The Formation of Large Galaxy Disks in Low z Major Mergers

Details The Formation of Large Galaxy Disks in Low z Major Mergers The Formation of Large Galaxy Disks in Low z Major Mergers

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21430805b&link_type=abstract

American Astronomical Society, AAS Meeting #214, #308.05; Bulletin of the American Astronomical Society, Vol. 41, p.737

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Using high resolution SPH simulations in a fully cosmological LambdaCDM context we study the formation of a bright disk dominated galaxy that originates from a "wet" major merger at z=0.8. A substantial thin stellar disk grows rapidly following the last major merger and the present day properties of the final remnant are typical of early type spiral galaxies. The key ingredients for the formation of a dominant stellar disk component after a major merger are: i) substantial and rapid accretion of gas through cold flows followed at late times by cooling of gas from the hot phase, ii) supernova feedback that is able to partially suppress star formation during mergers, and iii) relative fading of the spheroidal component. The gas fraction of the progenitor disks does not exceed 25% at z < 3, emphasizing that the continuous supply of gas from the local environment plays a major role in the regrowth of disks and in keeping the galaxies blue. The results of this simulation alleviate the problem posed for the existence of disk galaxies by the high likelihood of interactions and mergers for galaxy sized halos at relatively low z.

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