We employ a recently expanded sample of 8,000 galaxies that have been morphologically classified within the Galaxy And Mass Assembly (GAMA) survey and quantify the separate galaxy bulge and disk properties of this low-redshift (z<0.06), volume-limited sample with a large-scale automated procedure for fitting 2D, multi-component galaxy structure models. We use this structural information to examine the partitioning of galaxy stellar mass into bulge and disk dominated systems in the local universe and derive mass-size relations of pure spheroid/disk systems and separable bulge/disk galaxy components. We further break down the local galaxy stellar mass distribution into separate mass functions simultaneously by galaxy morphology/structure and environment, where galaxy environment is quantified on multiple scales from membership in filaments through groups/clusters and down to local pairings. We then compare the characteristic mass distributions of galaxy classes across environments in order to investigate the effects of environmental conditions on the buildup of stellar mass in bulges and disks, including the balance between merger accumulation and in situ mass growth in different environment regimes.
|Publication status||Published - 2015|
Moffett, A. J., Driver, S. P., Lange, R., Kelvin, L., & Robotham, A. (2015). Galaxy Bulge and Disk Buildup in Environmental Context with GAMA: IAU General Assembly. https://ui.adsabs.harvard.edu/abs/2015IAUGA..2256414M