CLASH: Cluster Lensing And Supernova survey with Hubble

ACS Parallels

WFC3 Parallels

6 arcmin. = 2.2 Mpc @ z=0.5

Footprints of HST Cameras: ACS FOV in yellow, WFC3/IR FOV in red, WFC3/UVIS in blue.

Cluster Pointings

SN search cadence:10d-20d, 4 epochs per orient

Lensing amplification small at these radii524 orbits, 25 clusters, 16 filters, ~3 years

M. Postman, P.I., with 34 co-investigators (18 institutions, 10 countries)

Abell 209 Abell 383 core Abell 611 Abell 963 Abell 2261 CLJ1226+3332

MACS 0329-0211 MACS 0717+3745 MACS 0744+3927 MACS 1115+0129 MACS 1149+2223 MACS 1206-0847

RXJ 0647+7015

Cutouts of x-ray images of 23 of the 25 CLASH clusters from Chandra Observatory

RXJ 1347-1145 RXJ 1423+2404 MS-2137 core RXJ 1720+3536 RXJ 2129+0005

MACS 0429-0253 MACS 1311-0310 RXJ 1532+3020 MACS 1931-2634 RXJ 2248-4431

All clusters have

Tx > 5 keV

z_med ~ 0.4

CLASH: 16 Passbands per cluster from UV to NIR

Mag distn of multiply lensed arcs in A1689 and CL0024

Will yield photometric redshifts with rms error of ~2% x (1 + z) for sources down to ~26 AB mag.

Spectroscopicredshifts

Photometricredshifts

Why 16 filters?

Arcs in A1689 and CL0024

F225W … 235.9 nm WFC3/UVISF275W … 270.4 nm WFC3/UVISF336W … 335.5 nm WFC3/UVISF390W … 392.1 nm WFC3/UVIS

F435W … 430.6 nm ACS/WFCF475W … 474.2 nm ACS/WFC F606W … 592.0 nm ACS/WFCF625W … 629.8 nm ACS/WFCF775W … 769.4 nm ACS/WFCF814W … 806.9 nm ACS/WFCF850LP … 906.0 nm ACS/WFC

F105W … 1.055 μm WFC3/IRF110W … 1.152 μm WFC3/IRF125W … 1.248 μm WFC3/IRF140W … 1.392 μm WFC3/IRF160W … 1.536 μm WFC3/IR

What is the characteristic distribution of DM in a typical cluster, and what implications does this distribution have

for structure formation and the nature of DM?

CLASH will: • Use 3 independent lensing constraints: SL, WL, mag bias• Have a well-selected cluster sample with minimal lensing bias• Definitively derive the representative equilibrium mass profile shape• Robustly measure cluster DM concentrations and their dispersion as a function of cluster mass (and possibly their redshift evolution).

• Provide excellent calibration of mass-observable relations for clusters

ΛC

DM

The

ory

ΛC

DM

The

ory

LCDM prediction from Duffy et al. 2008Umetsu et al. 2010

Abell 1689 Coe et al. 2010

What degree of substructure exists in the DM distribution in cluster cores?

HST Image of Cluster Reconstructed Mass Surface Density

Region of Reliable Reconstruction

DM substructure resolution in this map is ~23 kpc. DM substructure resolution for typical CLASH cluster will be ~30 – 40 kpc.

First CLASH Cluster: Abell 383

Does the Equation of State of Dark Energy Depend on Time?

Reference Discovery Difference Nov 18, 2010 Dec 8, 2010 Dec 28, 2010

WFC3-IR, F160W, z ~ 0.7 or 1.7 ACS, F850LP, z ~ 0.3

Abell 383 SN Candidate “Caligula” Abell 383 SN Candidate “Nero”

HST LIFETIME

CURRENT

MCTMCTΔ

mag

(vs.

wo =

-1, w

a = 0

)

Expect CLASH to find 10 – 20 SNe at z>1; and ~6 with z > 1.5, doubling the known number of z > 1 SNe.

Two MCT HST programs (CLASH and CANDELS) will detect SNe Ia at 1.0 < z < 2.5.

CLASH and CANDELS provide a direct test of the SN systematics in a matter-dominated universe.

Lensing greatly enhances the ability to detect distant galaxies and provides an additional constraint on their redshifts, as the projected position of the lensed object

is a function of the source redshift.

What are the characteristics of the most distant galaxies in the universe?

Bradley et al. 2010 (in prep): Abell 1703 – Brightest z ~ 7 candidate known (H160 ~ 24.3 AB), μ ~ 3 - 5

■ Reconstruction of a z = 4.92 source lensed by the z = 0.33 cluster MS1358+62.

■ Best resolved high-z object: spatial resolution of ~50 pc (rest-frame UV)

■ Equivalent to 20-m space telescope resolution of a non-lensed z=5 galaxy!

Zitrin et al. 2010

0.2”

ACS PSFz = 4.92 Galaxy

How object would look without cluster lensing

Concluding Comments CLASH observations with HST began in

November. The 25 clusters will be observed over the course of cycles 18-20 (~3 years): 10, 10, 5.

Represents a major observational initiative to constrain the properties of DM, high-z galaxies, and advance our understanding of DE.

Immediate public access to all HST data. High-level science products will be released on

a regular schedule, including compilations of x-ray, IR, sub-mm, and spectroscopic data.

http://www.stsci.edu/~postman/CLASH

CLASH Yields a Significant Expansion of SL Cluster Data

Strongly Lensing Clusters with 3 or more filters from HST (ACS and/or WFC3)

Figure credit: Dan Coe

CLASH doubles the number of SL clusters with >3 HST passbands.CLASH has uniform and well-defined sample selection criteria.

Vast improvement in number of SLCs with >6 passbands – new territory for science.