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Gravitational Lensing Analysis of CLASH clusters

Gravitational Lensing Analysis of CLASH clusters. Adi Zitrin @ HD 10/2011. Outline of talk. What have we done so far: clusters analyzed, methods, strong vs weak, recent developments What do we need to do by the next CLASH meeting How do we plan to do that. Bank of tools:.

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Gravitational Lensing Analysis of CLASH clusters

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  1. Gravitational Lensing Analysis of CLASH clusters Adi Zitrin @ HD 10/2011

  2. Outline of talk • What have we done so far: clusters analyzed, methods, strong vs weak, recent developments • What do we need to do by the next CLASH meeting • How do we plan to do that

  3. Bank of tools: Strong lensing: • Adi@Tom’s parametric method – ideal for finding multiple-images and to obtain a quick solution due to the small number of parameters. • Dan’s non-parametric method – very flexible and fast once multiple-images are known. • Stella’s etal parametric method. • Other public methods such as Lenstool etc for comparison if needed. Else?

  4. Bank of tools: Weak lensing: • Keiichi’s WL method (KSB based, Elinor’s color selection,Mario&Alberto). Both 1D, 2D analyses, recently including, importantly, a magnification bias constraint. • Keiichi’s multi-body method – same as above but by simulating several bodies – often seen also in background etc. • Claudio’s HST WL? • Stella’s etal, others?

  5. Bank of tools: Joint analysis: • One could combine independent SL and WL measurements, and say, fit an overall NFW profile etc. • Julian@Matthias’ SL+WL joint analysis method. Effect of LSS: • Ole, Ofer etal. Triaxiality fit: - Lensing+X-ray, SZ(?) – Dan, Megan etal

  6. What have we done so far?

  7. Abell 383 • SL+WL analysis, Paper accepted:

  8. MACS 1206 • SL analysis; Paper submitted ApJL

  9. A2261 • Paper ~ready, Coe etal, SL+WL, elongation, CM

  10. A2261

  11. Some preliminary modelsfor cycle 18 clusters: M11495 M0744 M2129 M0647

  12. Macs 0717 largest lens known

  13. Status and To-Do: In our lensing session tmrw we also need to decide on who does what

  14. What do we wish to study: • 1. Mass profiles (jointly)

  15. What do we wish to study: • 1a. Mass Profiles: establish an observational C-M relation, and the effect of triaxiality:

  16. What do we wish to study: • 1b. Magnification for High-z galaxies

  17. What do we wish to study: • 2a. Mass distribution: Strong regime: ellipticity, subtructure, effect on SL properties

  18. What do we wish to study: • 2b. Mass distribution: weak regime: multi-halo analysis and background structures BTW - More CCLs?

  19. What do we wish to study: • 2c: Mass distribution: constrain and calibrate the universal Einstein radius distribution: • 2d: Mass distribution: both regimes: how does DM condensate and concentrate? Could be put constraints on this? Tom? Leonidas?

  20. What do we wish to study: • 3. Constraints on the (higher end of) mass function • 4. Comparison to simulations, maybe look into over-cooling, feedback influence, adiabatic contraction

  21. What do we wish to study: • 5. Constraining the cosmological parameters: Dependence of the lensing distance (AD_dist) on the cosmological parameters. By Assuming different cosmologies one can probe the best fit (In prep., e.g.): Jullo + 2010 Zitrin + in prep. Jullo + 2010

  22. What do we wish to study: • 6. Very inner slopes, especially of/inside BCG regime. Need SL constraints from radial images, light SF, velocity dispersion etc. • Newman et al:

  23. Recent Development • MIF: fully automated Multiple-Image Finder • Goal: one button press to get a list of all multiple-images, with their redshift, and a refined lens or mass model. Possible? • Tryout: Gregor’s ArcFinder, BPZ (Txitxo, Alberto, Dan), Adi’s mass model: combined. • Let’s see a first result compared to a real analysis:

  24. Multiple-Image Finder: • Runtime of 1-2 days to finalized mass model!! (relative to ~1 month’s work before)

  25. Recent 2 • M1206 ref report + model-independent mass slope from multiple images (also for photo-z paper estimate on how errors propagate into the mass profile).

  26. Summary: • Many more CLASH clusters to analyze in SL, WL, derive mass distributions, profiles and Einstein radii, compare explicitly with X-ray, SZE, simulations. • C-M relation • CCL? • cD galaxies: M and M/L ratio and profile where multiple images are near. Inner profile • High-z galaxies • Constraints on cosmological models (later today) • Development of a tool for multiple-image finding • Details to be discussed in sessions

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