Abstract
The morphology of galaxies at high redshift ranges from elliptical and spiral to clumpy, including chains, clump clusters, doubles and tadpoles. Clumpy galaxies observed in the Hubble Ultra Deep Field at redshifts z = 1–5 contain star-forming complexes that are hundreds of times more massive than those forming in local galaxies, reflecting the more turbulent and gas-rich conditions in the early Universe. Numerical simulations suggest that the clumpy phase lasts for about a Gyr, fueled by cold flow accretion; feedback from supernovae does not quench star formation. Bulges and disks build up through coalescence or dispersal of large clumps. Grand design spiral structure first appears in the Universe at about z = 2. Local analogs of high redshift tadpole and clumpy galaxies have high star formation rates but metallicities that are lower in star-forming regions, consistent with ongoing external gas accretion.
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Acknowledgments
It is a pleasure to thank and congratulate my closest collaborator, Bruce Elmegreen, as we celebrate his illustrious career. Most of the work described here was done with him. I also congratulate my dear friend David Block for his stellar achievements as he joins the ranks of sexagenarians, and thank him and Ken Freeman for orchestrating another incomparable conference.
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Elmegreen, D. (2015). Galaxy Morphology at High Redshift. In: Freeman, K., Elmegreen, B., Block, D., Woolway, M. (eds) Lessons from the Local Group. Springer, Cham. https://doi.org/10.1007/978-3-319-10614-4_37
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DOI: https://doi.org/10.1007/978-3-319-10614-4_37
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