Secular Evolution at the End of the Hubble Sequence

Details Secular Evolution at the End of the Hubble Sequence Secular Evolution at the End of the Hubble Sequence

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50102m&link_type=abstract

Spitzer Proposal ID #50102

Computer Science

Scientific paper

The bulgeless disk galaxies at the end of the Hubble Sequence evolve at a glacial pace relative to their more violent, earlier-type cousins. The causes of their internal, or secular evolution are important because secular evolution represents the future fate of all galaxies in our accelerating Universe and is a key ingredient to understanding galaxy evolution in lower-density environments at present. The rate of secular evolution is largely determined by the stability of the cold ISM against collapse, star formation, and the buildup of a central bulge. Key diagnostics of the ISM's stability are the presence of compact molecular clouds and narrow dust lanes. Surprisingly, edge-on, bulgeless disk galaxies with circular velocities below 120 km/s do not appear to contain such dust lanes. We propose to obtain IRAC images of a well-selected sample of extremely late-type disk galaxies to measure the intensity and concentration of PAH emission to determine if they possess the molecular gas necessary to drive secular evolution and early evidence for pseudobulge growth. Our sample has been carefully constructed to include disk galaxies above and below the critical circular velocity of 120 km/s where the dust properties of edge-on disks change so remarkably. These data, when combined with our HST ACS images of the dust attenuation, VLA HI observations, and IRAM CO data, will provide a complete picture of the ISM in the bulgeless disk galaxies at the end of the Hubble Sequence.

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