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Modeling Faint Galaxy Production via Star Cluster Evolution: Insights from Low-Mass Systems

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This study explores the production of faint galaxies through star cluster evolution, focusing on the dynamics of low-mass stellar systems in different tidal fields. Utilizing N-body simulations, we analyze systems, including the Milky Way (MW) and M31, with various configurations for binaries and other factors. The findings contribute to our understanding of galaxy formation and structure, particularly regarding ultra-faint dwarfs and their environments. This research was presented at the ESO conference in Santiago, Chile, in April 2011.

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Modeling Faint Galaxy Production via Star Cluster Evolution: Insights from Low-Mass Systems

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  1. Models of Faint Galaxy Production through Star Cluster Evolution Jarrod Hurley (Centre for Astrophysics & Supercomputing) “Dynamics of Low-Mass Stellar Systems” ESO, Santiago, Chile April 4-8 2011

  2. Sizes of low-mass stellar systems Huxor+11 Models of Faint Galaxy Production through Star Cluster Evolution

  3. Sizes of low-mass stellar systems MW M31 Huxor+11 Models of Faint Galaxy Production through Star Cluster Evolution

  4. Sizes of low-mass stellar systems MW M31 M31 dIrr Huxor+11 Models of Faint Galaxy Production through Star Cluster Evolution

  5. Sizes of low-mass stellar systems MW M31 M31 dIrr DM halo Huxor+11 Models of Faint Galaxy Production through Star Cluster Evolution

  6. simulations of low-mass stellar systems in different tidal fields MW M31 M31 dIrr DM halo Huxor+11 Models of Faint Galaxy Production through Star Cluster Evolution

  7. N-body simulation background Equation of Motion O(N3) special-purpose GRAPE hardware GPU [ NBODY4/NBODY6:Aarseth 1999; Aarseth 2003] techniques for few-body subsystems tidal field stellar evolution binary evolution [Hurley et al. 2001] [Mardling & Aarseth 2001; Mikkola 2006, etc.] Models of Faint Galaxy Production through Star Cluster Evolution

  8. Models of Extended Clusters? N = 100,000, 5% binaries, Z = 0.001, KTG IMF, Plummer/King Models of Faint Galaxy Production through Star Cluster Evolution

  9. Models of Extended Clusters? N = 100,000, 5% binaries, Z = 0.001, KTG IMF, Plummer/King RGC = 10 kpc MG = 9x109MsunM = 9x1010Msun point-mass point-mass or 3-component e.g. NGC6822 e.g. M31 Models of Faint Galaxy Production through Star Cluster Evolution

  10. Models of Extended Clusters? N = 100,000, 5% binaries, Z = 0.001, KTG IMF, Plummer/King e.g. NGC6822 e.g. M31 Models of Faint Galaxy Production through Star Cluster Evolution

  11. Models of Extended Clusters? N = 100,000, 5% binaries, Z = 0.001, KTG IMF, Plummer/King Hurley+Mackey10 Models of Faint Galaxy Production through Star Cluster Evolution

  12. Models of Extended Clusters? Da Costa+09 Models of Faint Galaxy Production through Star Cluster Evolution

  13. Models of Extended Clusters? Da Costa+09 Models of Faint Galaxy Production through Star Cluster Evolution

  14. The N = 200,000 model 200k 2% binaries Rgc = 4 kpc 100k 5% binaries Rgc = 8.5 kpc Models of Faint Galaxy Production through Star Cluster Evolution

  15. Models of Ultra-Faint Dwarfs? 31 127 132 308 170 size/pc 25 64 152 321 554 Strigari+08 sigma ~ 3-10 km/s Models of Faint Galaxy Production through Star Cluster Evolution

  16. Models of Ultra-Faint Dwarfs? MNFW = 109 c = 16 Rgc = 0.5 kpc Models of Faint Galaxy Production through Star Cluster Evolution

  17. Models of Ultra-Faint Dwarfs? MNFW = 109 c = 16 Rgc = 0.5 kpc Models of Faint Galaxy Production through Star Cluster Evolution

  18. Models of Ultra-Faint Dwarfs? MNFW = 109 c = 16 Rgc = 0.5 kpc Models of Faint Galaxy Production through Star Cluster Evolution

  19. Models of Ultra-Faint Dwarfs? MNFW = 109 c = 16 Rgc = 0.5 kpc Models of Faint Galaxy Production through Star Cluster Evolution

  20. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries Models of Faint Galaxy Production through Star Cluster Evolution

  21. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries Models of Faint Galaxy Production through Star Cluster Evolution

  22. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries Models of Faint Galaxy Production through Star Cluster Evolution

  23. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries Models of Faint Galaxy Production through Star Cluster Evolution

  24. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries Models of Faint Galaxy Production through Star Cluster Evolution

  25. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries Sand+10 Leo IV Models of Faint Galaxy Production through Star Cluster Evolution

  26. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries Models of Faint Galaxy Production through Star Cluster Evolution

  27. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries rpl = 27 pc rpl = 15 pc Models of Faint Galaxy Production through Star Cluster Evolution

  28. Models of Ultra-Faint Dwarfs? Star cluster near centre (Rgc=20pc), MNFW = 108, c=20 N = 100,000, 5% binaries N = 28,000, 40% binaries Martin+08 Models of Faint Galaxy Production through Star Cluster Evolution

  29. Models of Ultra-Faint Dwarfs? M300 ~ 0.7x107Msun sigma ~ 5 km/s Models of Faint Galaxy Production through Star Cluster Evolution

  30. Future … • complex tidal fields • definition of tidal radius? • explore initial N, fb, density, sigma … • non-virialprotoclusters, e.g. Hurley+Bekki08 • include gas? • … Models of Faint Galaxy Production through Star Cluster Evolution

  31. N-body simulation background

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