![]() ![]() ![]() The presence of such large numbers of SEEs could be explained by a steep ( 1.4 to 1.8) local luminosity function or a starburst stage around z 0.5 caused by minor mergers. Combined with irregular/peculiar galaxies, they could be responsible for up to 80 of the galaxy excess over model predictions. These ``Small Exponential Elliptical (SEE)'' galaxies make up 21 25 of the population mix at 20 < I < 21. The excess galaxies are similar to local dwarf galaxies: same axial ratio distribution and colors ((B V) 0.4, (U B) 0.2). It appears that the axial ratio distribution of small (half-light radius < 0), faint (I 20.5) galaxies with exponential surface brightness profile has a marked excess at ratios around 0.7 (round = 1.0) over local samples of spiral galaxies. Although samples are still fairly small, very interesting results have been obtained, and HST imaging offers the exciting possibility of determining the morphology of the galaxies responsible for the faint galaxy excess.Īxial ratio is the simplest morphological parameter to measure. With this incredible spatial resolution, it is now possible to classify high-redshift galaxies according to the Hubble sequence, and, to quantify galaxy morphology with parameters such as central surface brightness, axial ratio, bulge-to-disk ratio, disk scale length and light profile models (point source, r, exponential). The Hubble Space Telescope (HST) has a point-spread-function FWHM of 0. ![]() Next: Models Up: The Faint Galaxy Previous: The Autofib Survey ![]()
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