Clash c luster l ensing a nd s upernova survey with h ubble
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CLASH: C luster L ensing A nd S upernova survey with H ubble. M. Postman, P.I., with 34 co-investigators (18 institutions, 10 countries) . WFC3 Parallels. Cluster Pointings. ACS Parallels. 6 arcmin. = 2.2 Mpc @ z=0.5. SN search cadence: 10d-20d , 4 epochs per orient.

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CLASH: C luster L ensing A nd S upernova survey with H ubble

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Clash c luster l ensing a nd s upernova survey with h ubble

CLASH:Cluster Lensing And Supernova survey with Hubble

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

WFC3 Parallels

Cluster Pointings

ACS Parallels

6 arcmin. = 2.2 Mpc @ z=0.5

SN search cadence:

10d-20d, 4 epochs per orient

Footprints of HST Cameras: ACS FOV in yellow,

WFC3/IR FOV in red, WFC3/UVIS in blue.

Lensing amplification small at these radii

524 orbits, 25 clusters, 16 filters, ~3 years


Clash c luster l ensing a nd s upernova survey with h ubble

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

MS-2137 core

RXJ 0647+7015

RXJ 1347-1145

RXJ 1423+2404

RXJ 1720+3536

RXJ 2129+0005

All clusters have

Tx > 5 keV

z_med ~ 0.4

MACS 0429-0253

RXJ 1532+3020

MACS 1931-2634

RXJ 2248-4431

MACS 1311-0310

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


Clash 16 passbands per cluster from uv to nir

CLASH: 16 Passbands per cluster from UV to NIR

Why 16 filters?

Spectroscopic

redshifts

Photometric

redshifts

  • F225W … 235.9 nm WFC3/UVIS

  • F275W … 270.4 nm WFC3/UVIS

  • F336W … 335.5 nm WFC3/UVIS

  • F390W … 392.1 nm WFC3/UVIS

  • F435W … 430.6 nm ACS/WFC

  • F475W … 474.2 nm ACS/WFC

  • F606W … 592.0 nm ACS/WFC

  • F625W … 629.8 nm ACS/WFC

  • F775W … 769.4 nm ACS/WFC

  • F814W … 806.9 nm ACS/WFC

  • F850LP … 906.0 nm ACS/WFC

  • F105W … 1.055 μm WFC3/IR

  • F110W … 1.152 μm WFC3/IR

  • F125W … 1.248 μm WFC3/IR

  • F140W … 1.392 μm WFC3/IR

  • F160W … 1.536 μm WFC3/IR

Mag distn of multiply lensed arcs in A1689 and CL0024

Arcs in A1689 and CL0024

Will yield photometric redshifts with rms error of

~2% x(1 + z) for sources down to ~26 AB mag.


Clash c luster l ensing a nd s upernova survey with h ubble

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?

ΛCDM Theory

ΛCDM Theory

Umetsu et al. 2010

LCDM prediction from Duffy et al. 2008

  • 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


What degree of substructure exists in the dm distribution in cluster cores

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

Abell 1689 Coe et al. 2010

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

First CLASH Cluster: Abell 383


Does the equation of state of dark energy depend on time

Abell 383 SN Candidate “Caligula”

Abell 383 SN Candidate “Nero”

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

Reference Discovery Difference

Nov 18, 2010 Dec 8, 2010 Dec 28, 2010

ACS, F850LP, z ~ 0.3

WFC3-IR, F160W, z ~ 0.7 or 1.7

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.

Δ mag (vs. wo = -1, wa = 0)

MCT

MCT

CURRENT

HST LIFETIME


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

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

Zitrin et al. 2010

  • 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!

z = 4.92 Galaxy

ACS PSF

How object would look without cluster lensing

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.

0.2”


Concluding comments

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

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 SLCswith >6 passbands – new territory for science.


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