C luster L ensing A nd S upernova survey with H ubble ACS Parallels WFC3 Parallels 6 arcmin 22 Mpc z05 Footprints of HST Cameras ACS FOV in yellow WFC3IR FOV in red ID: 186535
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Slide1
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 radii
524 orbits, 25 clusters, 16 filters,
~3 years
M. Postman, P.I.,
with 34 co-investigators (18 institutions, 10 countries) Slide2
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
T
x
> 5
keV
z_med
~ 0.4Slide3
CLASH:
16 Passbands per cluster from UV to NIRMag distn of multiply lensed arcs in A1689 and CL0024Will yield photometric redshifts with rms error of ~2% x (1 + z) for sources down to ~26 AB mag.
Spectroscopic
redshifts
Photometric
redshifts
Why
16
filters?
Arcs in A1689 and CL0024
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/IRF140W … 1.392
μm
WFC3/IR
F160W … 1.536 μm
WFC3/IRSlide4
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
ΛCDM Theory
ΛCDM Theory
LCDM prediction from Duffy et al. 2008
Umetsu
et al. 2010Slide5
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.Slide6
First CLASH Cluster: Abell 383Slide7
Does the Equation of State of Dark Energy Depend on Time?
Reference Discovery DifferenceNov 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
MCT
MCT
Δ
mag (
vs.
w
o
= -1,
w
a
= 0)
E
xpect 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.Slide8
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 PSF
z = 4.92 Galaxy
How object would look without cluster lensingSlide9
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/CLASHSlide10Slide11
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 CoeCLASH 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.