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