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Theoretical/Numerical predictionsfor weak lensing cluster search
Outline1. Basics of WL cluster search
2. Analytic model predictions
3. Survey power
4. Noise and scatter
5. WL & Spec, demonstrative results fromSuprime33
6. Summary
Takashi HamanaNAOJ
Miyazaki’s talk for observational aspects
1. Weak lensing survey with Hyper-Suprime is avery efficient way to locate massive clusters, ifthe seeing is less than 0.7”.
2. Weak lensing survey is complementary to X-raysurvey (Optical, SZ, as well)
3. >1/3 of high peaks on the weak lensing mass map(cluster candidates) are false signals.
4. Projection effects makes WL cluster massestimation uncertain.
5. Spectroscopic follow-up very nicely screens outfalse signals and improves the mass estimation.
Conclusions
Basics of weak lensingcluster search
Gravitational lensingUnlensed Lensed
3.0
1014
==
z
MM sun
Mass distributionof a cluster
coherent distortionin backgroundgalaxy images
Weak lensing
Weak lensing mass reconstruction
grav. potentialtidal field
(1) basics
Weak lensing mass reconstruction(1) basics
Recipes:(1) Taking imaging data(2) Object detection(3) Shape measurement(4) WL mass reconstruction
Imaging dataWL mass map
All we need for WLis imaging data
Signal & noise(1) basics
S
LSLSL
SL
D
DDzzf
zzf
=
∝
),(
),(MassSignal 1/3
<zS>
Signal = the peak height on the WL mass map
Signal & noise(1) basics
densitynumber galaxy :iesellipticitgalaxy of RMS:
/
gal
e
galelensingobs
intrinsiclensingobs
n
nee
eee
σσ+=
+=
2gal arcmin/30
4.0~)0.7"FWHM (seeingobs Cam-Suprime Typical
≥
<
neσ
Detection S/N is basicallydetermined by the number densityof the “usable galaxies” ngal
Usable galaxies(1) basics
Stars(seeing size)
usable galaxies
Not all detected galaxies areusable for weak lensing.Seeing erases the lensing signalof small galaxies (size<seeing).Only the large galaxies(size>seeing) are usable for WL.
Number of usable galaxies islimited by the seeing.Good seeing (<0.7”) is essentialfor weak lensing survey.
WL signal lost
Analytic predictions fromsimple models
Detectable clusters(2) predictions
1 arcmin/30
4.0~ parameters Obs*
profileNFW universe LCDM
:Models
2gal
==
**
S
e
znσ
Significant detection
02.0noise =σ
NOT mass selected(2) predictions
Undetectable
Weak lensing clusters areNOT “mass selected”but the “weak lensing signalselected”
The detectable minimum mass is redshift dependent
Number counts(2) predictions
function mass PS1
arcmin/30 4.0~
parameters Obs*profileNFW
universe LCDM:Models
2gal
*=
≥
**
S
e
znσ
N~5/sq deg for S/N>4N~/10sq deg for S/N>3
Survey power
WL VS X-ray(3) survey power
X-ray cluster counts
Rosati et al (2002)
])//[(NewtonXMMdeg1/10~)10(
ROSATdeg1/1~)10(
2
214
213
scmergffNfN
X
XX
XX
−‹>‹>
−
−N~5/sq deg for S/N>4N~10/sq deg for S/N>3
WL cluster counts
Exposure time
by Suprime-Cam
X-ray surveyby XMM-Newton
4 pointings to cover 1deg2
1/4 deg2 FOV each (Suprime-Cam) 9 pointings/1 deg 2(XMM-LSS design)
1 pointing 3.1 deg 2
2lim
deg1/5~)4S/N(mag26
hours21800s4
>=
=×
WLNR
2lim,
214-lim,
deg1/10~)(s/erg/cm1e
hours25ks109
XX
X
fNf
>=
=×
(3) survey power
Weak lensing surveysby Hyper-Suprime
2lim
deg1/5~)4S/N(mag26
hours5.01800s1
>=
=×
WLNR
1 cluster/2.5h 1 cluster/0.4h 1 cluster/0.03h
(1)Weak lensing survey is a very efficient way to
locate massive clusters.
Requirements:
(i) Very wide FOV camera <= Hyper-Suprime
(ii) Very good seeing condition <= Mauna-kea
(2) Weak lensing is complementary to X-ray:
X-ray misses X-ray faint massive clusters,
WL misses less massive X-ray bright clusters.
Conclusions (1)
Mock simulation with realistic noises
Completeness & contaminationof weak lensing survey
TH, Takada & Yoshida,(2004)
Lensing mass map from WL surveyHalos within 0.1<z<0.8 from N-body sim.
Large symbols: M>3e14small: 3e14>M14>8e13dots: 8e13>M14>1e13
Mock numerical simulation(4) simulation
02.0noise =σ
How many missing clusters ?
How many contaminations ?
Completeness & contamination(4) simulation
peakshigh of #
signals false of #clusters of #
clusters detected of #
Lowering the threshold S/N gives us a high completeness at aprice of a lot of contaminations (false signals). Screening out thefalse signals is key to a WL halo catalog being useful.
(1) Contaminations False signals from the random noise Projection of less massive halos
(2) Scatters in WL signal Random noise (positive or negative) Projection with structures in the same LOS (i) large-scale structures : RMS~0.01 (~0.5 x Noise RMS) unavoidable but weak effect (ii) surrounding structures: make the signal greater (in general) unavoidable a hint from a spectroscopic follow-up (iii)clusters/groups : unavoidable but very rare easily identifiable by a spectroscopic follow-up
Source of contaminants & scatter(4) simulation
*The projection effect makes WL mass estimate uncertain
somethingSignalSignal clusterobs +=
(3) A high completeness can be obtained by
lowering the threshold S/N (~3) but at a price
of a high contamination rate.
*False signals mainly arise from the noise
and partly from chance projections.
*The projection effect makes WL mass
estimate uncertain.
Conclusions (2)
How does the combinationof WL mass map and Spec. work ?
Screening out false signalsand getting better mass estimation
(4) Screening out the false signals is key to a WL
halo catalog being useful.
Spectroscopic follow-up is very important.
Requirements:
30-50 galaxies/cluster (3-5arcmin radius)
=>~1 galaxy/arcmin2
Conclusions (3)
(1)Weak lensing survey with Hyper-Suprime is a
very efficient way to locate massive clusters
(2) Weak lensing survey is complementary to
X-ray survey (Optical, SZ, as well)
(3) A high completeness can be obtained by
lowering the threshold S/N (~3) but at a price
of a high contamination rate.
(4) Spectroscopic follow-up very nicely screens
out false signals and improves the mass
estimation.
Summary
end