13 January, 2006 - 1:50 PM
The Dense ISM in (high redshift) Starbursts
Michael Kaufman (San Jose State University/NASA Ames)
Over the past 20 years, PDR models have developed into
mature and useful tools for analyzing emission from dense and diffuse interstellar clouds illuminated by FUV radiation. The classic PDR tracers are the OI 63 micron and CII 158 micron fine-structure
lines, along with the far-infrared continuum. While these tracers are useful for constraining the physical conditions in nearby individual PDRs, care must be used in applying the models to more distant regions in which both dense star forming regions and diffuse gas lie in the beam.
Observations of H2 and CO in nearby galaxies independently
probe the dense gas component and provide a calibration for
observations where many components lie in the beam. The implications
for ALMA observations of starbursts, particularly of CII and OI in galaxies with low metallicity
at high redshift, will be discussed.