Clustering of Galaxies in the Hubble Deep Field

Details Clustering of Galaxies in the Hubble Deep Field Clustering of Galaxies in the Hubble Deep Field

1996-06-13

arxiv.org/abs/astro-ph/9606084v2

Astronomy and Astrophysics

Astrophysics

9 pages, Latex, [aas2pp4], 5 Postscript figures. Figures obtainable via anonymous FTP from ftp://ecf.hq.eso.org/pub/preprints/

Scientific paper

10.1086/304072

We compute the two-point angular correlation function $w(\theta)$ for a sample of $\sim$ 1700 galaxies to a magnitude-limit equivalent to $R \sim 29.5$ using a catalog derived from the Hubble Deep Field images. A non zero value of $w(\theta)$ is measured down to $R=29.0$. The amplitude of $w(\theta)$ at the bright magnitude limit ($R \sim 26$) is consistent with previous ground-based observations. At fainter magnitudes the clustering amplitude continues to decrease but at a slower rate than that predicted by the power law $w(1'')\propto 10^{-0.27R}$ observed for shallower samples. The observed $w(\theta)$ over the magnitude range $20

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