Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 473, Issue 4, Pages 5468-5475Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx2745
Keywords
galaxies: fundamental parameters; galaxies: spiral; galaxies: structure
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Here I report the scaling relationship between the baryonic mass and scale-length of stellar discs for similar to 1000 morphologically late-type galaxies. The baryonic mass-size relationship is a single power law R* proportional to M-b(0.38) across similar to 3 orders of magnitude in baryonic mass. The scatter in size at fixed baryonic mass is nearly constant and there are no outliers. The baryonic mass-size relationship provides a more fundamental description of the structure of the disc than the stellar mass-size relationship. The slope and the scatter of the stellar mass-size relationship can be understood in the context of the baryonic mass-size relationship. For gas-rich galaxies, the stars are no longer a good tracer for the baryons. High-baryonic-mass, gas-rich galaxies appear to be much larger at fixed stellar mass because most of the baryonic content is gas. The stellar mass-size relationship thus deviates from the power-law baryonic relationship, and the scatter increases at the low-stellar-mass end. These extremely gas-rich low-mass galaxies can be classified as ultra-diffuse galaxies based on the structure.
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