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Galaxy Dynamics in CLASH Clusters

Galaxy Dynamics in CLASH Clusters. Doron Lemze (Johns Hopkins). CLASH team + VLT team + Margaret Geller, Michael J. Kurtz, and Kenneth J. Rines. Clusters with reduced redshifts :. A963 - Hectospec (Margaret’s team) A2261 - Hectospec (Margaret’s team)

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Galaxy Dynamics in CLASH Clusters

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  1. Galaxy Dynamics in CLASH Clusters DoronLemze (Johns Hopkins) CLASH team + VLT team + Margaret Geller, Michael J. Kurtz, and Kenneth J. Rines

  2. Clusters with reduced redshifts: • A963 - Hectospec (Margaret’s team) • A2261 - Hectospec (Margaret’s team) • RXJ2129 - Hectospec (Margaret’s team) • MACS1206 – VLT & Magellan (Piero & DanK)

  3. Cluster members – removing interlopers Why? • Effects estimated quantities such as virial mass and • concentration parameter. • Effects substructure measurements. • Effects estimating the level of relaxation.

  4. Cluster members – A963 # cluster members: 205 den Hartog & Katkert 1996

  5. Cluster members – RXJ2129 # cluster members: 195

  6. Cluster members – A2261 # cluster members: 213

  7. Cluster members – MACSJ1206 # cluster members: 311

  8. Substructure Dressler & Shectman 1988 – a 3D method

  9. Substructure – A963

  10. Substructure – RXJ2129

  11. Substructure – A2261

  12. Substructure – MACSJ1206

  13. A2261 & MACSJ1206: substantial substructure Substructure – summary A963 & RXJ2129: some substructure level, but maybe not very significant? Is it consistent with X-ray info? Yes! Out of the 20 relaxed CLASH clusters 8 have some evidence for substructure, among them A2261 & MACSJ1206 (Postman et al. 2011).

  14. Mass profiles

  15. Mass profiles – A963

  16. Mass profiles – RXJ2129

  17. Mass profiles – MACSJ1206

  18. Mass profiles – A2261

  19. M – C relation Coe et al.

  20. If at least some of the clusters are not fully relaxed, maybe comparing the unrelaxed clusters inferred concentrations to concentrations measured from simulated relaxed clusters is not comparing apples to apples. However, since unrelaxed clusters should have slightly lower concentrations (Neto et al. 2007; Duffy et al. 2008), this actually increases the mass-concentration tension between observed inferred values and theoretical expectations.

  21. MACSJ1206 – Astronomy Picture of the Day

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