Kathryn Johnston
Kathryn Johnston Kathryn Johnston
Given: Motivation – hierarchical structure formation; – properties of Local Group dwarfs What can we say about: – stellar halos – satellite systems – substructure in stellar halos (NGC5907, Shang et al 1999) (inspired by Majewski, Spaghetti, SDSS, Ibata et al, Guhathakurta....) Modeling (and observational) problem: low luminosity and surface brightness of objects and features we’re interested in. (related studies: Brook et al; Knebe et al; Rende et al; Abadi, Navarro, Steinmetz; Diemand, Madau, Moore....)
Dark matter modeled via merger tree. 100,000-particle N-body model run for each luminous satellite accreted. Masses, orbits accretion times dictated by cosmology Methods - Our Approach time Light matter painted on subsequently to match properties of Local Group dwarfs today....
- Page 1: Stellar Halos and Satellite Systems
- Page 5 and 6: Model for Formation of a Halo Color
- Page 7 and 8: Features brighter than 30 mag/ arcs
- Page 9 and 10: Model for Formation of a Halo - Hal
- Page 11 and 12: Abundance Patterns in Satellites vs
- Page 13 and 14: Abundance Patterns in Satellites vs
- Page 15 and 16: Abundance Patterns in Satellites vs
- Page 17 and 18: ... only stars with [alpha/ Fe]
Given:<br />
Motivation<br />
– hierarchical structure formation;<br />
– properties of Local Group dwarfs<br />
What can we say about:<br />
– stellar halos<br />
– satellite systems<br />
– substructure in stellar halos<br />
(NGC5907, Shang et al 1999)<br />
(inspired by Majewski, Spaghetti, SDSS, Ibata et al, Guhathakurta....)<br />
Modeling (and observational) problem: low<br />
luminosity and surface brightness of objects<br />
and features we’re interested in.<br />
(related studies: Brook et al; Knebe et al; Rende et al; Abadi, Navarro,<br />
Steinmetz; Diemand, Madau, Moore....)
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