cluster lenses & high redshift clusters (macs) a status report

Cluster Lenses & Cluster Lenses & High Redshift Clusters (MACS)High Redshift Clusters (MACS)

A Status ReportA Status Report Jean-Paul KNEIBJean-Paul KNEIB

Observatoire Astronomique Marseille Provence, Marseille, France

H. Ebeling, G. Smith, H. Ebeling, G. Smith, A. Gal-Yam, I. Smail, A. Edge, J. Greene, P. Hudelot, S. I. Smail, A. Edge, J. Greene, P. Hudelot, S. Bardeau, G. Soucail, P. Marshall, E. Egami, G. Covone, E.Jullo and many othersBardeau, G. Soucail, P. Marshall, E. Egami, G. Covone, E.Jullo and many others

October 25, 2005 Ringberg, Hi-z clusters 2

OutlineLensing in ClustersMass Distribution in Cluster: strong & weak lensing at low-zMACS Clusters (0.3<z<0.8):

ACS deep surveyMACS Snapshot, RXJ0152(SN search)

Future prospects


Theory: Lens DiagramTheory: Lens Diagram

CFHT BRI 1990

Z_cluster=0.375Z_arc=0.725 (Soucail et al 1988)


Science with Cluster LensesScience with Cluster Lenses

• Study the mass distribution of cluster => cosmology?

• Study the distant lensed Universe

• Direct constrain on cosmological parameters


The lensing equation is a mapping from image plane to source plane:

Dls/DsDls/Ds

For a point mass, the deflection angle is: 4GM/bc2

(b is the impact parameter) -> typically 10” for a 1014 Solar mass

Amplification

matrix:

Theory: Lens MappingTheory: Lens Mapping


Cluster LensesCluster Lenses

Most massive clustersEinstein radius: 10-45”

Strong Lensing in the core,Weak lensing on large scale

Ned Wrigth, UCLA

Insensitive to:

•Nature of matter

•Physical state of matter

Cleanest available probe of Dark Matter


Mass distribution in cluster coresMass distribution in cluster cores


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)


Strong and Weak LensingStrong and Weak LensingAbsolute central mass relative total mass and slope


An Example from An Example from space:space:

Cl0024+1654Cl0024+1654 HST wide field HST wide field sparse mosaicsparse mosaic

• 76 orbits, 38 pointings• Probe regions up to ~5Mpc

Aim: learn cluster physics of clusters by comparing with other mass estimates: X-ray, dynamics

(Treu et al 2003, Kneib et al 2003)


0024: Shear Profile0024: Shear Profile

• 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.

SIS fitting strong lensing dataSIS fitting strong lensing data

NFW fitting strongNFW fitting strongAnd weak lesningAnd weak lesning

~3 Mpc


Cl0024: Mass vs. LightCl0024: Mass vs. Light

•NFW and Power-Law model fit the strong+weak lensingBut high concentration compared to expectations(similar results on other clusters: A1689 …)

•SIS does not fit the strong+weak lensing

•M/L is constant with radius with M/LK~40

Mass traces Light !!!Mass traces Light !!!

Kneib et al 2003

SIS model fitting SIS model fitting weak lensingweak lensing

NFW modelNFW model

Light profileLight profile

Red sequence selectionRed sequence selection

Broader sequence selectionBroader sequence selection


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?


Multi-wavelength/epoch study

• Study of 10 clusters at z~0.2– HST, WFPC2, F702W, 75ksec

– Chandra, ACIS-I(S), 4-40ksec

– UKIRT, UFTI, 9ksec

– CFHT12k, BRI, weak shear

• z=0.21+/-0.04

• Lx>8x1044erg/sA68

A209

A267

A383

A773

A963 Ellis et al. 1991

A1763

A1835

A2218 Kneib et al. 1996

A2219 Smail et al. 1995

X-r

ay L

um

inosit

y t~2Gyr 2Gyr 2Gyr

z=0 z=0.2 z=0.5 z~1


Example:Abell 68 (z=0.25)

Data and constraints– ID multiple image systems (HST)

– Spectroscopic redshifts (Keck+)

– Weak lensing constraints (HST)

Measurements– Cluster mass (R<500kpc)

– Dark matter morphology

Triply-imaged “ERO”R-K=5.4

z=1.6

Smith et al 2001,2003,2005


Quantitative structural classificationRelaxedRelaxed

MassMass

[Lensin[Lensing]g]

ICMICM

[X-ray][X-ray]

Typical Typical UnrelaxedUnrelaxed

Atypical Atypical UnrelaxedUnrelaxed

70% of X-ray luminous cluster cores at z=0.2 are dynamically immature and strongly heterogeneous

Ndm 1 2 1

Mcen/Mtot 0.97±0.01 0.77±0.01 0.96±0.01

Ttot/Tann 0.8±0.1 1.0±0.1 1.0±0.2Δr (arcsec) <1 10±2 22±1

Smith et al., Smith et al., 20052005


M-T relation or M-T scatter plot?

Smith et al., 2005StructurStructur

al al segregatsegregat

ionion[~40%][~40%]

PossiblePossibleSystematicSystematic

s?s?[~10-20%][~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)

Finoguenov et al., 2001


Better agreement with weak lensing?


weak lensing shear profile


weak lensing scatter plots…

Lensing

dyna

mic

s

lens

ing

X-ray

(~150 z/cluster)


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 10s to sample of 100s


The MAssive Cluster Survey (MACS)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


MACS clusters at 0.5<z<0.6X

-ray L

um

inosit

yt~2Gyr 2Gyr 2Gyr

z=0 z=0.2 z=0.5 z~1

• 10 clusters at z~0.55• HST/ACS imaging

– F555W, F814W– 5ksec/filter

• Keck/LRIS + VLT/FORS spectroscopy (arcs and cluster galaxies)– Blue and Red spectroscopy

• SUBARU/Suprime imaging– Weak lensing and galaxy

population


MACS 1149

z=1.89

z=1.5


MACS 0717

z=2.96Ly- blob


MACS 0257

z=1.06


MA

CS

/HS

T w

eak

lens

ing


MA

CS

/HS

T w

eak

lens

ing

Atomic Inference

Simulation data

Classical 2D reconstruction

Cluster mass reconstruction method using (NFW) blobs that can combine strong+weak lensing data: usingMCMC techniquesTo cope with complexShape seen at high-z

Marshall et al 2006


4Mpc filament in MACSJ0717.5+3745Ebeling et al (GO: 10420, cycle 14)

X-ray+Gal density Lensing Subaru+Gal density+ ACS survey


4Mpc filament in MACSJ0717.5+3745Ebeling, Barrett, Donovan, 2004

Galaxies with Spectra Redshift distribution


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=0.2z=0.55

Strong lensing clusters 8/1010/10

Unrelaxed clusters 4/10 9/10

Candidate unrelaxed clusters 3/10 0/10

Relaxed cool core clusters 2/10 1/10

Relaxed non cool core clusters 1/10 0/10

7

3

9

1


MACS Snapshot ACSEbeling et al (GO: 10491, cycle 14)

• List of 124 MACS clusters to be observed with HST/ACS in SNAP mode in F814W

• Aim at finding effective lensing clusters and strongly distorted arcs (statistics and magnified sources)

• 5 clusters already observed


MACS Snapshot ACSEbeling et al (GO: 10491) First Strong Lensing IDsFirst Strong Lensing IDs

RXJ0152-29 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)

VIMOS/IFUVIMOS/IFUField of viewField of view


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 (10s) need much larger sample, but will learn some physics.

cluster lenses & high redshift clusters (macs) a status report

Documents

mass distribution of

implications of cluster

z clustersstrong

z clustersquestions

z clusters0024

z clusterscl0024

z clustersoutlinelensing

z clustersscience