Gravitational lensing with
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)
2018/6/11 SUGAR-RUSH@Shanghai

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)• new wide-field (1.7 deg ) camera at Subaru telescope• 3-layer survey (2014-2019?)
2• The HSC 2fields are selected based on …!

– Synergy with other data sets: SDSS/BOSS, The Atacama
Cosmology Telescope CMB survey (from Chile), X-ray (XMMLSS), spectroscopic data sets!
– Spread in RA!
lim– Low dust extinction!

− Wide(1400 deg , r ~ 26, grizy)− Deep(27 deg2, rlim ~ 27, grizy+3NBs)− Ultra-Deep (3.5 deg2, rlim ~ 28, grizy+3NBs)

HSC survey progress???

• 2/3 of nights already allocatedMandelbaum, Miyatake+ PASJ 70(2018)S25

First year shear catalog• first-year shear catalog from ~1/5 of total data
• shape measurements w/ re-Gaussianization
method (Hirata & Seljak 2003)

Publ. Astron. Soc. Japan (2018) 70 (SP1), S25 (1–43)
doi: 10.1093/pasj/psx130
Advance Access Publication Date: 2017 December 23

The first-year shear catalog of the Subaru Hyper
Suprime-Cam Subaru Strategic Program Survey
Rachel MANDELBAUM,1,∗ Hironao MIYATAKE,2,3 Takashi HAMANA,4
Masamune OGURI,3,5,6 Melanie SIMET,2,7 Robert ARMSTRONG,8James BOSCH,8 Ryoma MURATA,3,6 François LANUSSE,1 Alexie LEAUTHAUD,9Jean COUPON,10 Surhud MORE,3 Masahiro TAKADA,3 Satoshi MIYAZAKI,4

Mandelbaum, Miyatake+ PASJ 70(2018)S25

2 after bright star mask
total
areaof~137
deg•Fig. 1. Map of the i-band PSF FWHM across each field. The holes in area coverage are due to masking bright stars, while the other aspects ofFig. 1. Map of the i-band PSF FWHM across each field. The holes in area coverage are due to masking bright stars, while the other aspects of thearea
coveragedetermined
as describedin subsection
2.2. (Coloronline)
area
coveragearearedetermined
as describedin subsection
2.2. (Coloronline)• mean seeing of 0.58″, neffFig. 1. Map of the i-band PSF FWHM across each field. The holes in area coverage are due to masking bright stars, while the other aspects of thFig. 1. Map of the i-band PSF FWHM across each field. The holes in area coverage are due to14masking bright stars, while the other aspects of the14
area
coveragearedetermined
as describedin
2.2. (Coloronline)
thatwillhereafter
hereafter
referred
to HECTOMAP,
assubsection
HECTOMAP,
VVDS,
limiting
magnitude
is defined
database.
thatwillbe bereferred
to asThis This
limiting
magnitude
is definedas the as
area
coverageare determined
as describedin subsection 2.2.VVDS,(Color online) database.

−2~ 22 arcmin

WIDE12H,
GAMA15H,
GAMA09H,
XMM.
magnitude
at whichthephotometry
PSF photometry
hasWIDE12H,
GAMA15H,
GAMA09H,
andandXMM.
magnitude
at which
the PSF
has S/N∼ S/N
5σ ∼14see theForthe
theweaklensing
shear
catalog,
makea number (for (forweaklensing
shear
catalog,
we wemakea numberdetails,
seeHSCthe HSCDR1 paper).
However,
details,
DR1 paper).
However,wethat For
will
hereafterbereferredtoas
HECTOMAP,VVDS,

mock catalogs which follow the same spatial distribution of galaxies as
the HSC shear catalog and includes cosmic shear from ray-tracing simulations (see Oguri et al. 2018 for more details). The χ 2 and p values forthe null hypothesis for each field are summarized in table 2.

Mandelbaum, Miyatake+ PASJ 70(2018)S25

S25-26

Null tests

Publications of the Astronomical Society of Japan (2018), Vol. 70, No. SP1↑ tangential and cross shear
aroundbrightstars
original PSF shape (as traced by star shapes) leaks into

Fig. 15. Average cross shear around SDSS CMASS galaxies acrossthe Average
entire survey
at allandredshifts.
quantitybe zeroFig. 14.
tangential
× shearThis
aroundbrightshouldstars acrossthedueto survey,
symmetry.
entiredefined as all stars with i-band magnitude ≤22.5 (andpassing other cuts as defined in subsection 4.1). We restrict ourselves
to small scales here so that we can investigate the impact of nearbystars on shear estimates, for example due to their inducing errors in sky
the galaxy shapes. First we consider the left-hand panel,background estimation.

←the tangentialandshear(11)] isstar–star correlations,wherecrossonly ξ [equationshown. These curves are fairly flat over separations of aaround random points
degree, indicating that the PSF shape exhibits slow spatial+Fig. 13. Stacked tangential (upper) and cross (lower) shear profiles

variations in the coadd. The magnitude of the curves, from

Weak lensing mass reconstruction• we want to know convergence κ (DM dist.)from shear γ (observed galaxy shape)−systematics tests from B-mode maps
−find clusters, voids, troughs, …
−cross-correlations with other maps1ˆ (~`) = ̂(~`)D̂(~`)⇡~(✓)→1
0 =⇡D̂(~`) = ⇡Z

`21

`22 + 2i`1 `2⇡2=D̂⇤ (~`)|~`|20 ~0⇤ ~~d✓ (✓ )D (✓0~✓)(Kaiser & Squires 1993)

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

MO, Miyazaki+ PASJ 70(2018)S26

WL
mass
map

galaxy
mass
map
XMM

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

MO, Miyazaki+ PASJ 70(2018)S26
Publications of the Astronomical Society of Japan (2018), Vol. 70, No. SP1

E-mode x galaxy

sum of thas"!
κl ≈WLmassmapkcorrelation
coefficient≡

B-mode x galaxysmoothing scaleFig. 9. Pearson correlation coefficients [equation (6)] between mass
maps from weak lensing and galaxy mass maps from LRGs as a function of the smoothing size θ s in equation (2). Filled squares show cross-!

Qk

where Hthe critica
approxim

galaxymass
map% (z) ≈−1
crit,lwith z̄l =lens reds
XMM

3D mass reconstruction• by using photometric redshifts, we can derive

WL mass maps for different source redshifts zs• then 3D mass reconstruction is essentiallya linear inversion problem(✓, zs,i ) =2D projectedmass dist.
<latexit sha1_base64="gaoNm62xpCLBPw17a5JfojM++6k=">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</latexit>

XjR(zs,i , zl,j )⇢(✓, zl,j )3Dmass dist.

⇢(✓, zl,j ) =<latexit sha1_base64="pl/Rsm2VqNpl9xDiQy+2zKOKBIo=">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</latexit>

X⇥iR1

⇤

ij

• 3D mass reconstruction is very noisy, thus(✓, zs,i )needs efficient filtering using e.g., Wiener filter(e.g., Hu & Keeton 2003)

MO, Miyazaki+ PASJ 70(2018)S26

Largest 3D mass map ever createdsee also Subaru press release: https://www.naoj.org/Pressrelease/2018/02/26/

Application of mass map: peaks• high S/N peaks of mass maps corresponds
to massive clusters of galaxies• provide a unique means of constructing ashear (mass) selected cluster sample(e.g., Wittman+2001, Miyazaki+2002, Schirmer+2007, …)• however it was difficult to construct a large
sample of mass selected clusters because
it requires both wide and deep imaging

Miyazaki, MO+ PASJ 70(2018)S27

Importance of high neff

number density ofmass map peaks with S/N>5

Publications of the Astronomical Society of Japan (2018), Vol. 70, No. SP1

peaks ashalo model prediction

DESKiDS

HSC

galaxy number density neff

Fig. 17. Expected number of significant (ν > 5) mass map peaks perS27-7

Miyazaki, MO+ PASJ 70(2018)S27

Shear selected cluster sample
Publications of the Astronomical Society of Japan (2018), Vol. 70, No. SP1

open circles:
mass mappeaks
filled circles:
optical(CAMIRA)
clusters• 65 mass map peaks with S/N>4.7(by far the largest shear-selected cluster sample)• almost all of them match optical clustersMO, Lin+ PASJ 70(2018)S20

CAMIRA HSC cluster catalogue• red-sequence cluster finder CAMIRA (MO 2014)
applied to HSC survey data
• uniform cluster catalog out to z=1.1!

richness
Fig. 6. Comoving number density of HSC Wide S16A clusters as a function of cluster redshift (solid). The Poisson error is sufficiently small,∼10% in each bin. Dotted lines show the predicted number densitiesof halos with masses M200m > 5 × 1013 h−1 M⊙ (top), 1014 h−1 M⊙(middle), and 2 × 1014 h−1 M⊙ (bottom), which are computed using aredshift

BCG spec-z

Publications of the Astronomical Society of Japan (2018), Vol. 70, No. SP1

S20-8

cluster photo-z

Miyazaki, MO+ PASJ 70(2018)S27

Shear selected clusters

Publications of the Astronomical Society of Japan (2018), Vol. 70, No. SP1

cluster masscompletenesscomputed byhalo modelcluster redshift
Fig. 9. Completeness of shear-selected clusters (ν > 4.7) estimated fromthe analytic model, assuming the WMAP9 cosmology (solid line contour) in the M500 –z plane [equation (A9)]. The filled circles show the• well-defined selection function is advantage!

Fig. 10. Redshift distributio
histograms show the obmatch CAMIRA only andMiyazaki, MO+ PASJ 70(2018)S27

X-ray underluminous?

• stacked RASS X-ray images of shear selectedversus X-ray clusters w/ similar masses
70, No. clusters
SP1S27-16• factor of 2 difference in average X-ray luminosity!

shear-selected clustersX-ray clusters

Fig. 13. Stacked 0.5–2.0 keV RASS images of shear-selected clusters (leftOther HSC lensing results• weak lensing mass measurements of SZ clusters
to calibrate hydrostatic mass bias
(Medezinski+2018, Miyatake+2018)[see Hironao Miyatake’s talk on Wednesday!]• discovery of many strong lenses(Tanaka+2016, Chan+2016, More+2017, Sonnenfeld+2018a)• combining weak and strong lensing analysis(Sonnenfeld+2018b)[see Alessandro Sonnenfeld’s talk on Friday!]Hikage, MO+ in prep.

Coming soon: cosmic shear• analysis in Fourier space w/ pseudo-Cl method(see Hikage+2011, Hikage & MO 2016)• cosmology-dependent covariance• accuracy of Cl measurement and covariancetested against realistic mock shear catalogs• B-model Cl consistent with zero, and best-fit
2
χ of E-mode Cl fully acceptable• analysis blinded both catalog and analysis level

Hikage, MO+ in prep.

Coming soon: cosmic shear

blications of the Astronomical Society of Japan, (2014), Vol. 00, No. 015(normalization blinded)

4-bin tomography
marginalize overphoto-z error, IA,PSF residual error
4% constraint on
S8=σ8(Ωm/0.3)0.45

Summary• HSC survey is an ideal survey for lensing!
• its high galaxy number density allows us toreconstruct high-resolution mass maps,
crucial for finding clusters by lensing• a large sample of purely mass selectedcluster sample sheds new light on clusters• cosmological constraints coming soon!