The clustering of Lyman-break galaxies and Dark Matter Halos at z~ 3.

Details The clustering of Lyman-break galaxies and Dark Matter Halos at z~ 3. The clustering of Lyman-break galaxies and Dark Matter Halos at z~ 3.

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop..352g&link_type=abstract

NOAO Proposal ID #2000A-0352

Physics

Scientific paper

We request observing time with the 4-m telescope plus the Mosaic Imager, and with the MMT plus the MiniCam for U_nG R imaging to study the clustering properties of Lyman-break galaxies (LBGs) at z 3 and their dependence with the luminosity. Previous work has provided indications that these galaxies are strongly clustered in space, implying that they are biased tracers of the mass, and also that their clustering strength is a function of the UV luminosity. If our preliminary findings are confirmed with larger samples, this will be direct evidence of a physical link between the properties of the dark matter distribution (the clustering scaling laws) and the process of galaxy formation (the star formation rate). The implications will be that the first galaxies form in massive dark matter halos with an efficiency that is primarily regulated by the halos' mass. This will provide the first empirical test of one of the fundamental paradigms of cosmology, and a deep insight into the mechanisms of galaxy formation. One Mosaic pointings will cover an effective co-moving volume at z 3 larger than our entire current U-band dropout survey (encompassing more than 4 years of imaging effort), and comparable to the volumes of local surveys ( 2× 10^6h^-3 Mpc^3 for Ω=0.2). One MiniCam pointing will double the current HDF sample (North plus South) of faint Lyman-break galaxies at R 27. For the first time, it will be possible to accurately measure the correlation function and luminosity function of the LBG population at bar z=3 without the dangers of sample variance that have plagued previous attempts.

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