Mathematics – Logic
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50393k&link_type=abstract
Spitzer Proposal ID #50393
Mathematics
Logic
Scientific paper
The physical processes responsible for driving the transformation of star-forming field galaxies to passively evolving cluster members are still poorly understood. Several mechanisms have been proposed, some of which would directly suppress star formation activity, while others would instead trigger a burst of star formation that subsequently consumes most of a galaxy's gas supply. We can directly test for this latter class of mechanisms by searching for a starburst population of galaxies in and around clusters. Furthermore since many of the proposed processes are most effective at different galaxy and gas densities, the location and properties of the local environments in which these galaxies are found will help constrain the mechanism which trigger their activity. We propose 3.6-8 micron IRAC and 24 micron MIPS observations of the massive, relaxed cluster MACS J1423.8+2404 at z=0.54 in order to carry out a comparative study with our pending observations of the morphologically disturbed cluster MACS J0717.5+3745 at z=0.55. While the two systems have nearly identical global properties, there is ongoing galaxy accretion into MACS J0717.5+3745 through a large-scale filament connected to the system, whereas no such activity or signs of significant substructure are detected in MACS J1423.8+2404. We intend to use the observations to map the distribution of any galaxies undergoing a starburst phase from the cluster core out to the field population. The distinct environments offered by the two clusters, one with actively infalling galaxies and the other with a more virialized population, will allow us to better isolate the effects that these conditions have on triggering starburst activity. Furthermore, similarities in the global properties of the two clusters, such as system redshift and mass, will enable us to disentangle the role of large-scale versus local environment in driving galaxy evolution in these systems.
Ebeling Harald
Kocevski Dale D.
Ma Cheng-Jiun
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