TL;DR
This paper presents a semi-analytic model that traces the formation and evolution of galaxy disks within a cosmological framework, accurately reproducing observed size distributions and exploring clustering dependence on galaxy size.
Contribution
It introduces a novel approach modeling gas and stellar disk growth separately, with detailed angular momentum tracking, improving upon previous models.
Findings
Successfully reproduces local stellar mass--radius distribution
Matches observed gas-to-stellar disk size ratios
Shows qualitative agreement with observed clustering dependence
Abstract
We introduce a model which uses semi-analytic techniques to trace formation and evolution of galaxy disks in their cosmological context. For the first time we model the growth of gas and stellar disks separately. In contrast to previous work we follow in detail the angular momentum accumulation history through the gas cooling, merging and star formation processes. Our model successfully reproduces the stellar mass--radius distribution and gas-to-stellar disk size ratio distribution observed locally. We also investigate the dependence of clustering on galaxy size and find qualitative agreement with observation. There is still some discrepancy at small scale for less massive galaxies, indicating that our treatment of satellite galaxies needs to be improved.
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