Galaxy Galaxy Lensing in CLASH clusters

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Elinor Medezinski Johns Hopkins University Galaxy Galaxy Lensing in CLASH clusters

description

Galaxy Galaxy Lensing in CLASH clusters. Elinor Medezinski Johns Hopkins University. Galaxy-Galaxy Lensing. Dynamical methods work well within optical radius r < 20 kpc Galaxy-Galaxy lensing is a unique method to probe galaxy Dark Matter Halos out to large radii - PowerPoint PPT Presentation

Transcript of Galaxy Galaxy Lensing in CLASH clusters

Page 1: Galaxy Galaxy Lensing in CLASH  clusters

Elinor Medezinski

Johns Hopkins University

Galaxy Galaxy Lensing in CLASH clusters

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E. Medezinski - CLASH team meeting

Galaxy-Galaxy LensingDynamical methods work well within optical radius r < 20 kpc

Galaxy-Galaxy lensing is a unique method to probe galaxy Dark Matter Halos out to large radii

100 h-1kpc ~ 200 h-1kpc

Stacking background galaxies inside aperture around cluster galaxy gives mass of galaxy lens

Averaging over many cluster galaxies within cluster annulus averages out cluster contribution

One can then deduce:M/L ratios of galaxiesTruncation of galaxies in different part of clusters

aperture

cluster

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E. Medezinski - CLASH team meeting

B-R vs. R-z’ selected samples

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E. Medezinski - CLASH team meeting

Truncated Singular Isothermal Sphere (TSIS) density profile

2sin2cos)(1

)()(1

4

,rrfor 0

rrfor cos14

242

rrfor 0

rrfor 2

21

2

t

t1

2

2

22

2

2

2

2

ggrgrrr

rrrg

DDD

Gc

rr

rDDD

crr

GRdrr

GrM

Grr

LSL

scrit

tS

LSLv

crit

tvvsubhalo

t

tv

TSIS

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Marginalize over parameter space to find best-fit V,Rt,,

Exclude inner 20-30 kpc/h from fit

E. Medezinski - CLASH team meeting

MCMC analysis

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MACSJ1206 MCMC results0.1Rvir<R<0.6Rvir

0.6Rvir<R<1.1Rvir

1.1Rvir<R<1.8Rvir

1.8Rvir<R<2.8Rvir

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Exclude inner cluster core where strong contribution from cluster lensingHalo truncated outside R>Rvir

E. Medezinski - CLASH team meeting

Halo properties vs. Cluster radius – MACSJ1206

Truncation radius galaxy type

Mass Luminosity M/L

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E. Medezinski - CLASH team meeting

Use specstroscopic redshifts to reliably select a subsample of cluster galaxies.

Two main clouds – red and blue cluster galaxies

Spec-z selected samples

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E. Medezinski - CLASH team meeting

Red galaxies clustered, blue galaxies not clustered – do they belong to the cluster?

Number density profiles

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E. Medezinski - CLASH team meeting

Red cluster g-gMass Luminosity M/L

Truncation radius galaxy type

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Blue cluster (?) g-gMass Luminosity M/L

Truncation radius galaxy type

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A2261 Results – CC selected sample

E. Medezinski - CLASH team meeting

Truncation radius galaxy type

Mass Luminosity M/L

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A2261 BVR from Subaru, i'z' from KPNO – shallow.

galaxy type

Red cl. Blue cl.

Mass

Luminosity

M/L

Truncation radius galaxy type

Luminosity

Truncation radius

M/L

Mass

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E. Medezinski - CLASH team meeting

A383

Problems – not as deep (old reduction of Mario) l.o.s stuctures, cluster substructure No spec-z's redshifts of cluster galaxies

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A370 ZwCl0024

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Natarajan et al. 2009

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Next steps More clusters with more spectro-selected cluster

galaxies Use 2D multi-halo model to subtract cluster

lensing contribution Incorporate HST shapes in centeral bins Try other galaxy mass models? NFW? Stack several clusters for better statistics Divide by stellar mass, local density, type etc. to

get information on the galactic halo in different enviroments