Cluster Lenses High Redshift Clusters MACS A Status

Cluster Lenses & High Redshift Clusters (MACS) A Status Report Jean-Paul KNEIB Observatoire Astronomique Marseille Provence, Marseille, France H. Ebeling, G. Smith, A. Gal-Yam, I. Smail, A. Edge, J. Greene, P. Hudelot, S. Bardeau, G. Soucail, P. Marshall, E. Egami, G. Covone, E. Jullo and many others October 25, 2005 Ringberg, Hi-z clusters

Outline v. Lensing in Clusters v. Mass Distribution in Cluster: strong & weak lensing at low-z v. MACS Clusters (0. 3<z<0. 8): v. ACS deep survey v. MACS Snapshot, RXJ 0152 v(SN search) v. Future prospects October 25, 2005 Ringberg, Hi-z clusters 2

Theory: Lens Diagram CFHT BRI 1990 Z_cluster=0. 375 Z_arc=0. 725 (Soucail et al 1988) October 25, 2005 Ringberg, Hi-z clusters 3

Science with Cluster Lenses • Study the mass distribution of cluster => cosmology? • Study the distant lensed Universe • Direct constrain on cosmological parameters October 25, 2005 Ringberg, Hi-z clusters 4

Theory: Lens Mapping a The lensing equation is a mapping from image plane to source plane: q - b = Dls/Ds. a = Dls/Ds df/dq For a point mass, the deflection angle is: a = 4 GM/bc 2 (b is the impact parameter) -> typically 10” for a 1014 Solar mass Amplification matrix: October 25, 2005 Ringberg, Hi-z clusters 5

Cluster Lenses Insensitive to: • Nature of matter • Physical state of matter Cleanest available probe of Dark Matter Strong Lensing in the core, Weak lensing on large scale Most massive clusters Einstein radius: 10 -45” October 25, 2005 Ned Wrigth, UCLA Ringberg, Hi-z clusters 6

Mass distribution in cluster cores October 25, 2005 Ringberg, Hi-z clusters 7

Cluster Lens: Mass Reconstruction • Parameterized mass distribution, involving various multiple image system (works better, less free parameters) • Need to include galaxy scale mass components using scaling relations (dominate locally the mass) October 25, 2005 Ringberg, Hi-z clusters 8

Strong and Weak Lensing Absolute central mass October 25, 2005 relative total mass and slope Ringberg, Hi-z clusters 9

An Example from space: Cl 0024+1654 HST wide field sparse mosaic • 76 orbits, 38 pointings • Probe regions up to ~5 Mpc Aim: learn cluster physics of clusters by comparing with other mass estimates: X-ray, dynamics October 25, 2005 (Treu et al 2003, Kneib et al 2003) Ringberg, Hi-z clusters 10

0024: Shear Profile SIS fitting strong lensing data • Extrapolate strong lensing models at large scale by exploring various cluster mass profile. • Rule out SIS model • NFW (with large c~20) or Power-law models give comparatively good model. October 25, 2005 NFW fitting strong And weak lesning ~3 Mpc Ringberg, Hi-z clusters 11

Cl 0024: Mass vs. Light • NFW and Power-Law model fit the strong+weak lensing But high concentration compared to expectations (similar results on other clusters: A 1689 …) Mass traces Light !!! Red sequence selection Light profile NFW model Broader sequence selection SIS model fitting weak lensing • SIS does not fit the strong+weak lensing • M/L is constant with radius with M/LK~40 October 25, 2005 Kneib et al 2003 Ringberg, Hi-z clusters 12

Questions for Cluster Physics • What are the total mass and structural properties of massive clusters? • How are the mass and structure of clusters related to the global thermodynamics (Tx, Lx)? • How do cluster substructure and thermodynamics evolve with redshift? • Implications of cluster mass and substructure for cluster Cosmology? October 25, 2005 Ringberg, Hi-z clusters 13

X-ray Luminosity Multi-wavelength/epoch study Dt~2 Gyr z=0 z=0. 2 2 Gyr • z=0. 21+/-0. 04 • Lx>8 x 1044 erg/s z=0. 5 z~1 • Study of 10 clusters at z~0. 2 – – HST, WFPC 2, F 702 W, 7 5 ksec Chandra, ACIS-I(S), 4 -40 ksec UKIRT, UFTI, 9 ksec October 25, 2005 Ringberg, Hi-z clusters CFHT 12 k, BRI, weak shear A 68 A 209 A 267 A 383 A 773 A 963 Ellis et al. 1991 A 1763 A 1835 A 2218 Kneib et al. 1996 A 2219 Smail et al. 1995 14

Example: Abell 68 (z=0. 25) Smith et al 2001, 2003, 2005 Triply-imaged “ERO” R-K=5. 4 z=1. 6 Data and constraints – ID multiple image systems (HST) – Spectroscopic redshifts (Keck+) – Weak lensing constraints (HST) Measurements – Cluster mass (R<500 kpc) – Dark matter morphology October 25, 2005 Ringberg, Hi-z clusters 15

Quantitative structural classification Smith et al. , 2005 Relaxed Typical Unrelaxed Atypical Unrelaxed Mass [Lensing] ICM [X-ray] Ndm 1 Mcen/Mtot Ttot/Tann Δr (arcsec) 2 1 0. 97± 0. 01 0. 77± 0. 01 0. 8± 0. 1 1. 0± 0. 1 <1 10± 2 22± 1 0. 96± 0. 01 1. 0± 0. 2 Ø 70% of X-ray luminous cluster cores at z=0. 2 are dynamically immature and strongly heterogeneous October 25, 2005 Ringberg, Hi-z clusters 16

M-T relation or M-T scatter plot? Smith et al. , 2005 Structural segregatio n [~40%] Finoguenov et al. , 2001 Possible Systematics? [~10 -20%] • Unrelaxed clusters are 40% hotter than relaxed clusters (2. 5σ) • Consistent with hydro simulations of cluster-cluster mergers (Ricker & Sarazin 2001, Randall et al. 2003) October 25, 2005 Ringberg, Hi-z clusters 17

Better agreement with weak lensing? October 25, 2005 Ringberg, Hi-z clusters 18

weak lensing shear profile October 25, 2005 Ringberg, Hi-z clusters 19

(~150 z/cluster) lensing dynamics weak lensing scatter plots… Lensing October 25, 2005 Ringberg, Hi-z clusters X-ray 20

Better agreement with weak lensing? • Offset between dynamics and mass: sign of merger due to optical selection ? Or the fact that those systems are still young? • A big scatter between Tx and Mass: we can probably do better (including strong lensing) but … limited by cluster substructure • Need better data and statistics … ie. go from sample of 10 s to sample of 100 s October 25, 2005 Ringberg, Hi-z clusters 21

The MAssive Cluster Survey (MACS) • MACS is covering a very wide area and thus is able to discover the most x-ray luminous clusters unlike other surveys. • Most massive clusters should be strong lenses • ~120 z>0. 3 MACS clusters to be observed with Chandra & ACS SNAP • 10 MACS cluster have been observed with HST/ACS October 25, 2005 Ringberg, Hi-z clusters 22

MACS clusters at 0. 5<z<0. 6 2 Gyr • 10 clusters at z~0. 55 • HST/ACS imaging 2 Gyr X-ray Luminosity Dt~2 Gyr z=0 – F 555 W, F 814 W – 5 ksec/filter • Keck/LRIS + VLT/FORS spectroscopy (arcs and cluster galaxies) z=0. 2 z=0. 5 z~1 – Blue and Red spectroscopy • SUBARU/Suprime imaging – Weak lensing and galaxy population October 25, 2005 Ringberg, Hi-z clusters 23

MACS 1149 z=1. 5 z=1. 89 October 25, 2005 Ringberg, Hi-z clusters 24

MACS 0717 z=2. 96 Ly- blob October 25, 2005 Ringberg, Hi-z clusters 25

MACS 0257 z=1. 06 October 25, 2005 Ringberg, Hi-z clusters 26

MACS/HST weak lensing October 25, 2005 Ringberg, Hi-z clusters 27

MACS/HST weak lensing Marshall et al 2006 Cluster mass reconstruction method using (NFW) blobs that can combine strong+weak lensing data: using MCMC techniques To cope with complex Shape seen at high-z Simulation data Atomic Inference October 25, 2005 Classical 2 D reconstruction Ringberg, Hi-z clusters 28

4 Mpc filament in MACSJ 0717. 5+3745 Ebeling et al (GO: 10420, cycle 14) X-ray+Gal density October 25, 2005 Lensing Subaru+Gal density+ ACS survey Ringberg, Hi-z clusters 29

4 Mpc filament in MACSJ 0717. 5+3745 Ebeling, Barrett, Donovan, 2004 Galaxies with Spectra October 25, 2005 Redshift distribution Ringberg, Hi-z clusters 30

Does cluster substructure evolve? • Current status of MACS strong lensing analysis – Candidate gravitational multiple images identified – [Ground-based spectroscopy of arcs <~50% complete] • Broad brush demographics: z=0. 2 z=0. 55 Strong lensing clusters 8/10 Unrelaxed clusters 4/10 9/10 Candidate unrelaxed clusters Relaxed cool core clusters 2/10 Relaxed non cool core clusters October 25, 2005 10/10 3/10 1/10 Ringberg, Hi-z clusters 7 9 0/10 3 1 0/10 31

MACS Snapshot ACS Ebeling et al (GO: 10491, cycle 14) • List of 124 MACS clusters to be observed with HST/ACS in SNAP mode in F 814 W • Aim at finding effective lensing clusters and strongly distorted arcs (statistics and magnified sources) • 5 clusters already observed October 25, 2005 Ringberg, Hi-z clusters 32

MACS Snapshot ACS Ebeling et al (GO: 10491) First Strong Lensing IDs October 25, 2005 Ringberg, Hi-z clusters 33

RXJ 0152 -29 a massive cluster at z~0. 83 • X-ray luminous cluster at z=0. 83 • At least 8 multiple image systems, one at z=3. 9 (Umetsu et al 2005)=> high ellipticity for DM, indicative of a merger. • Ideal probe for VIMOS/IFU • Potential interest for cosmology (Golse et al 2002) October 25, 2005 VIMOS/IFU Field of view Ringberg, Hi-z clusters

Lensing for Cluster Physics • Lensing is probing mass relatively easily, measuring substructure gets more difficult at higher z, but is clearly seen! • Scattered relation between Mass and X-ray depends on physical state and substructure (merger/relaxed) • Higher substructures at higher redshift (lots of lensing till z~0. 8 in massive systems)? • Cosmology with cluster is likely to be hard - at least with current cluster sample size (10 s) need much larger sample, but will learn some physics. October 25, 2005 Ringberg, Hi-z clusters 35