(観測的)宇宙論は面白い(よ)！
高田昌広(Kavli IPMU)
一昨日までスロベニアにいました@ Summer School, 2018

Science from night sky!

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

宇宙論の面白さ• 観測と理論が直結！
• ノーベル賞級（教科書に載るような）問
題、発見の可能性がある• やるなら（研究に人生を捧げるなら）、
ノーベル賞を狙いましょう！
• 勉強、経験を積みましょう！

Fundamental physics with cosmology• Dark energy or The origin of cosmic acceleration(modified gravity)• Dark matter (e.g., discovery of primordial black hole)• Light relics/particles (e.g., axison)• Non-trivial properties of primordial scalar perturbations:e.g. primordial non-Gaussianity, running spectral index,
features in the primordial power spectrum• Primordial gravitational wave
• Curvature (ΩK)
• Detection of neutrino mass
• どれか、あるいはこれらを好きになって、とことん追求してくださいCosmic microwave background (CMB)~6×106 pixels

Triumph of Physics
6000

D`T T [µK2 ]5000

Theory (linear theory)

4000

Data (measurement)

3000

Errors (meas./theory)

2000
1000

D`T T

0
600

60
30
0
-30
-60

300
0
-300
-600
2

10

30

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2500

Linear Theory: Transfer function• Consider scalar perturbations alone• Different Fourier modes evolve independently• Linearized perturbation theory: Differential equation of eachfluctuation field has a form like

The coefficients depend only on k and/or background quantities• The solution is expressed in terms of “transfer function” as+Tiso (k; ...)⇥iso (k, ⌘ini )<latexit sha1_base64="OvRVxakr+K320IyyM6WIxKLY/1s=">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</latexit>

Transfer function: the same forall the Fourier mode with

the initial condition(depends on )Public codes, CMBFast, CAMB, Class, to compute the transfer functions

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

CMB (width ~ 5Mpc)

VCMB

4⇡fsky (14 Gpc)2 ⇥ (0.005 Gpc)⇠

7 (Gpc/h)3⇠+ time evolution btw
z~1000 and z~0

VSubaru ⇠ 9 (Gpc/h)3 (fsky /0.04)<latexit sha1_base64="KeFH9KSvE8cTxVUgOFjen9lgAoc=">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</latexit>

Tegmark & Zaldarriaga 09

A huge 3D volume is stillavailable for cosmology

Formation of cosmologicalhierarchical structures
expansion vs. gravity

note: N-body sim. in physical coordinates

Background and Perturbations
Decomposition of physical quantities into background (isotropy &homogeneous) and perturbations (inhomogeneities)r = a(t)x⇢(x, t) = ⇢¯(t) [1 + (x, t)]gµ⌫ (x, t) = a(t)2 [⌘⌫µ + h⌫µ (x, t)]<latexit sha1_base64="fevQjgt73lgzIsVtW7Axrvd146E=">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</latexit>•“Comoving” coordinates: cosmic expansion is extracted and matter
stay at the same coordinates (if the universe is isotropic andhomogeneous)•Cosmological perturbation theory (Kodama & Sasaki 84)<latexit sha1_base64="fZH0dUMo++9KEIEU/p4RZXdUYPg=">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</latexit>com

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

time

4⇡G¯
⇢m m = 0

gravity (dark matter)cosmic expansion (dark energy)

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

Structure formation:
Expansion vs. Dark matter
w/o Λ

SCDM

with ΛLCDM

Jenkins+99
Similar CMB spectra in these two models

From Benedikt Diemer

佐々木節さん（IPMU) のスライドより

Constraining the scalar primordial perturbations
over many orders of magnitude scales
Bringmann+ 13

10 1

2

10

6

10

7

P (k)

10

5

❙

10

4

10 2

WIMP kinetic decoupling

10 3

❙

10 3
Allowed regions

10 4

Ultracompact minihalos (gamma rays, Fermi-LAT)

10 5

Ultracompact minihalos (reionisation, WMAP5 ⌧e )10 6

Primordial black holes

10 8

10 7

CMB, Lyman-↵, LSS and other cosmological probes

10

9

10 8

10

10

10 9
10

3

10

2

10

1

1

10 102 103 104 105 106 107 108 109 101 101 101 101 101 101 101 101 101 101
10

k (Mpc )

1

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3

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7

PR (k)

10

Subaru M31 microlensing (Niikura, MT+17)

8

9

23桁！

SuMIRe = Subaru Measurement of
Images 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 energylKeep 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)

HSC

PFS

BAO
• Measure galaxy
clustering strengths: 2pt
correlations (or P(k))

dP = n g2 [1+ ξ g (r)] dV 2

dV

r

r
~150Mpc
BAO
dV

q

DA(z)

• Find a tiny excess in thegalaxy pairs at BAO
scale (a priori known
from CMB to be~150Mpc)rBAO = DA (z)θ obs
Eisenstein et al 05

BAO=Cosmological geometrical test
• Suppose that you have an object whose size or lengthscale you a priori know – standard ruler

Redshift of center: z• The standard ruler allows us to infer the radial andangular diameter distances, from the redshift and angularextents

SDSS Baryon Oscillation Spectroscopic Survey (BOSS)

Shun Saito(MPA)• ~8σ significance for
the BAO detection⇥ ⇠ cos(ks), s ⌘

Z

d⌘ cs

19

“Super” survey mode (soft mode)• Inflation predicts all-scale
perturbations• Any cosmological survey probes a
finite volume in the universe• Nonlinear mode coupling (coupling
btw different Fourier modes)• N-body simulation is done with afinite volume (with periodic
boundary conditions)• In the late-time universe, threemight be additional perturbations(e.g. dark energy) that can’t beseen in CMBSurvey region

Super-survey modesL
short-wavelength mode
long-wavelength mode
survey region or N-body simulation box• Long-wavelength modes can be expanded around the survey region

mean density modulation

gradient field

tidal fieldSeparate universe picture
The effect of large scale mode can be absorbed by a change
in the background expansion of local universe⌦K = 0⌦K 6= 0(⇠b)<latexit sha1_base64="FpW5N8d+vq64FcNId3SGuvhVt8w=">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</latexit><latexit sha1_base64="St7gcqpM7JiOcuNNxdMN28+KyzI=">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</latexit>b<latexit sha1_base64="t4eLnmAzJjtBu/tAm21RKT1Md3w=">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</latexit>

BAO scale modified⌧ij

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Takada & Hu 13; Li+14…

ak (t)<latexit sha1_base64="GGgnYcN98fKX0PAfveqC62b8OfQ=">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</latexit>

anisotropic expansionai (t)<latexit sha1_base64="MHF5bjRIv+Uc4x4kv+tzxbxZlXY=">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</latexit>

Alignment btw halo shapes andOsato +18
surrounding tidal field
銀河団ハロー周りの平均的な質量分布（N体より）
0+<latexit sha1_base64="i7MpximWxBLx/ChZpYGWC8zg+As=">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</latexit>

Align theprincipal axis ofeach clusterscale halo to thez-axis direction,and then stackthe surrounding
mass
distribution

2.4

80

>0
60b

315

40

1.6
0.8

20
<latexit sha1_base64="RX/ZQT0c5UudUKOnvXUwGLtLLVc=">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</latexit><090
b halo center<latexit sha1_base64="RX/ZQT0c5UudUKOnvXUwGLtLLVc=">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</latexit>

b <2700

0.0

log10 ⇠hm+

BAO scale
+…
45

0.8
1.6

135

<latexit sha1_base64="i7MpximWxBLx/ChZpYGWC8zg+As=">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</latexit>

b >0
180

225

2.4
3.2

Gravitational wave (stretch of space time)transverse and quadrupoleレーザー干渉計重力波天文台 LIGO (米国）
LIGO Livingston

4km arm

LIGO Hanford

Primordial GW affects galaxy shapes?

2

ds =
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2

2

i

dt + a(t) [ ij + hij (x, t)] dx dx

Schmidt + 15

j

• halo/galaxies are from matter• stretch of spacetime is by PGWhij (k)<latexit sha1_base64="C8B1ig/umNVVg40u2TvfzmPYddw=">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</latexit>

early universe (e.g., z ~ 1000)

cdm + baryon<latexit sha1_base64="7nhmPnhc5pxzyHGAv8pBJaA0nLI=">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</latexit>

PGW ⇠ a few Gpc

a few Gyr later (e.g., z~2)

intrinsic shapes can be induced by large-scale GW

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stoch. GW ' cf

1

stoch. GW ' a few ⇥ 103km

⇠ 3 ⇥ 1010 [cm/s] ⇥ 109 [s] ⇠ 10 pc

Gravitational lensing= GR prediction
8π G
Gµν = 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 gravitational lensing (shear)“characterize” the shapeof every faint galaxy

Weak lensing
The signal is tiny: allows for a direct reconstruction of gravitational
potential due to Z
nonlinear matter distribution in the universe
zs

shear

ij ⇠

0

dzl 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)31

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

Subaru HSC Survey
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

33– Wide: Cosmology, Deep: galaxy evolution, UD: cosmic reionization

Subaru HSC = superb image quality2◦ 00’ne↵ ' 22 arcmin 2

1◦ 30’

0.9

6 fields (~140 sq. deg. in total)<latexit sha1_base64="dJww/3mJCV7P5yMc3OBiyfIR/WU=">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</latexit>

HECTOMAP

VVDS◦

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)⇔ DES: ~0.9”
GAMA09H

0.6

XMM

4

-2◦ 00’◦2◦

Dec [deg]

Dec [deg]-3◦ 00’0.5-4◦ 00’-5◦ 00’0◦

0.4-6◦ 00’140◦135◦RA [deg]

130◦

38◦

36◦

34◦
RA [deg]

32◦

30◦

seeing [arcsec]

Dec [deg]

44 00’

Mandelbaum, Miyatake+, PASJ 2018

HSC galaxy shape catalog• Developed the pipeline for galaxy
shape measurement

R. Mandelbaum Hironao Miyatake（CMU）(Nagoya/IPMU)• Tested/validated the galaxy shapecatalog with sophisticated image
simulations
solid: HSC data

• ~10M galaxies (~20 gals/sq. arcmin.,~140 sq. deg.)• Ready to use for weak lensing science
Input galaxy inimage simulation

real HSC galaxy

simulated galaxy
image with noise

dashed: image
sims.

Cosmic shear cosmology• Pros– Can measure “total” matter power
clustering
✓
◆
Z
`
2
2 NL
C` = d WGL ( )Pm k = ; z( )<latexit sha1_base64="sXDiv2DX4fMho27gqUNLjoouDCU=">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</latexit>• Cons– All the systematic errors additively
contribute the measurements (⇔ g-g
lensing)– Challenges: Photo-z errors and baryonicphysics– HSC data are very deep compared to
DES: precursor of LSST

Cosmic shear
tomography• Used photo-z’s of eachgalaxy to have 4
tomographic bins
• Used the HSC-Widedepth data of COSMOS
field for galaxies after the
WL cut to calibrate thephoto-z errors• Test the results against thedifferent photo-z catalogs

Pseudo-power spectrum estimator Ẽ`m ± iB̃`m =(Hikage, MT, Hamana, Spergel 11)<latexit sha1_base64="IxpAW9oN7k+tj/N2lSAk1INvS2o=">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</latexit>
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sha1_base64="x4nAfQh390HE1T8iL54TSupAlho=">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</latexit>Z

d2 n w(n) [ 1 (n) ± i 2 (n)] Y`m (n)ĈlEE = Mll01

Arbitrary scaled (Blinded)<latexit sha1_base64="37limAYdDXcnh9fZ6he7G7UiEpw=">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</latexit>

⇥

ClEE
0

Nl 0

137 sq. deg.
0.3<z<1.5300<ell<1900n_eff~16.5 arcmin-2

total S/N~16, corresponding
to ~3% in S_8⇤

HSC collaboration (HSC WLWG)
ブライド解析

We (HSC WLWG) unblinded
the cosmological results(catalog and analysis levels) at
the telecon of 26 June, 2018

Arbitrary scaled (Blinded)

model canreproduce themeasurements!

Challenges: Nonlinear, nonlinear, nonlinear…

• Cosmology with galaxy surveys ismore complicated than CMB (LHC
⇔ electron/positron colliders)• Complications: Galaxy bias,
nonlinear clustering, baryon …
• However, we should keep in mind
which observables are clean or
dirty; we have conservations (massand momentum)• E.g., halo bias is little affected bybaryonic physics

Towards precision cosmology:
Modeling LSS observables• Hydrodynamical simulations– unique way to model galaxy formation– still too expensive• Perturbation theoryMakino, Sasaki & Suto 92; Matsubara+; Taruya+– very accurate. The effective field theory approach forgalaxy bias (rigorous due to symmetry). The theory
errors are under control– however, breaks down at k>k_NL• Halo-based approach– easy to model (at least in N-body sims.)– use halos and their statistics for cosmology– need parameters or ways to connect halos in simulations
and galaxies (observables) in a survey• Reconstruction of initial conditions (fields)

42Perturbation theory
or Effective field theory of LSS• Effective field of theory• Goal<latexit sha1_base64="bjkZH3GL8zTS6jYE9jiQ8X6F6to=">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</latexit>

L
(k)
=
F
(k;
⌦
,
n
,
....,
p
,
M,
...;
(q) + ✏(q)hms
astrophysPT looks appealing… though
105

1.5

Desjacques, Jeong & Schmidt PRR
NLO
Pmm(k)/PL (k)NLO
Phm(k)/(b1 PL (k))

P (k)/PL (k)P (k) [Mpc3 /h3 ]

1.0

104

b r2
b2
bK 2
btd

0.5

0.0
Pmm (k)103

Phm (k)0.5

Phh (k)10 2

10 1
wavenumber k [h/Mpc]

10 1
wavenumber k [h/Mpc]• Well defined and rigorous. The theory error well controlled• Need to introduce many nuisance parameters (>7 parameters)(nonlinearities, primordial peak shapes, halo exclusion effect, etc.)• PT for “matter” clustering anyway breaks down at k≳0.15 h/Mpc (alsosee Nishizawa, Nishimichi & MT 15)

Any useful information in nonlinear regime?
Zhao, Saito, Percival+ 12: The work with BOSS data

• Various model predictions
for nonlinear galaxy
redshift-space power
spectrum• Nonlinear effects become
significant at k>0.1 h/Mpc• Some models introduce
nuisance parameters tomodel unknown effects
such as galaxy bias

Any useful information in nonlinear regime?
Zhao, Saito, Percival+ 12: The work with BOSS data
No improvement in cosmo paras by adding the information of k=[0.1,0.2],
regardless of a factor 8 more information content in P(k)Σ mν [eV]0.6P(k), kmax = 0.1 h/Mpc
CMASS BAO

1.0

P(k), kmax = 0.2 h/Mpc
CMASS BAO

0.8

L/Lmax

0.8

0.4
0.2
0.0
0.20

0.6
0.4
0.2

0.25

0.30

ΩM

0.35

0.25

0.30

ΩM

0.35

0.0
0

Halo model: DM halos ⇔ Galaxies
Dark matter

DM halosgalaxies

central & sat gals

• Galaxies (central and satellite gals) reside in dark matter halos• Clustering of dark matter halos are relatively easy to model
based on simulations and/or analytical models

Cosmology with HSC and BOSS
Nishimichi, MT in prep.

2h
1h
Pgm (k) = Pgm (k) +Pgm (k)<latexit sha1_base64="0dOkELy1K0kF0fpzkREd53ifX6w=">AAADoHicpVFLb9NAEB7XPIp5NIULEhfTKFECKFqbqCmVkCrg0Bt5kLai20ZrZ+tY8Yu1EwiW/wB/gAOnIiGE+Bkc4AgHDv0JiGORuHBg7LilPRQOrOXdme+bb2Z21ggcO4wI2ZNm5FOnz5ydPaecv3Dx0lxh/vJa6I+Eybum7/hiw2Ahd2yPdyM7cvhGIDhzDYevG8P7Kb8+5iK0fe9RNAn4lsssz96xTRYh1JuXlqnBLduL+ROPCcEmNxKlVC6rT3sxFa5qWUmlXVVpIPwg8tWKkcNJdVtXqe1F9Dp1WTQQbtxPBJIBE8xxuJOo9Jk9DXZdzHFL9A65KqVZDfqAOxGjHdty2dEq1GAClQM/yRMkh2X/p2QzT4LcsKreVZvbma8PkmOEUrp5QGnHKYVyr39kUL1CkdTuLC3q9UWV1AhpaLqWGnqjfruuaoikqwj5avqFt0ChDz6YMAIXOHgQoe0AgxC/TdCAQIDYFsSICbTsjOeQgILaEUZxjGCIDnG30NvMUQ/9NGeYqU2s4uAvUKlCiXwl78g++UTek2/k14m54ixH2ssET2Oq5UFv7sXVzs9/qlw8Ixj8Uf215wh2YCnr1cbegwxJb2FO9ePnL/c7y+1SXCavyXfsf5fskQ94A2/8w3zT4u1XoOADHExZPdlY02saqWktvbhyL3+KWbgGC1DBeTdgBVahCV0wpV3po/RZ+iIvyKvyQ7k1DZ2Rcs0VOLbkx78ByFz8AA==</latexit>from Halo Emulator (Takahiro’s talk)<latexit sha1_base64="Ua/WtQW87vElJTFsRQInpVDA4Hg=">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</latexit>

many nuisance parameters(~10) to connect galaxies
and halos<latexit sha1_base64="74/6PVoWuFy1H9JuToavmABrIDE=">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</latexit>

✓
T
T

◆2
2
⇠ D`2 /TCMB= `(` + 1)C` /2⇡

クイズ✓<latexit sha1_base64="wlLGtn3G5li2yLhxu2yE9LcjGpo=">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</latexit>

TT◆2⇠ ⇣ 2 ! ⇣ ⇠ 10 5

なぜhigh-multipoleの温度ゆらぎは増幅されているの？

最近の素朴な疑問• 晴れ上がり前には陽子、電子、ヘリウムはなぜ一緒に運動するのかな？
• 晴れ上がり後は残存電子、水素、ヘリウムは一緒に運動するのかな？
• 1億年後、100億年後のCMBの空はどのようにに見えるのかな？（今のCMBマップと違う？）• ニュートリノ背景放射の角度異方性スペクトルはどんな形？
• 陽子-電子散乱、電子-陽電子散乱、電子-電子散乱の電磁放射は違うのかな？
• 重力波が伝播しても物差しも一緒に伸びるから、息子の身長は同じように見えるのかな？
• 原始重力波をどうやって測れるかな、、、、

研究スタイル• 理論研究‒ 地道に未解決問題を調べる（答えがでるとは限らない）‒ 基本的にうまくいかない‒ 発見、新しい物理的効果が見つかれば、影響は大‒ 観測的に検証できることを調べたほうが良いのでは？

• 観測的研究 or 観測データ‒ 世界最高データにアクセスがあれば、最初から優位‒ 過去の測定結果の改善。（簡単に研究ができる）‒ インパクトは大。ただし、新しい観測結果が出るとそれ以降は忘れられる• ハイブリット研究‒ 観測にも関心を持ちつつ、理論研究にも通じている‒ どちらにも拘らず、興味の赴くままに研究皆さん、宇宙論をたくさん勉強
して、宇宙の神秘、精巧さを学んでください。そして、存分に楽しみましょう！
機会があれば、一緒に研究しま
しょう！