The Clustering of Faint Galaxies on Small Angular Scales

Details The Clustering of Faint Galaxies on Small Angular Scales The Clustering of Faint Galaxies on Small Angular Scales

1999-08-13

arxiv.org/abs/astro-ph/9908148v1

Astronomy and Astrophysics

Astrophysics

4 pages, 1 figure, uses paspconf.sty. To be published in the proceedings of "The Hy-redshift Universe", eds. A. Bunker & W. va

Scientific paper

We present a preliminary measurement of the angular clustering of faint ($R \le 25$) field galaxies in which we concentrate on the behavior of $w(\theta)$ on small angular scales ($\theta \ls 10''$). The galaxies are strongly clustered and $w(\theta)$ is well-characterized by a power law of the form $A_w \theta^{-\delta}$. The best-fitting value of the power law index, $\delta$, is, however, steeper than the fiducial value of $\delta = 0.8$, indicating there are more pairs of galaxies separated by $\theta \ls 10''$ in our sample than would be otherwise expected. Using the best-fitting form of $w(\theta)$, we estimate that $\sim 10%$ of the galaxies are in physically close pairs (separations $\ls 21 h^{-1}$ kpc). This is a factor of order 2 larger than local galaxy samples, but comparable to galaxy samples with $ \sim 0.4$. The mean redshift of our galaxies is of order 0.95, and, therefore, our result suggests that there was little or no evolution in the merger rate of galaxies between $z \sim 1$ and $z \sim 0.4$.

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