The Angular Clustering of Lyman-Break Galaxies at Redshift z=3

Details The Angular Clustering of Lyman-Break Galaxies at Redshift z=3 The Angular Clustering of Lyman-Break Galaxies at Redshift z=3

1998-02-25

arxiv.org/abs/astro-ph/9802318v1

Astrophys.J. 503 (1998) 543

Astronomy and Astrophysics

Astrophysics

24 pages, 4 postscript figures, LaTex, uses aaspp4.sty, to be published in The Astrophysical Journal

Scientific paper

10.1086/306027

We have measured the angular correlation function w(theta) for a sample of 871 Lyman-break galaxies (LBGs) at z=3. Fitting a power-law to a weighted average of w(theta) from 5 fields, we find the amplitude to be A_w=2 arcsec^{\beta} and the slope \beta=0.9. The slope is the same as in the local and moderate redshift universe. A slope \beta=0.25 or shallower is ruled out by the data at the 99.9% confidence level. Because N(z) of LBGs is well determined from 376 spectroscopic redshifts, the real-space correlation function can be derived from the angular one through the Limber transform. This inversion is rather insensitive to the still relatively large errors on A_w and \beta, and the spatial correlation length is much more tightly constrained than either of these parameters. We estimate r_0=3.3 -0.6 +0.7 (2.1 -0.5 +0.4) h^{-1} Mpc (comoving) for q_0=0.1 (0.5) at z=3.04 (h is in units of 100 km/s/Mpc). The correlation length of LBGs at z=3 is comparable to that of present-day spiral galaxies and is only about 50% smaller than that of the ellipticals; it is as large or larger than any measured in galaxy samples at 0.3

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