z '= 25.5的一个连续区域内，通过U-V和V-z'颜色选择LBG。我们研究的集群强度的依赖关系的静止帧UV和光学星等，这可以是恒星形成率和恒星质量的指标，分别。的相关长度被发现是一个强大的功能，紫外线和光学星等与更明亮的星系被聚集在这两种情况下比微弱的。此外，相关长度是依赖于UV和光学星等的组合，在这个意义上，星系明亮的光学星等有大的相关长度，而不考虑UV星等，而星系暗淡的光学星等的相关长度随着UV亮度的降低而降低。这些结果表明，大恒星质量的星系总是属于大质量的晕，他们可以有不同的恒星形成率，而小恒星质量的星系居住在较小的质量晕，只有当他们有低的恒星形成率。恒星质量和恒星形成速率似乎有一个上限，这取决于暗晕的质量。
英文摘要：
We investigate clustering properties of Lyman-break galaxies (LBGs) at z~3 based on deep multi-waveband imaging data from optical to near-infrared wavelengths in the Subaru/XMM-Newton Deep Field. The LBGs are selected by U-V and V-z' colors in one contiguous area of 561 arcmin^2 down to z'=25.5. We study the dependence of the clustering strength on rest-frame UV and optical magnitudes, which can be indicators of star formation rate and stellar mass, respectively. The correlation length is found to be a strong function of both UV and optical magnitudes with brighter galaxies being more clustered than faint ones in both cases. Furthermore, the correlation length is dependent on a combination of UV and optical magnitudes in the sense that galaxies bright in optical magnitude have large correlation lengths irrespective of UV magnitude, while galaxies faint in optical magnitude have correlation lengths decreasing with decreasing UV brightness. These results suggest that galaxies with large stellar masses always belong to massive halos in which they can have various star formation rates, while galaxies with small stellar masses reside in less massive halos only if they have low star formation rates. There appears to be an upper limit to the stellar mass and the star formation rate which is determined by the mass of hosting dark halos.
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