Computer Science
Scientific paper
Jul 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009hst..prop12196r&link_type=abstract
HST Proposal ID #12196. Cycle 18
Computer Science
Scientific paper
Traditionally, the radial surface-brightness profile of a galaxy disk has been modelled by a single exponential profile. However, the vast majority of disk galaxies actually show signs of a disk truncation, where the profile suddenly breaks to a steeper second exponential profile. The cause of this break remains poorly understood.In Lambda-CDM cosmology, the radii at which disk truncations are found are also the most recently formed. Disk truncations may therefore be a direct result of the disk-galaxy assembly process. Many theories have thus been proposed to connect the truncations to theories of disk galaxy formation. Generally, break formation models either form the stars in the observed distribution {e.g., a star formation threshold} or employ dynamical effects to redistribute them into the current configuration {e.g., tidal stripping}. These models need to be constrained observationally to probe the underlying mechanism of outer-disk formation responsible for creating the truncations.Using our previous experience with deep CMDs from HST observations of resolved extragalactic stellar populations, we propose a comprehensive survey of disk truncations across a variety of disk morphologies and sizes. With resolved stellar populations we are able to map the truncations as a function of age to a very low equivalent surface brightness. Additionally, we will carry out simulations of different truncation formation scenarios for each galaxy {based on disk type and mass} to compare directly with the observations. Combining the two will prove crucial to understanding the mechanism for creating disk truncations and the ongoing processes in disk formation. HST is the only observatory capable of discriminating the formation models due the unique resolution and depth of the ACS and WFC3 instruments.;
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