Dependence of Clustering Strength on Stellar Mass and SFR for LBGs at z˜ 3

Details Dependence of Clustering Strength on Stellar Mass and SFR for LBGs at z˜ 3 Dependence of Clustering Strength on Stellar Mass and SFR for LBGs at z˜ 3

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..399..276y&link_type=abstract

Panoramic Views of Galaxy Formation and Evolution ASP Conference Series, Vol. 399, proceedings of the conference held 11-16 Dece

Astronomy and Astrophysics

Astronomy

Scientific paper

We study the dependence of the clustering strength on stellar mass and star-formation rate for Lyman-break galaxies (LBGs), using a sample of 708 LBG candidates at z˜ 3. This sample is constructed from deep multi-waveband imaging data from optical to near-infrared wavelengths in the Subaru/XMM-Newton Deep Field. We find that the correlation length strongly depends on a combination of rest-frame UV brightness (an indicator of star-formation rate) and rest-frame optical brightness (an indicator of stellar mass) in the sense that galaxies bright in optical brightness have large correlation lengths irrespectively of ultraviolet (UV) brightness, while galaxies faint in optical brightness have correlation lengths decreasing with decreasing UV brightness. These results indicate 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 lower star-formation rates. There appears to be an upper limit to stellar mass and star-formation rate which is determined by the mass of hosting halos.

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