Weak lensing mass-selected cluster Weak lensing mass-selected cluster cataloguescatalogues

Richard Massey (CalTech)

with

Justin Albert (CalTech), Joel Berge (Saclay), Richard Ellis (CalTech), Takashi Hamana (Tokyo),

Jean-Paul Kneib (Marseille), Alexie Leauthaud (Marseille), Satoshi Miyazaki (Subaru), Alexandre Refregier (Saclay), Jason

Rhodes (JPL), Nick Scoville (CalTech),James Taylor (CalTech) and the COSMOS team

Lensing sensitivity with redshiftLensing sensitivity with redshiftN

um

ber

of

reso

lved

gala

xie

s

z

Clusters are just… Clusters are just… patterns in a shear fieldpatterns in a shear field

Patterns in a shear fieldPatterns in a shear field

Mass maps from ACS dataMass maps from ACS data

Residual systematics in ACS dataResidual systematics in ACS data

Residual systematics in ACS dataResidual systematics in ACS data

E-mode signal

B-mode signal

Theory

Mass vs lightMass vs light

Nick Scoville

Mass vs x-raysMass vs x-rays

Gunther Hasinger, Alexis Finoguenov & Nico Cappelluti

Tomography (3D maps)Tomography (3D maps)N

um

ber

of

reso

lved

gala

xie

s

z

Tomography (3D maps)Tomography (3D maps)

Tomography (3D maps):Tomography (3D maps):z~0.3z~0.3

Tomography (3D maps):Tomography (3D maps):z~0.5z~0.5

Tomography (3D maps):Tomography (3D maps):z~0.7z~0.7

Shear measurement from SubaruShear measurement from Subaru

Deconvolve from the ground-based PSF using shapelets.

~25 galaxies/arcmin2 with Subaru data, rather than ~60 galaxies/arcmin2 using ACS

Su

baru

sh

ear

(sh

ap

ele

ts)

Subaru mass mapsSubaru mass maps

Subaru mass mapsSubaru mass maps

Residual systematics in Subaru Residual systematics in Subaru datadata

1% level residuals

FITS versions of all these maps available at: www.astro.caltech.edu/~rjm/mass_maps

ConclusionsConclusionsProjected 2D mass maps

Somewhat coarser 3D mass maps

More optimally-tuned analysis around identified structures

Systematics checks: E/B-mode split

Systematics checks: ground vs space