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High-Redshift Clumpy Disks and Bulges in Cosmological Simulations

This work by Daniel Ceverino et al. explores the formation and evolution of high-redshift clumpy disks and bulges through cosmological simulations. Focusing on gas dynamics in galaxies at z=2.3, the study investigates the interplay between cold and hot gas phases and their gravitational instability leading to clump formation. It discusses star formation rates, stellar density, and clump migration over time scales of 400 Myr. The results aim to elucidate how large clumpy structures evolve into bulges, contributing to our understanding of galaxy evolution in the early universe.

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High-Redshift Clumpy Disks and Bulges in Cosmological Simulations

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  1. High-Redshift Clumpy Disks & Bulges in Cosmological Simulations Daniel Ceverino (HU) Potsdam, 2009 AvishaiDekel (HU) , ReemSari(HU), Tobias Goerdt(HU), Anatoly Klypin (NMSU)

  2. From Disks to Bulges Rest-frame visible Rest-frame UV Genzel et al. 2008 Elmegreen et al. 2009

  3. Cold Streams & Hot halosat z=2.3 2Rvir=140 kpc Mvir=4 1011 M Rvir Streams Disk Cold Gas (T<105.5 K) Hot Gas (T>105.5 K)

  4. Gravitationally UnstableDisks Gas Surface Density Clumps !! log (M/pc2) 15 kpc

  5. More Clumpy Galaxies Gas Surface Density 10 kpc Face-on view Edge-on view

  6. Star Formation Maps in log(M/yr/kpc2) 10 kpc Face-on view Edge-on view

  7. A Massive Bulge Stellar Surface Density 10 kpc Face-on view Edge-on view

  8. More Clumpy Disks Gas Surface Density 10 kpc

  9. SINSand Simulations SFR vs Stellar Mass Stellar Mass vs Max. Velocity Data (Red circles) from Forster Schreiber et al. 2009 Data (Red circles) from Cresci et al. 2009

  10. Clumps Evolution (400 Myr)

  11. Clump Formation 8 kpc

  12. Clump Migration 8 kpc

  13. Steady-State Regime z=1.9 z=1.6 z=1.3

  14. Summary

  15. The End

  16. Artificial Fragmentation

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