Optical surveys of clusters ofgalaxies
Masamune Oguri(Center for Frontier Science, Chiba U.)

2022/4/26 Galaxy Cluster 2022@STScI䛾୧᪉䛾䝕
dirty-map 䝃䜲䝗䝻䞊
䛔䜛䛜䚸୰䜜䛶SZ䛾䛶䜛䚹

dirty map

Searching for cluster of galaxies
12m+7mdeconvolved map
Kitayama+2016

Suzakugalaxytraditional

X-ray

SZ

 Multi-Sca
deconvolv
weak lensing5”䛾ศゎ⬟

new䛾୧᪉䛾䝕dirty-map 䝃䜲䝗䝻䞊
䛔䜛䛜䚸୰
䜜䛶SZ䛾
䛶䜛䚹

dirty map

Searching for cluster of galaxies
12m+7mdeconvolved map
Kitayama+2016

SuzakugalaxyX-ray

SZ

traditional Multi-Scadeconvolv
weak lensing5”䛾ศゎ⬟

newtoday’s talk
(optical surveys)

Cluster samples: history
number105
104

galaxyX-ray
SZ
weak lensing
Abell58

Wen15
redMaPPer
maxBCG
Abell89

CODEX
ACT

MCXC
Planck15
SPT
REFLEXHSC-Y3BCS
Planck11
EMSS

1000
100

HSC-Y1

1960

1980

2000

2020yearGalaxy-selected clusters
SDSS(Wen+)

all sky>1014M⊙/h

HSC S21A(MO+)
MaDCoWS(Gonzalez+)X-ray-selected clusters

eRASS[extrapolatedfrom eFEDS]

all sky>1014M⊙/hSZ-selected clusters

PlanckSZ

all sky>1014M⊙/h

ACT(Hilton+)

SPT(Bocquet+)Weak-lensing-selected clusters
all sky>1014M⊙/hHSC-Y3 (MO+)

Future prospect
number105

galaxyX-ray
SZ
weak lensing

eROSITA

EuclidLSST
CMB-S4104

Euclid
LSST

1000
100
1980

2000

2020yearalso talks by Yen-Ting Lin
and Michael Strauss

Subaru HSC-SSP survey• one of stage-III dark energy surveys

KiDS (2012-2019) DES (2013-2019) HSC (2014-2021)
1500 deg2, rlim~25 5000 deg2, rlim~25 1400 deg2, rlim~26

MO MNRAS 444(2014)147; MO, Lin+ PASJ 70(2018)S20richness

CAMIRA cluster finding algorithm

cluster photo-z

red-sequence(find cluster, photo-z)

1921 optical clusters
at 0.1<z<1.1
from HSC-SSP Y1(~200 deg2)

Latest HSC-SSP cluster catalog
richness

BCG spec-z(~1090 deg2)

cluster photo-z

10281 optical clusters
at 0.1<z<1.38

cluster photo-z

photo-z accuracyσz/(1+z)~0.01

wide range of applications!

cend dlnln 3D2D/d/dlnln
rR

0.5
0.5
001
12260.5
0.5

r [h Mpc]

Galaxies
Emulator

R200m

001122445
60.5
13 50.5 R [h1 1Mpc] 3r [h 1Mpc]

cend ln 2D/d ln R

100

100.1
10.010.1

1
3 5
R [h1 11Mpc] 3

Galaxies
Emulator

R200m

0.50.5r [h Mpc]

300112260.5
1
3 50.5 R [h1 1Mpc] 3

r [h 1Mpc]

100

100

100.1
10.01
0.1

Galaxies
Emulator

R200m

0.5
1
3 50.5R [h 111Mpc] 3

r [h Mpc]

34451001
3 5
R [h1 11Mpc] 3001122r [h 1Mpc]

r [h Mpc]

33
44560.5
1
3 50.5 R [h1 1Mpc] 3• detection at highest-z!
• consistent w/ theoretical prediction
100[h 115Mpc]
0.7 < zcl R< 1.0,< N < 200
1Mpc]
0.4 < zcl R< [h0.7, 15< N < 200
1gobs
3 (R) 3g (r) [h2DMpc ]

0.01
0.1

1
3 5
R [h1 11Mpc] 3

33
44
5

10.5
1
3 5
high-z1100cend dlnln 3D2D/d/dlnln
rRobs
3 (R) 3]g (r) [h2DMpc

R200m

1
3 5
mid-z

Mpc]
0.1 < zclR< [h0.4, 15< N < 200
1100.1

Emulator0.51100

0.01
0.1

Emulator

13 5
low-z

0.1 < zclR<[h1.0, Mpc]
15 < N < 200
11Galaxies
Emulator

233
Publications of the Astronomical Society of Japan, (2014), Vol. 00, No. 0
44Galaxies
Galaxies

0.5

1

100.1

42obs
(R)
2D(r) [h3Mpc 3]

1allz3 5

3obs
3 (R) 32D(r)[hMpc ]gGalaxies
Emulator

2cend dlnln 3D2D/d/dlnln
rR

40.5

cluster-gal 2PCF

Murata, Sunayama,1 MO+ PASJ 72(2020)64
1Splashback radius

30cend dlnln 3D2D/d/dlnln
rR

10cen
d ln 2D/d ln R

1cen
d ln 2D/d ln Rcend ln 2D/d ln R0210slope

0100Galaxies
Emulator

0.5
13 50.5R [h 11Mpc] 3

r [h 1Mpc]) [h Mpc ]33) [h3Mpc 3]) [h3Mpc 3]) [h3Mpc 3]

Fig. 1: In the top row, we show observed projected cross-correlation measurements between the clusters and galaxies (points with10101010error bars in red color) from left to right, for the Full, Low-z , Mid-z , and High-z cluster samples from Table 3 with the fiducial
absolute
colored regions show(cf.
the 16thMore+2016)
1 magnitude cut Mz 5log10 h <1 18.8 for galaxy selections. Shaded
1
1 and 84th percentiles ofthe model predictions from the MCMC chains for each cluster sample. The dashed profile curves in the top row show contributions

Public release• CAMIRA cluster catalog in HSC-SSP PDR3(~800 deg2) was released in 2022 Marchhttps://hsc-release.mtk.nao.ac.jp/doc/index.php/camira-cluster-catalog__pdr3/• if you are interested in a large homogenous
cluster catalog out to z~1, please check!

(e.g., poster by Roohi Dalal for BCG study w/ CAMIRA)WL mass map

bars: observed galaxy distorsion (shear)color: reconstructed mass map(e.g., Kaiser & Squires 1993; Schneider 1996; …)

WL selected clusters

clusters from peaks in mass map[purely gravitational selection!]Miyazaki, MO+ PASJ 70(2018)S27

number density of peaks (clusters)

Depth is importanthigh ngal
HSCDES, KiDS

high resolutionof mass maps

galaxy number densityChallenge: deep and wide imaging≲ 10 clusters

beforeHSC-SSPMO, Miyazaki+ PASJ 73(2021)817

Three year WL selected clustersMO, Miyazaki+ PASJ 73(2021)817

Three year
WL
selectedclusters
Publications of the Astronomical Society of Japan, (20TI05mass
M500c [h 1M ]10418 clusters

15withS/N > 4.7

1014

1013

significantly large
sample forstatistical studies!
0.2

0.4

0.6
0.8
zcl redshift

1.0

1.2

ear-selected clusters in the TG15 (left), TI05 (middle), and TI20 (right) catalogs. Redurface density profile fitting. Blue open circles indicate clusters that are matched with theWL selected clusters
HSC Y5 (?)
HSC Y3HSC Y1

Applications• clean and well-understood selection function
enables accurate cluster cosmology(talk by Kai-Feng Chen)• testing selection effects of X-ray (eROSITA)
selected clusters, and searching for X-ray
underluminous clusters(talk by Miriam Ramos-Ceja)Summary• unique samples of clusters from HSC-SSP!
• CAMIRA algorithm provides a large
homogeneous sample of galaxy-selectedclusters out to z~1• HSC-SSP begins to provide a significant
sample of weak lensing shear-selectedclusters