Galaxy Size Evolution at High Redshift and Surface Brightness Selection Effects: Constraints from the Hubble Ultra Deep Field

We use the exceptional depth of the Ultra Deep Field (UDF) and UDFParallel ACS fields to study the sizes of high redshift (z ∼ 2 − 6) galaxies and address long-standing questions about possible biases in the cosmic star formation rate due to surface brightness dimming. Contrasting B, V , and i-dropout samples culled from the deeper data with those obtained from the shallower GOODS fields, we demonstrate that the shallower data are essentially complete at bright magnitudes to z . 5.5 and that the principal effect of depth is to add objects at the magnitude limit. This indicates that high redshift galaxies are compact in size (∼ 0.1−0.3) and that large (& 0.4, & 3 kpc) low surface brightness galaxies are rare. A simple comparison of the half-light radii of the HDF-N + HDF-S U dropouts with B, V , and i-dropouts from the UDF shows that the sizes follow a (1 + z) scaling towards high redshift. A more rigorous measurement compares different scalings of our U -dropout sample with the mean profiles for a set of intermediate magnitude (26.0 < z850,AB < 27.5) i-dropouts from the UDF. The best-fit is found with a (1+z) +0.19 −0.25 size scaling (for fixed luminosity). This result is then verified by repeating this experiment with different size measures, low redshift samples, and magnitude ranges. Very similar scalings are found for all comparisons. A robust measurement of size evolution is thereby demonstrated for galaxies from z ∼ 6 to z ∼ 2.5 using data from the UDF. Subject headings: galaxies: evolution — galaxies: high-redshift