High Redshift Galaxies in the Hubble Deep Field: II. Colours and Number Counts

Details High Redshift Galaxies in the Hubble Deep Field: II. Colours and Number Counts High Redshift Galaxies in the Hubble Deep Field: II. Colours and Number Counts

1998-03-12

arxiv.org/abs/astro-ph/9803144v2

Astronomy and Astrophysics

Astrophysics

TeX, 13 pages, 10 figures, submitted to the MNRAS Note: replaced with (hopefully) correctly formatted version

Scientific paper

10.1046/j.1365-8711.1998.01724.x

We discuss the deep galaxy counts from the Hubble Deep Field (HDF) imaging survey. At faint magnitudes, the slope of the differential number-magnitude relation is flatter than 0.2 in all four HDF bandpasses. In the ultraviolet, a fluctuation analysis shows that the flattening observed below U=26 mag is not due to incompleteness and is more pronounced than in the other bands, consistent with the idea that a redshift limit has been reached in the galaxy distribution. A reddening trend of about 0.5 magnitude is observed at faint fluxes in the colour-magnitude diagram, (U-V)_{eff} vs. V. We interpret these results as the effect of intergalactic attenuation on distant galaxies. At flux levels of AB=27 mag and in agreement with the fluctuation analysis and the colour-magnitude relation, about 7% of the sources in U, 30% in B and 35% in V are Lyman-break ``dropouts'', i.e. candidate star-forming galaxies at z>2. By integrating the number counts to the limits of the HDF survey we find that the mean surface brightness of the extragalactic sky is dominated by galaxies that are relatively bright and are known to have =0.6. To AB=29 mag, the integrated light from resolved galaxies in the I-band is 2.1\pm 0.4 \times 10^{-20} erg/cm^2/s/Hz/sr, and its spectrum is well described by a broken power-law. We discuss the predictions for the counts, colours, and luminosity densities from standard low-q_0 pure-luminosity-evolution models without dust obscuration, and find that they are unable to reproduce all the observed properties of faint field galaxies.

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