Clusters of galaxies in Subaru
Hyper Suprime-Cam survey
Survey webpage: http://hsc.mtk.nao.ac.jp/ssp/
Public data release: https://hsc-release.mtk.nao.ac.jp/doc/

Masamune Oguri(University of Tokyo)
2017/6/16 Galaxy evolution across time@ParisPI: Satoshi Miyazaki (NAOJ)

Hyper Suprime-Cam(HSC)
HSC Survey Fields
HSC-D

R.A.

HSC-W

DEC

HSC-D

HSC-D/UD
Galactic Extinction E(B-V)• The HSC fields are selected based on …!

2)with–Synergy
other data sets:Atacama
newwide-field(1.7degcamera
atSDSS/BOSS,SubaruThetelescope•
Cosmology Telescope CMB survey (from Chile), X-ray (XMM(first light in 2013) LSS), spectroscopic data sets!

for imaging survey (HSC-SSP)• 300 nights awarded• three-layer survey from 2014 to 2019?
– Spread in RA!
– Low dust extinction!

HSC-SSP: ``Eiffel-tower’’-type survey
UltraDeep(3.5 deg2, rlim ~ 28, grizy+3NBs)

Deep(27 deg2, rlim ~ 27, grizy+3NBs)

Wide2(1400 deg , rlim ~ 26, grizy)

https://hsc-release.mtk.nao.ac.jp/doc/

Public data release
Fist public releaseon 2017 Feb 28,2
containing ~100 deg
images with full color(Aihara+ 1702.08449)

SQL server + very
nice image browser(hscMap)
Please use it!

Oguri MNRAS 444(2014)147

Optical cluster finder: CAMIRA• “red-sequence” cluster finder with arbitrary
set of filters• fit all photometric galaxies with SPS model(BC03) to derive likelihood of being cluster
members as a function of redshift• construct a 3D richness map to find clusters
as peaks in the map• successfully applied to SDSS DR8 to produce
a catalog of ~70,000 clusters at 0.1<z<0.6(available at: http://www.slac.stanford.edu/~oguri/cluster/ )The power of HSC survey
HSC WideDES SV (Rykoff et al.)SDSSall members(>0.2L*) out
to z~1.1!

Oguri et al., arXiv:1701.00818

CAMIRA HSC cluster catalogue• clusters frominternal releaseof HSC data(S16A) covering2~232 degOguri et al., arXiv:1701.00818

redshift• 1921 clusters with

N>15 at 0.1<zcl<1.1• very good photo-z!

cluster spec-zrichness

CAMIRA HSC cluster catalogue

cluster photo-z

N=64.7 z=0.812

N=43.6 z=1.074

Future extension?

• pushing the redshift limit to z~1.4(work in progress)

rich clusterat z~1.3

1Publications of the Astronomical Society of Japan, (2014), Vol. 00, No. 0

ple of clusteslight decrea
trinsic scatte
faint end, theof the photo
however, thesic scatter, w
z=0.33
photometric

Cluster galaxy evolution studies
Publications of the Astronomical Society Publicationsof Japan, (2014),
00, No. 0 Society of Japan, (2014), Vol. 00, No. 0of theVol.
Astronomicalfield

0.2 < z < 0.520.2 < z < 0.5

0.2 < z < 0.5cluster

0.2 < z < 0.5

0.5
0.2 < z < 0.5

0.2 < z < 0.5

10Nmem = [10,25]-1Field

NmemField= [10,25]

0.5 < z < 0.8-2

0.5 < z < 0.8log10(SFR) [M yr-1]

0.5 < z < 0.8

Nmem = [>25][>25]
NN
mem= =[10,25]
mem

Nmem = [>25]

0.5 < z < 0.8

0.8
0.5 < z < 0.8

0.5 < z < 0.8

10-1
Field

Nmem = [10,25]
NmemField= [10,25]

0.8-2< z < 1.1

0.8 < z < 1.1

0.8 < z < 1.1

Nmem = [>25][>25]
NN
mem= =[10,25]
mem

Nmem = [>25]

0.8 < z < 1.1

1.1
0.8 < z < 1.1z=0.85

0.8 < z < 1.1

10-1
Field

NmemField= [10,25]-2108119810

Nmem = [10,25]

NN
[>25]
mem
mem= =[10,25]

9101189118
910
1111log10(Stellar Mass) [M*/M]
log10(Stellar Mass) [M*/M]
log10(Stellar Mass) [M*/M]

Nmem = [>25]10812

Nmem = [>25]
91112101112evolutionof M*-SFR
stackedcolor-magFig. 3. Color-magnitude
diagrams (CMDs) thatare derived
by stacking pho-diagram
tometricgalaxies
over all CAMIRA clusters. (Nishizawa+Foreground and backgroundrelation(Jian+1704.06219)
submitted)

e color-coded number densities of stacked galaxies for the SFR-M∗ relation in three redshift ranges from [0.2,0.5], [0.5, 08] to
1.
The images
show galaxies
the color-codednumber∗ densities
stackedgalaxies
for fromthe SFR-M
in threeredshift ranges from [0.2,0.5], [0.5, 08] todensitiesof stacked
for the SFR-M
relation inofthree
redshiftranges[0.2,0.5],[0.5, 08]to∗ relatione bottom) and in three different environments, including the field (left), groups (middle), and clusters (right), respectively. The(fromenvironments,
the top to the includingbottom) andthreedifferent
the fieldrespectively.
(left), groupsThe(middle), and clusters (right), respectively. The
e 1.1]
different
the infield(left),
groupsenvironments,(middle), and including
clusters (right),
proportional
tothenumbercountsineachcellnormalizedbythecellwith
themaximum
count.
The
diagonallines
the lines represent thermber
scalecounts
in the color-bar
is proportional
to the cellnumber
in eachcount.
cell normalized
by thecellrepresent
with the maximum
count.represent
The diagonalin each cellnormalized bywith counts
the maximum
The diagonallines
ther-formingand quiescentpopulations.
They are sSFR
= 10.1They
in 0.2are< z < 0.5,
10. inin0.2
0.5<<zz<<0.5,0.8,10.
andin 9.9z <and1.1,
ndaries
to separating
and quiescent= 10.1
0.5in<0.8
z <<0.8,9.9 in 0.8 < z < 1.1,
nt populations.
They star-forming
are sSFR = 10.1
in 0.2 < zpopulations.
< 0.5, 10. in
0.5 < zsSFR< 0.8,
and 9.9
in 0.8 < z < 1.1,
lines witherror-bars,
estimatedusing
thefromjack-knife
resamplingeight
sub-samples,
the atmedian values
SFRs
at values of SFRs atectively.
Thewhitelines witherror-bars,
estimatedusing the fromjack-knife
resampling
fromdenoteeight
sub-samples,
denoteofthe
medianestimatedusing
thesolid
jack-knife
resamplingeight sub-samples,
denotethemedian valuesof SFRs
can qualitatively learn the redshift evolution of galaxies in three distinct environments, and at the same redshift, the differences ofgalaxies are subtracted statistically (see the text for details). Left panels

Other exciting (galaxy) results• Hα/[OIII]/[OII] emitting galaxies from NB imaging(Hayashi+, Koyama+)• quasars at z~4-7 (Matsuoka+, Akiyama+)• LBGs at z~4-7 (Ono+), LAEs at z=5.7/6.6 (Shibuya+)• strong lensing (Sonnenfeld+)• weak lensing is ready (Mandelbaum+, Oguri+)• and many others.... keep an eye on arXiv!

Summary• HSC-SSP survey is ongoing and first publicdata release was made in 2017 Feblim~26•• a lot of science results including galaxy and2
already >200 deg in grizy with rcluster studies• reliable optical cluster selection out to z~1and beyond