HSCWLWG (March 17, 2009) Mass Density Profiles of Strong Lensing Clusters Keiichi Umetsu (ASIAA, LeCosPA/NTU)

Radial Density Profiles of Self-Gravitating DM Halos Logarithmic density slope:  Inner density slope  Inner density slope,  r r  0 > Collisional nature of DM particles > DM equation-of-state (cold, warm) > Degree of velocity anisotropy: dynamics > Affect the DM annihilation rate (  DM 2 ) Outer density slope,  Outer density slope,  r r  Rvir > Smooth accretion after early fast collapse > boundary condition (finite mass)  Mass Concentration  Mass Concentration (e.g., C vir =R -2 /R vir ) > Imprints of structure formation > Growth of outskirts (Rvir, or Mvir) > Progenitor formation epoch (R -2 ): DE, Structure formation (  8)

Empirical NFW Profile for CDM Halos Jing & Suto 99 Simulation based prediction for gravitationally-bound CDM halos: Universal density profile of CDM halos Navaro,Frenk,& White (NFW) 96, 97 Equilibrium-state dln  /dlnr, sensitive to DM nature Outer: ρ ∝ r^ -3 Inner: ρ ∝ r^ -1 Galaxies Groups Clusters N-body CDM halos

LCDM Predictions?  Universal NFW profile (Navarro, Frenk, White 1996, 1997) N-body based empirical form:  DM “Entropy  DM “Entropy” (Bertschinger 1985; Taylor & Navarro 01; Hansen 04), related to a proximity to the coarse-grained phase-space density, Q(r)  -profile N-body simulations show a power-law behavior in equilibrium regions:  -profile (Navarro+08; Lapi & Cavariere 08,09)  -profileJeans eq  -profile + Jeans eq. allows for an analytical modeling of equilibrium-state CDM halo profiles (Lapi & Cavariere 08,09)  Range of density slope is constrained, with some correction by the velocity anisotropy,  (r)

Mass and Velocity Structure of A1689 (z=0.183)

Weak and Strong Lensing (Subaru/S-Cam + HST/ACS) oBroadhurst, Takada, KU et al. 05, ApJL oOguri, Takada, KU, Broadhurst 05 oMedezinski, Broadhurst, KU+07, ApJ oBroadhurst, KU et al. 08, ApJL oKU & Broadhurst 08, ApJ oKU+ 09, ApJ (AMiBA+Subaru)

Equilibrium-State DM Density Profile NFW (CDM) consistent profiles KU & Broadhurst 08, ApJ A1689 Broadhurst,KU+08, ApJL Surface mass density profile Tangential shear profile ACS high-resolution imaging  inner SL profile (<1’) S-Cam wide-field imaging  outer WL profile (1’<r<20’) Observational evidence of the continuously steepening density profile, dln  /dlnr(r), expected for collisionless, non-relativistic (Cold) DM

Weak/Strong Lensing and Cluster Dynamics (Subaru/S-Cam, HST/ACS, VLT/VIMOS) oLemze, Broadhurst, Rephaeli, Barkana, KU 09, ApJ accepted

Velocity Caustic Structure Lemze, Broadhurst, Rephaeli, Barkana, & KU 08, ApJ acceptd (arXiv: ) Projected velocity distribution of ~500 members Projected velocity distribution of ~500 members from VLT/VIMOS spec data Velocity Caustic Diagram Velocity Caustic Diagram (Diaferio 1999) -- Application to A1689 Zero escape-velocity the lensing derived R vir =2.1Mpc/h   Symmetric, smooth caustic curves steadily r>300kpc  relaxed, no- prominent velocity substructure   Reaching the zero matching the lensing-derived virial radius  clear boundary at R vir, well- isolated cluster   Caustics clearly separate cluster and field galaxies, allowing for an accurate measurement,  1D = (1400 +/- 60) km/s A(R): ~escape velocity A1689 (z=0.18)

Multi-Wavelength Dynamical Analysis for the 3D Velocity Anisotropy Jeans equation Jeans equation with “static”, “spherically symmetric” spatial distributions, but including 3D velocity anisotropy   Projected galaxy distribution as measured from S-Cam (Vi’) imaging   Projected velocity dispersion profile from 500 caustic-identified member galaxies from strong/weak lensing Solve J.Eq. for (1) the 3D galaxy density profile (n gal (r)) and (2) the 3D velocity anisotropy profile (  (r)) constrained by observed projected profiles:

Inner/Outer Density Slopes With the analytic DM “entropy” model in the framework of LCDM, L+C09 showed that the standard LCDM can explain simultaneously the observed flatter inner density slope and the steeper outer slope, assuming a central velocity-anisotropy dominated by tangential orbits (  (0)=-0.15). (Lapi & Cavaliere 09, ApJL accepted)

Radial Mass Density Profile of the Strong Lensing Cluster CL0024 (z=0.395) oZitrin, Broadhurst, KU et al. 09, ApJ submitted oKU+09, ApJ in prep.

HST ACS+NIC3 BVgriJH imaging for accurate photo-z of background galaxies 33 multiply lensed images (11 BG galaxies) in 8”<r<48”

ACS vs. Subaru Data Cluster virial radius (8’) HST/ACS (2’x2’ region) 33 multiply lensed images (11 BG galaxies) in 8”<r<48”

CL0024: Luminosity vs. Mass Maps

Subaru Distortion g+ Measurment

Comparison of g+ Profiles

Joint ACS+Subaru Constraints

Weak Lensing and SZE (Subaru/S-Cam + AMiBA)

Mass and Hot Baryons in a Merging Cluster First AMiBA7 papers: Ho et al. 2009, ApJ in press (arXiv: ) Nishioka et al. 2009, ApJ in press (arXiv: ) Umetsu et al. 2009, ApJ in press (arXiv: ) Wu et al. 2009, ApJ in press (arXiv: ) Koch et al., ApJS, submitted Lin et al., ApJ, submitted A few more science/instrumentation papers to be submitted to ApJ soon Color: AMiBA SZE decrement (Wu+09)  electron pressure Contours: Subaru WL (Okabe & Umetsu 08; Umetsu+09)  mass (~DM) A2142 (z=0.09) Ho+09

Weak/Strong Lensing, SZE, and X-ray (Subaru/S-Cam + HST/ACS + AMiBA + T X )

Cluster Hot-Baryon Fractions Umetsu+09, ApJ in press (arXiv: ) Averaged f gas profile of 4 AMiBA-lensing clusters with =1.2e15 M sun /h Averaged f gas profile of 4 AMiBA-lensing clusters with =1.2e15 M sun /h ( A1689,A2142,A2261,A2390 )   (22 +/- 16)% of the baryons are missing from the “hot” cluster environment (~5% accounted for by cold baryons)   First WL+SZE based f gas measurements on large scales (up to r200) without the hydrostatic-equilibrium assumption   Consistent with X-ray based measurements with the hydro- equilibrium assumption