The properties of Lyman break galaxies at z ∼ 5

In a recent paper, Lehnert & Bremer have photometrically selected a sample of Lyman break galaxies at z > 4.8 from a single VLT/FORS2 pointing and spectroscopically confirmed half of them to be at 4.8 < z < 5.8 . To study the properties of such galaxies further, we have photometrically selected a similar sample ( V AB > 28, i AB < 26.3, i AB − z AB > 0) from the Hubble Space Telescope Advanced Camera for Surveys ( HST ACS) images of the Chandra Deep Field ‐South. This selection results in a sample of 44 sources from ∼150 arcmin 2 . We find that such galaxies are often barely resolved in the ACS images, having half‐light radii of 0.1–0.3 arcsec (<2 kpc). They show no difference in spatial clustering from sources selected by i AB < 26.3, i AB − z AB > 0 , which are generally galaxies of lower redshift. However, their distribution over the field is not uniform and their surface density varies considerably over areas comparable to a single 8‐m or HST pointing. A reliable determination of the surface and volume densities of such galaxies requires a sky area considerably larger than the current ACS imaging of this field. No individual Lyman break candidate was detected to a 3σ limit of 6 × 10 −17 erg s −1 cm −2 at 0.5–5 keV by Chandra (a limiting luminosity of below 2 × 10 43 erg s −1 at z ∼ 5.3 ). By summing over all positions, we find that the mean source must be undetected at a level at least a factor of 4 times fainter than this. This rules out anything other than a weak active galactic nucleus (AGN) contribution to the emission from these objects; we conclude that luminous AGNs made little contribution to the final stages of re‐ionization of the Universe.