Gravitational Lensing Analysis of CLASH clusters
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Transcript of Gravitational Lensing Analysis of CLASH clusters
Gravitational LensingAnalysis 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: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?
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?
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
What have we done so far?
Abell 383• SL+WL analysis, Paper accepted:
MACS 1206
• SL analysis; Paper submitted ApJL
A2261
• Paper ~ready, Coe etal, SL+WL, elongation, CM
A2261
Some preliminary modelsfor cycle 18 clusters:
M11495 M0744
M0647M2129
Macs 0717 largest lens known
Status and To-Do:
In our lensing session tmrw we also need to decide on who does what
What do we wish to study:
• 1. Mass profiles (jointly)
• 1a. Mass Profiles: establish an observational C-M relation, and the effect of triaxiality:
What do we wish to study:
What do we wish to study:
• 1b. Magnification for High-z galaxies
• 2a. Mass distribution: Strong regime: ellipticity, subtructure, effect on SL properties
What do we wish to study:
• 2b. Mass distribution: weak regime: multi-halo analysis and background structures
What do we wish to study:
BTW - More CCLs?
• 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?
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
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.):
Zitrin + in prep.
Jullo + 2010
Jullo + 2010
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:
What do we wish to study:
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:
Multiple-Image Finder:
• Runtime of 1-2 days to finalized mass model!! (relative to ~1 month’s work before)
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).
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