Caltech faint galaxy redshift survey. XIV. galaxy morphology in the rubble deep field (north) and its flanking fields to z=1.21

Morphological classifications are reported for Hubble Space Telescope images of 241 galaxies in the Hubble Deep Field and its flanking fields with measured redshifts in the interval 0.25 < z < 1.2, drawn from a magnitude-limited redshift survey to R = 24.0. The galaxies are divided into three groups with redshifts in the intervals 0.25-0.6, 0.6-0.8, and 0.8-1.2. R-606 images from the first group and I-814 images from the second and third groups are compared with B-band images of nearby galaxies. All classifications were therefore made at approximately the same rest wavelength. Selection biases are discussed. We corroborate and extend the results of earlier investigations by observing that 1. Most intermediate- and late-type galaxies with z greater than or similar to 0.5 have morphologies that are dramatically different from those of local galaxies and cannot be shoehorned into the Hubble "tuning fork" classification scheme; 2. Grand-design spirals appear to be rare or absent for z greater than or similar to 0.3; 3. Many Sa and Sb spirals with z greater than or similar to 0.6 do not exhibit well-defined spiral arms, and the arms of distant Sc galaxies appear more chaotic than those of their nearby counterparts; 4. The fraction of all galaxies that are of types Sc and Scd drops from 23% at z similar to 0 to 5% for z > 0.6. 5. Barred spirals are extremely rare for z greater than or similar to 0.5; 6. Roughly one in five galaxies with z greater than or similar to 0.8 is a compact objects that resembles local E, SO, or Sa galaxies. 7. Peculiar galaxies are more common beyond z = 0.3, especially among late-type spirals, than they are at z similar to 0; 8. Merging galaxies, particularly those with three or more components, also become more common with increasing redshift. On the basis of these and similar observations, it is inferred that the development of pronounced spiral structure was delayed until similar to5 Gyr and that most bulges are probably not formed by disintegrating bars. Major morphological changes were still taking place only similar to5 Gyr ago, even though changes in the integrated light of most galaxies were then much slower than they were similar to 10 Gyr ago.