すばる広天域銀河サーベイによる基礎物理（fundamental physics)の探求（に向けて）

Masahiro Takada

素粒子物理学の進展＠京都大学, 2017年8月

Fundamental physics
with cosmology• Dark energy & Cosmic acceleration• Neutrino mass
• The nature of dark matter• Light relics (new particles beyond SM)• The nature of primordial perturbations (theinitial conditions of the Universe)2CMB success: the triumph of physics!
6000

Based on linear perturbation
theory of structure formation(e.g., Kodama & Sasaki 87)

D`T T [µK2 ]

5000
4000
3000
2000
1000

D`T T0600

60300-30-603000-300-600
210305001000

`

1500

20002500

ΛCDM standard cosmological model
0.05%!

5.6σ!

(late-time) cosmology is easy!
Modern Cosmology (AcademicPress)
Scott Dodelson
This textbook is enough tounderstand the basics ofstructure formation
Will become ready to startresearch
Also see for cosmology/particle
physics contents
arXiv:1503.08043, 1610.02743,1703.00894, ...

5

CMB (~2D) vs. Galaxy Surveys (3D)kpri

CMB (width ~ 5Mpc)

VCMB

⇠⇠

4⇡fsky (14 Gpc)2 ⇥ (0.005 Gpc)
7 (Gpc/h)3

VPFS ⇠ 9 (Gpc/h)3 (fsky 0.04)
Tegmark & Zaldarriaga 09

A huge 3D volume is stillavailable for cosmology

Large-scale structure formation: ΛCDM model
Structure formation = Time evolution of matter
inhomogeneities of each scale (wavelength)¨m + 2H ˙mCMB ⇒initial conditions

time4⇡G¯⇢m m = 0gravity (dark matter)cosmic expansion (dark energy)

Galaxy survey ⇒ large-scale structure
A result of gravitational instability

Structure formation:Expansion vs. Dark matterw/o ΛSCDMwith ΛLCDM

Jenkins+99
Similar CMB spectra in these two models

σ8 tension? New physics?
σ8: the present-day rms of mass density fluctuations of 8 Mpc/h scale
Planck σ8 value: extrapolated of fluctuations from z~1100 assuming ΛCDM
KiDS-450
CFHTLenS (MID J16)
WMAP9+ACT+SPT
Planck15

1.2

8

1.0

• Planck value is notconsistent with theresults of LSS probes(e.g. weak lensing)

0.8

0.6

Hildebrandt et al. 16
0.16

0.24

0.32

0.40

⌦m

KiDS: the Kilo-Degree Survey (Leiden, …)
9σ8 tension? New physics?
fitting formula (Hu & Jain 04)
8 ⇡⇣5.59 ⇥ 10 5✓2

⌦b h0.024◆ 1/3 ✓2

⌦m h
0.14

where◆0.563(3.123h)G0 ⇡ 0.76✓⌦m0.27(ns 1)/2

◆0.236✓h0.72◆0.693

G00.76

4/3

F [⌦de (1 + wde )]F (x) = (1 + 0.498x + 4.88x3 ) 1• σ8 can be accurately computed in linear theory oncethe cosmological model is fixed• Which physics can lower σ8? – New physics?
– Dark energy (wde>-1)– Neutrino mass (e.g, 0.1eV neutrino mass can reconcile)– Modified gravity????
10Galaxy survey; imaging vs. spectroscopy
Imaging• Find objects– Stars, galaxies, galaxy clusters• Measure the image shape of eachobject → weak gravitational lensing• For cosmology purpose– Pros: many galaxies, areconstruction of dark matter
distribution– Cons: 2D information, limited
redshift info. (photo-z at best)Spectroscopy• Measure the photon-energy
spectrum of target object• Distance to the object can be
known → 3D clustering analysis• For cosmology– Pros: more fluctuation modes in 3D
than in 2D– Cons: need the pre-imaging data fortargeting; observationally more
expensive (or less galaxies)

Subaru Telescope

Prime-Focus Instrument

Subaru Telescope(NAOJ)@ summit of Mt. Mauna Kea (4200m), Big Island, Hawaii

SuMIRe = Subaru Measurement ofImages and Redshifts
H. Murayama (Kavli IPMU Director)l

IPMU director Hitoshi Murayama funded(~$32M) by the Cabinet in Mar 2009, as oneof the stimulus package programsl

Build wide-field camera (Hyper Suprime-Cam;~$55M) and wide-field multi-object
spectrograph (Prime Focus Spectrograph;~$80M) for the Subaru Telescope (8.2m)

lExplore the fate of our Universe: dark matter,dark energyl

Keep the Subaru Telescope a world-leading
telescope in the TMT eralPrecise images of 1B galaxieslMeasure distances of ~4M galaxiesl

Do SDSS-like survey at z>1

Subaru (NAOJ)

HSCPFSImaging + Spectroscopy (1.5M gals for 2.5m SDSS)

Distant (faint) universe = The universe in the past

HSC+PFS can probe the 3D Universe at z~1!

A journey through simulated universe (Millennium Simulation)

Subaru SuMIRe16

Wide-area galaxy survey

DESI (4m, LBL, 2019-)

SuMIRe (2015-25)

Euclid (ESA, 2022-)

WFIRST (NASA, 2025-)
LSST (6.5m, SLAC, 2022-)

宇宙物理と素粒子物理の融合領域。2030年までは様々な展開・発展が約束。そのなかで
日本SuMIReが先陣を切る
17

Time line (DE experiments)
2020

2019

2018

2017

2016

2015

2014

2013

BAO

2012

2011
WL

Subaru HSC
DESLSST(2020-)?
SDSS/BOSS

Euclid (ESA, 2022-)
Subaru PFS
DESI(LBL+)WFIRST(NASA 2025-)?
We are in a good position!

Hyper Suprime-Cam (HSC)• largest camera• 3m high• weigh 3 ton• 104 CCDs(~0.9B pixels)• Japan, Taiwan andPrinceton

Subaru Telescope:
wide FoV&excellent
imagequality
Hyper Suprime-Cam FoV• Fast, Wide, Deep & Sharp• a cosmological survey needs theseHSTThe current SprimeCam image (M. Oguri)
Galaxy cluster~50,000 galaxy images

HSC Collaboration

International collaboration (Japan, Taiwan, Princeton U.)

HSC Survey Fields
HSC-D

R.A.

HSC-W

DEC

HSC-D/UD
Galactic Extinction E(B-V)• Subaru 300 nights granted (2014 – 19)• HSC Survey Fields selected based on– Overlap with SDSS regions and other interesting, external datasets(ACT CMB, NIR, spectroscopic surveys, …); Low dust extinction;
Spread in RA• The main scientific objectives are– Wide: Cosmology, Deep: galaxy evolution, UD: cosmic reionization

22

First Data Release (DR1) of HSC SSP
28 Feb, 2017
~60 Subaru nights, ~100 sq. deg., ~108 objects ≃10yrs SDSSNearby galaxies

upper: HSC (8.2m)
lower: SDSS (2.5m)

1’’
All data reduced by the HSC pipeline

A. Leauthaud S. Huang

Galaxy Clusters
M. Oguri

SDSS (2.5m, r<21, ~1’’)

Subaru HSC (8.2m, r<26, 0.6’’)~2Mpc

the same rich cluster region at z=0.41

Gravitational lensing = GRprediction
8π GGµν = 4 Tµνc
⇒ light path: x = x[z; gµν ]Light-ray path, emitted from a distant galaxy, isbent by the foreground matter distribution
It causes a distortion in galaxy image
Cosmic acceleration (DE)

Dark matterdistorted galaxy shapes

Weak lensing effect• Extract coherent distortion
pattern in different galaxy images• Need to analyze many galaxy
images to extract the signal• All galaxies lensed more or less
• Tiny signal: O(0.01) in ellipticity• A sharp image/an accurate
methodWeak lensing
The signal is tiny: allows for a direct reconstruction of gravitational
potential due to Z
nonlinear matter distribution in the universe
zsshearij ⇠0dzl W (zs , zl )r?i r?j [xphoton path (t)]r2 (x, t) = 4⇡G¯
⇢m a2 m (x, t)

Simulatedlensing map(color = 2DDM map,stick=shear)lensing mode
(E mode)non-lensing
mode (e.g.,systematics)(B mode)28

Subaru HSC weak lensing WG

Team members in Japan (2008-)••••••••••••••••

red=PD
blue=student

Satoshi Miyazaki (NAOJ)
Masahiro Takada (Kavli IPMU)
Takashi Hamana (NAOJ)
Masamune Oguri (U Tokyo/IPMU)
Surhud More (IPMU)
Miyatake Hironao (JPL/Caltech/IPMU)
Atsushi Nishizawa (IPMU⇒Nagoya)
Chiaki Hikage (IPMU)
Ryoma Murata (IPMU)
Takahiro Nishimichi (IPMU)
Masato Shirasaki (NAOJ)
Yuki Okura (RIKEN)
Nobu Okabe (IPMU⇒Hiroshima)
Ryuiichi Takahashi (Hirosaki)
Yousuke Utsumi (Hiroshima)….

29

Galaxy shape catalog now fixed(after 3 years work)!
About 1/10 data of the full 5-year data
R. Mandelbaum(CMU)

H. Miyatake(JPL/Caltech/IPMU)

galaxy shape30

Subaru HSC = superb image quality
HECTOMAP

VVDS
2◦ 00’
0.9

1◦ 30’Dec [deg]43◦ 30’00’
42◦ 30’00’
0◦ 30’00’-0◦ 30’

248◦

246◦

244◦

242◦
RA [deg]

240◦

238◦

WIDE12H336◦
RA [deg]

334◦

332◦
0.8

GAMA15H

1◦ 00’

1◦ 00’

0◦ 30’

0◦ 30’Dec [deg]

Dec [deg]

338◦

340◦

00’-0◦ 30’◦-1 00’00’
0.7-0◦ 30’◦-1 00’
30’30’
182◦

180◦
RA [deg]

178◦

176◦

225◦

220◦

215◦
RA [deg]

Subaru HSC typically 0.6” seeing FWHM (spatial resolution)
GAMA09H

XMM-2◦ 00’

4◦-3◦ 00’2◦

Dec [deg]

Dec [deg]

0.6

0.5-4◦ 00’-5◦ 00’0◦0.4-6◦ 00’
140◦

135◦
RA [deg]

130◦

38◦

36◦

34◦
RA [deg]

32◦

30◦

compared with the Dark Energy Survey (DES; Fermilab): ~1”

seeing [arcsec]

Dec [deg]

44◦ 00’WL becoming experimental physics• Performed image simulationsof galaxies based on theHubble space data, fully
taking into account the HSC
data properties (pixel, seeing,noise, …)• Use the image simulations toestimate calibration factors forthe shape measurements

32

Null tests (tests of systematic errors)
So far no major residual systematics

33

WL mass (dark matter) maps

Z zsdzl W (zs , zl )r?i r?j [x(t)] !
ij ⇠2D0◦−02.00⇠ r 1 r 1 ij ! ⌃2Dm (✓)
4.0

Map of projected mass density

3.2

Dec (J2000)−03.00◦2.4
1.6−04.00◦0.8−05.00◦Masamune Oguri−0.8(Tokyo/IPMU)
0.0−06.00◦38.00◦−02.00◦36.00◦

34.00◦RA (J2000)

32.00◦

30.00◦

Map of projected galaxy distribution−1.6
0.00080.0007

arXiv:1705.06792
0.0005Oguri et al.
0.0006

Dec (J2000)−03.00◦0.0004◦−04.000.00030.0002−05.00◦0.00010.0000−0.0001−06.00◦38.00◦

36.00◦

34.00◦

32.00◦

30.00◦−0.000234

3D mass map
Combining thegalaxy shapes andphotometric redshiftof each galaxy(approximate
distance measure),
we can recover the
3D distribution ofmatter
Mass and galaxy
maps show a nicecorrespondence35

~1.3 deg
HSC (~20 gals/arcmin2, ~0.6”) DES-like (~7 gals/arcmin2,~1”) 36

Galaxy(cluster)-shear lensing• HSC SSP survey regions have a full overlap with
the SDSS spectroscopic survey fields (=bright,massive galaxies)• Measure a coherent tangential shear pattern ofbackground galaxies, around each SDSS galaxy⇒ can probe the average mass distribution
around the galaxies

background gals

halo

Subaru data
spec. gal

SDSS spec. galaxy37

y-axis value is blinded

HSC galaxy-galaxy lensing

for the first time

~8000 SDSS lens gals
~10M HSC source gals

• The average,
projected massdensity profilearound galaxies• Clearly show theexistence of DM
around brightgalaxies• The superior HSC
data allows for adetection of very
tiny signal up to~100Mpc• Large-scale signal= clean (more inthe linear regime)

Radius from the lensing galaxy38

Challenges in WL cosmology• Residual systematic errors in shape measurements 😄
• Blending in galaxies in deep Subaru data 😵
• Uncertainties in photometric redshifts (distances tosource galaxies) 😕
• Nonlinearities in structure formation 😄
• Baryonic (astrophysical) effects on structure formation ☹
• Galaxy bias uncertainty ☹

39

Halo Emulator• 1Gpc/h or 2 Gpc/h,
Npart=20483 for eachrealization• 24 (20) realizations for Planck• 60 realizations for different
cosmologies• 21 snapshots over 0<z<1.5(stepped by growth rate)• ~200Tb (so far)
• Prost-processing (Rockstar)– Halos & subhalos– Halo center: the potential
minimum– SO mass. Every member DM
particle belongs to one halo
(avoid double counting)Nishimichi et al. in prep.

Latin Hypercube Design!b : ±5%,!c : ±10%,ln(1010 As ) : ±20%,⌦de : ±20%

ns : 5%,wDE : ±20%dn
⇠m (r; z),, ⇠hm (r; z, M ), ⇠hh (r; z, M1 , M2 )dM⌃(R; z, M ), ⌃(R; z, M ), whh (R; z, M1 , M2 ), · · ·as a function of cosmological model,redshift, mass, separation, ….

Developing the python
package for Halo Emulator
41Murata et al. 17Emulator can reproduce the measurements⌃(R) [h M /comoving pc2 ] 30

10111014
1hM200m, 20 100i = 1.91+0.05
0.05 ⇥ 10 h M
1500.211050

R [h 1 comoving Mpc]

 55

55 100

101shaded = MCMC 68 percentile 100abundance(number ofclusters in eachrichness bin)

10000080000⇥N⌃(R) [h M /comoving pc2 ]8,312 clusters
39M galaxy shapes

14
1hM200mi = 2.04+0.06
0.06 ⇥ 10 h M⌃(R) [h M /comoving pc2 ]40 Planck cosmology

10R [h 1 comoving Mpc]

100

 40

2min /dof = 79.5/75

14
1hM200mi = 1.38+0.04
0.04 ⇥ 10 h M

0.230 100⌃(R) [h M /comoving pc2 ]

20 

100

1060000

40000
12000014
1hM200mi = 3.00+0.110.13 ⇥ 10 h M

0.2

1101

R [h comoving Mpc]

141
hM200mi = 4.56+0.16
0.17 ⇥ 10 h M

50

0.2

11050

02030

4050

60

70 80 90 100

1R [h comoving Mpc]

42

Other particle physics/cosmology science• Boundary of dark matter halo (self-interacting DM)• Dark matter annihilation: Subaru PFS measurementof dwarf galaxy, WL mass and Fermi crosscorrelation• Isocurvature perturbation• Curvature (ΩK~10-3): multiverse (string theory)• Primordial non-Gaussianity• Microlensing due to primordial black hole/cosmicstring• Axion (relic light particles)• ….
43

10 15MPBH [M ]10 10

10 5100

KeplerFemto

EROS/MACHO

CMB

10 3

BH Evaporat

10 2dense (2min)cadencedata of M31

ion

10 1f=⌦PBH/⌦DM

A mass fraction of PBHs to DM

HSC microlensing constrain
on PBH abundance

10 4
10 5 15
10HSC (95%)
tightest
boundon PBH
with MPBH=[1020,1028]g
HSC M31constraint(95% limit)
1 HSC night ⇔ 2 years Kepler data
1020

1025

MPBH [g]

1030

1035
Niikura, MT, + 17

Summary• The wide-field capability of Subaru is so unique,and very powerful for survey-oriented
astronomy/cosmology• Hyper Suprime-Cam (HSC) = Wide-field imager– HSC SSP survey: 2014 – 2019(20)– First public data release (28 Feb, 2016)• so many science cases in interdisciplinary fields
between cosmology and particle physics– Neutrino mass
– Relic light particles– Primordial perturbations