cluster lenses & high redshift clusters (macs) a status report
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Cluster Lenses & High Redshift Clusters (MACS) A Status Report. Jean-Paul KNEIB Observatoire Astronomique Marseille Provence , Marseille, France - PowerPoint PPT PresentationTRANSCRIPT
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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
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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
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October 25, 2005 Ringberg, Hi-z clusters 3
Theory: Lens DiagramTheory: Lens Diagram
CFHT BRI 1990
Z_cluster=0.375Z_arc=0.725 (Soucail et al 1988)
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October 25, 2005 Ringberg, Hi-z clusters 4
Science with Cluster LensesScience with Cluster Lenses
• Study the mass distribution of cluster => cosmology?
• Study the distant lensed Universe
• Direct constrain on cosmological parameters
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October 25, 2005 Ringberg, Hi-z clusters 5
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
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October 25, 2005 Ringberg, Hi-z clusters 6
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
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October 25, 2005 Ringberg, Hi-z clusters 7
Mass distribution in cluster coresMass distribution in cluster cores
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October 25, 2005 Ringberg, Hi-z clusters 8
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)
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October 25, 2005 Ringberg, Hi-z clusters 9
Strong and Weak LensingStrong and Weak LensingAbsolute central mass relative total mass and slope
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October 25, 2005 Ringberg, Hi-z clusters 10
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)
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October 25, 2005 Ringberg, Hi-z clusters 11
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
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October 25, 2005 Ringberg, Hi-z clusters 12
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
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October 25, 2005 Ringberg, Hi-z clusters 13
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?
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October 25, 2005 Ringberg, Hi-z clusters 14
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
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October 25, 2005 Ringberg, Hi-z clusters 15
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
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October 25, 2005 Ringberg, Hi-z clusters 16
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
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October 25, 2005 Ringberg, Hi-z clusters 17
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
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October 25, 2005 Ringberg, Hi-z clusters 18
Better agreement with weak lensing?
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October 25, 2005 Ringberg, Hi-z clusters 19
weak lensing shear profile
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October 25, 2005 Ringberg, Hi-z clusters 20
weak lensing scatter plots…
Lensing
dyna
mic
s
lens
ing
X-ray
(~150 z/cluster)
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October 25, 2005 Ringberg, Hi-z clusters 21
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
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October 25, 2005 Ringberg, Hi-z clusters 22
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
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October 25, 2005 Ringberg, Hi-z clusters 23
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
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October 25, 2005 Ringberg, Hi-z clusters 24
MACS 1149
z=1.89
z=1.5
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October 25, 2005 Ringberg, Hi-z clusters 25
MACS 0717
z=2.96Ly- blob
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October 25, 2005 Ringberg, Hi-z clusters 26
MACS 0257
z=1.06
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October 25, 2005 Ringberg, Hi-z clusters 27
MA
CS
/HS
T w
eak
lens
ing
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October 25, 2005 Ringberg, Hi-z clusters 28
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
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October 25, 2005 Ringberg, Hi-z clusters 29
4Mpc filament in MACSJ0717.5+3745Ebeling et al (GO: 10420, cycle 14)
X-ray+Gal density Lensing Subaru+Gal density+ ACS survey
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October 25, 2005 Ringberg, Hi-z clusters 30
4Mpc filament in MACSJ0717.5+3745Ebeling, Barrett, Donovan, 2004
Galaxies with Spectra Redshift distribution
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October 25, 2005 Ringberg, Hi-z clusters 31
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
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October 25, 2005 Ringberg, Hi-z clusters 32
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
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October 25, 2005 Ringberg, Hi-z clusters 33
MACS Snapshot ACSEbeling et al (GO: 10491) First Strong Lensing IDsFirst Strong Lensing IDs
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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
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October 25, 2005 Ringberg, Hi-z clusters 35
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.