Observations of Thick Disks in the Hubble Space Telescope Ultra Deep   Field
  The vertical profiles of chain and spiral galaxies in the Hubble Space Telescope Ultra Deep Field (UDF) are fit to sech^2(z/z_0) functions convolved with stellar profiles in order to measure the disk scale heights z_0 in four passbands. The bulge regions of the spirals are avoided. Photometric redshifts give absolute scales. The rms heights of the giant clumps in these galaxies are also measured. The results indicate that UDF disks are thick with an average z_0 of 1.0\pm0.4 kpc. The ratio of radial exponential scale length to z_0 is \~3\pm1.5. The scale heights are only 20% larger than the radii of the giant star-forming clumps and a factor of ~10 larger than the rms clump deviations around the midplanes. This suggests the clumps formed from midplane gas and dissolved to make the thick disks. Redshifted stellar population models suggest ages of ~1 Gy and mass column densities from 4 to 40 Msun pc^{-2}. The UDF disks look like young versions of modern thick disks. This resemblance is difficult to understand if galaxies grow over time or if subsequent accretion of thin disks gravitationally shrinks the observed thick disks. More likely, high redshift disks are thick because their mass column densities are low; a velocity dispersion of only 14 km/s reproduces the observed thickness. Modern thick disks require more heating at high redshift. This is possible if the gas that eventually makes the thin disk is in place before the youngest age of a modern thick disk, and if the existing stars are heated during the delivery of this gas. 
Bruce G. Elmegreen (1), Debra Meloy Elmegreen (2) ((1) IBM T.J. Watson   Research Center, (2) Vassar College)