Massive Clumps in Local Galaxies: Comparisons with High-Redshift Clumps
  Local UV-bright galaxies in the Kiso survey include clumpy systems with
kpc-size star complexes that resemble clumpy young galaxies in surveys at high
redshift. We compare clump masses and underlying disks in several dozen
galaxies from each of these surveys to the star complexes and disks of normal
spirals. Photometry and spectroscopy for the Kiso and spiral sample come from
the Sloan Digital Sky Survey. We find that the largest Kiso clumpy galaxies
resemble UDF clumpies in terms of the star formation rates, clump masses, and
clump surface densities. Clump masses and surface densities in normal spirals
are smaller. If the clump masses are proportional to the turbulent Jeans mass
in the interstellar medium, then for the most luminous galaxies in the sequence
of normal:Kiso:UDF, the turbulent speeds and surface densities increase in the
proportions 1.0:4.7:5.0 and 1.0:4.0:5.1, respectively, for fixed restframe
B-band absolute magnitude. For the least luminous galaxies in the overlapping
magnitude range, the turbulent speed and surface density trends are 1.0:2.7:7.4
and 1.0:1.4:3.0, respectively. We also find that while all three types have
radially decreasing disk intensities when measured with ellipse-fit azimuthal
averages, the average profiles are more irregular for UDF clumpies (which are
viewed in their restframe UV) than for Kiso galaxies (viewed at g-band), and
major axis intensity scans are even more irregular for the UDF than Kiso
galaxies. Local clumpy galaxies in the Kiso survey appear to be intermediate
between UDF clumpies and normal spirals.
