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GEMS and GOODS fields were examined to z~1.4 for galaxy interactions andmergers. The basic morphologies are familiar: antennae with long tidal tails,tidal dwarfs, and merged cores; M51-type galaxies with disk spirals and tidalarm companions; early-type galaxies with diffuse plumes; equal-massgrazing-collisions; and thick J-shaped tails beaded with star formation anddouble cores. One type is not common locally and is apparently a looseassemblage of smaller galaxies. Photometric measurements were made of the tailsand clumps, and physical sizes were determined assuming photometric redshifts.Antennae tails are a factor of ~3 smaller in GEMS and GOODS systems compared tolocal antennae; their disks are a factor of ~2 smaller than locally. Collisionsamong early type galaxies generally show no fine structure in their tails,indicating that stellar debris is usually not unstable. One exception has a5x10**9 Msun smooth red clump that could be a pure stellar condensation. Mosttidal dwarfs are blue and probably form by gravitational instabilities in thegas. One tidal dwarf looks like it existed previously and was incorporated intothe arm tip by tidal forces. The star-forming regions in tidal arms are 10 to1000 times more massive than star complexes in local galaxies, although theirseparations are about the same. If they all form by gravitationalinstabilities, then the gaseous velocity dispersions in interacting galaxieshave to be larger than in local galaxies by a factor of ~5 or more; the gascolumn densities have to be larger by the square of this factor.

Smooth and Starburst Tidal Tails in the GEMS and GOODS Fields