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Structure and dynamics of disks in galaxies
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Structure and dynamics of disks in galaxies
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One the most cited papers in astronomy is Ken Freeman's 1970 paper on exponential disks in galaxies. In this contribution I review what has been done in this area since then and what we can infer about systematic properties of disks in galaxies from surface photometry, HI synthesis observations and measurements of stellar kinematics. Most disks have radial truncations at $3.6 \pm 0.6$ radial scalelengths $h\subr{R}$. Galaxy disk thicknesses $h\subr{R}/h\subr{z}= 7.3 \pm 2.2$ imply that these disk cannot be ``maximum disks''. I briefly discuss a recent study of the ``superthin'' edge-on galaxy IC 5249.
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Cited by 1 Pith paper
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Kinematic scaling of thin and thick discs from SAMI to NewHorizon
Thin and thick disc components follow parallel mass–velocity dispersion relations, with thick discs about 1.6 times hotter than thin discs under circularity-based definitions.
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