The Morphological Mix of Field Galaxies to [ITAL]m[/ITAL][TINF][ITAL]I[/ITAL][/TINF] = 24.25 Magnitudes ([ITAL]b[/ITAL][TINF][ITAL]J[/ITAL][/TINF] ∼ 26 Magnitudes) from a Deep [ITAL]Hubble Space Telescope[/ITAL] WFPC2 Image

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Abstract
We determine the morphological mix of field galaxies down to mI 24.25 mag (mB ~ 26.0 mag) from a single ultradeep Hubble Space Telescope wide field planetary camera (WFPC2) image in both the V606 and the I814 filters. In total, we find 227 objects with mI ≤ 24.5 mag and classify these into three types: ellipticals (16%), early-type spirals (37%), and late-type spirals/irregulars (47%). The differential number counts for each type are compared with simple models in a standard flat cosmology. We find that both the elliptical and the early-type spiral number counts are well described by little-or-no-evolution models, but only when normalized at bJ = 18.0 mag. Given the uncertainties in the luminosity function (LF) normalization, both populations are consistent with a mild evolutionary scenario based on a normal/low rate of star formation. This constrains the end of the last major star formation epoch in the giant galaxy populations to z ≥ 0.8. Conversely, the density of the observed late-type/irregular population is found to be a factor of 10 in excess of the conventional no-evolution model. This large population might be explained by a modified local dwarf-rich LF and/or strong evolution acting on the local LF. For the dwarf-rich case, a steep faint-end Schechter slope (α -1.8) is required, plus a fivefold increase in the dwarf normalization. For a purely evolving model based on a flat Loveday et al. LF (α -1.0), a ubiquitous starburst of ΔI ~ 2.0 mag is needed at z 0.5 for the entire late-type population. We argue for a combination of these possibilities, and show that for a steep Marzke et al. LF (α -1.5) a starburst of ~1.3 mag is required at z 0.5 in the entire late-type population, or ~2.0 mag in ~20% of the population.
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