Hot Dust in Galaxies at 0.25 < z < 0.29



Journal Title

Journal ISSN

Volume Title



Thermal dust emission within galaxies is driven by heating from young, hot stars. Because of this, one way to examine star formation in a galaxy is through the distribution of starlight and hot dust light. Independent component analysis (ICA) is a method of separating each source in a mixed signal by maximizing each signal’s negentropy. Negentropy is the opposite of entropy, which is a measure of the disorder in a system, so the sources are separated by maximizing their order. ICA can be used to separate starlight and hot dust light within galaxies, and has been used previously to calculate total stellar masses and study star for- mation in galaxies at z 0. This thesis applies this method to characterize the distribution of starlight and dust light in galaxies at 0.25 ≤ z ≤ 0.29 and calculate their total stellar masses. The results in this thesis show that star formation in the target galaxies is primarily on the outermost edges of the galaxies, potentially indicating an inside-out star formation history. Additionally, the results presented here show that star formation decreases with increasing total stellar mass. Galaxies in this range of redshifts emitted the light observed about 3 billion years ago, so these results provide insight into how galaxies have changed since this era.



astronomy, astrophysics, galaxies, dust