Formation of Galaxies

The formation of galaxies has to be seen in the context of the limitations now set by the anisotropy measurements of the microwave background, discussed above. It appears that gravitational instability coupled with strong dissipation first leads to spheroidal systems, possibly driven by interaction with neighboring systems, and then to disk formation much later.

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These disks slowly accrete gas towards the center, and thus can produce exponential disks, central starbursts, and also, central feeding of an AGN.

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The gravitational potential of the dark matter has a core radius of similar scale as the turnover radius of the present rotation curve, and the dark matter appears to be "pulled" in by the deeper gravitational well of the dissipative matter.

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Elliptical Galaxies, in addition, can have global accretion both from a cooling flow in gas (see above), and from merging with smaller satellite galaxies, leading in extreme cases to the central cD galaxies in clusters, and also to the activity associated with a well-fed AGN at the center.

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