暗黒エネルギーとすばる - æ±äº¬å¤§å­¦ç´ ç²’å­ç‰©ç†å›½éš›ç ”ç©¶ã‚»ãƒ³ã‚¿ãƒ¼

UC Berkeley
2010410

• ~0.5%
• ~0.1–1.5%
• 4.5%
• 22%
• 74%
• 0%

• ~0.5%
• ~0.1–1.5%
• 4.5%
• 22%
• 74%
• 0%

()

IRCS (AO188)
Infrared imager and
spectrograph (#/$#=20,000)
HiCIAO (AO188)
Coronagraphic imager with
differential imaging
techniques
AO188
188-element
curvature
sensing
adaptive optics
system with a
laser guide star
capability
Nasmyth
Focus
Cassegrain
Focus
Prime
Focus
Illustration by Takaetsu Endo,
taken from Nikkei Science 1996
Suprime-Cam
Optical imager (34!"27!)
Nasmyth
Focus
8-10m class
HDS
Optical spectrograph
(#/$#=100,000)
FOCAS
Optical imager and
spectrograph
COMICS
IR imager and spectrograph
MOIRCS
NIR imager (7!"4!) and multiobject
(50)
5
spectrograph

~100Mpc(~300M light year)@z~0.5~5deg
Hyper-SC
SC
Other 8m Tels

• Ia
Ia

Ia
• Ia
•

Ia
• Ia
•
•

Ia
• Ia
•
•
•

Ia
• Ia
•
•
•
•

Ω Λ
1.5
Supernova Cosmology Project
Kowalski, et al., Ap.J. (2008)
Union 08
SN Ia
compilation
1.0
SNe
0.5
BAO
0.0
0.0 0.5 1.0
Ω m
Flat
CMB
acceleration
decceleration
•
•
•
•
•
•

E = 1 2 mȧ2 − G Nm
a
4π
3 a3 ρ m
a
a
ȧ
a 2
= 8π 3 G N ρ m − k a 2
•
•
a(t)
E>0, k=–1
E>0, k=0
E

• (70)

• (70)
•

• (70)
•
•

• (70)
•
•
•

• (70)
•
•
•
•

• (70)
•
•
•
•
•

• (70)
•
•
•
•
•

• (70)
•
•
•
•
•

Friedmann
ȧ
a 2
= 8π 3 G Nρ − k a 2 + Λ 3
= H 2 0
Ωrad
a 4
+ Ω m
a 3
+ Ω k
a 2 +
Ω
DE
a −3(1+w)
•
˙ρ = −3H(p + ρ) =−3H(w + 1)ρ
ρ = ρ 0 a −3(w+1) , ρa 3 = ρ 0 a −3w
ȧ ∝ a −(1+3w)/2
ä ∝−(1 + 3w) > 0 → w

•
•
•

•
•
•

•
•
•

•
(w

•
(w

•
(w

•
• “quintessence”
• m≈H0≈(TeV 8 /MPl 6 )
≈10 –84 GeV
• hierarchy problem
• w>–1

landscape
• ρΛ≈MPl 4 ≈10 120 ρΛobs
•
•
ρΛ

Cosmic Coincidence
Problem
• ρΛ≈(2meV) 4 ≈(TeV 2 /MPl) 4
• DMTeV-scale WIMP
ρm≈(TeV 2 /MPl)T 3
•
T≈(TeV 2 /MPl)≈10K
•
! [GeV cm –3 ]
10 67
10 61
10 55
10 49
10 43
10 37
10 31
10 25
10 19
10 13
10 7
10 1
10 –5
10 ! –11
10 "
–17
10 –23
10 –29
10 –35
10 –41
10 –18
10 6
10 4
T now
! radiation
! matter
10 2
10 0
10 –2 10 –4
T [GeV]
10 –6 10 –8 10 –10 10 –12 10 –14 10 –16

•
•
• w=–p/ρ=w(a)
• Dark Energy Task Force (NASA+DOE+NSF
panel) parameterization
w(a) =w 0 + w a (1 − a)

•
•
• w=–p/ρ=w(a)
• Dark Energy Task Force (NASA+DOE+NSF
panel) parameterization
w(a) =w 0 + w a (1 − a)

•
• redshift
• a/a0 = 1/(1+z)
•
• standard candle: SNe
• standard ruler: BAO

ds 2 = dt 2 − a(t) 2 dr
2
1 − kr 2 + r2 d 2 Ω
• comoving (proper) distance
ds 2 =0−→ d =
• luminosity distance
• angular diameter distance
dr
√
1 − kr
2 =
d L = d(1 + z)
d A = d/(1 + z)
dt
a(t) =
dz
H(z)

• growth factor g(z)
¨g +2Hġ =4πG N ρ m g = 3Ω mH 2 0
2a 3
• H
g
• exponential
• matter dominant
•

4
• SN (Type-Ia supernovae)
• CL (cluster survey)
• WL (weak lensing)
• BAO (baryon acoustic oscillation)

4
• SN (Type-Ia supernovae)
• CL (cluster survey)
• WL (weak lensing)
systematics
(DETF)
• BAO (baryon acoustic oscillation)

Weak Lensing

Abell

y
(x,y)
x
r r0
d 1 lens d 2
star

1
y
(x,y)
x
r r0
star
d 1 lens d -1 -0.5 0.5 1
2
0.5
-0.5
-1

Text

~10%

2000
~10%

2000
~10%

2000
~10%

No. ]

Intrinsic shape of a
background galaxy (ε~0.3)
Simulated lensing map
Gravitational lensing!
Galaxy shape actually seen
after GL: ε obs ~ε+γ GL
! The distortion signal of interest is tiny: γ GL ~0.01-0.1
! Indeed this coherent signal is statistically measurable
need ~10 galaxies per point

Sarah Bridle

cosmic shear
• 2lensing power
γ(θ) ∝ Ω m0
zS
0
dz L
d LS (z L ,z S )d L (z L )
d S (z S )
δ(z L , θ)
•
• power spectrum, bispectrum etc
•
~1%
10 8

state of the art
CFHT (4m)
ξ γ (θ) =γ(φ)γ ∗ (φ + θ) F.T.
−→ C γ (l)

photometric redshift

Baryon Acoustic
Oscillation

BAO

BAO

BAO

BAO
5

BAO
•
(148±3 Mpc)
5

BAO
•
(148±3 Mpc)
5

BAO
•
(148±3 Mpc)
•
5

BAO
•
(148±3 Mpc)
•
•
5

BAO
•
(148±3 Mpc)
•
•
•
5

BAO
•
(148±3 Mpc)
•
•
5
•
•

BAO
•
(148±3 Mpc)
•
•
5
•
•
•

sound horizon
http://astro.berkeley.edu/~mwhite/bao/

sound horizon
http://astro.berkeley.edu/~mwhite/bao/

sound horizon
http://astro.berkeley.edu/~mwhite/bao/

sound horizon
http://astro.berkeley.edu/~mwhite/bao/

sound horizon
http://astro.berkeley.edu/~mwhite/bao/

sound horizon
http://astro.berkeley.edu/~mwhite/bao/

sound horizon
http://astro.berkeley.edu/~mwhite/bao/

sound horizon
http://astro.berkeley.edu/~mwhite/bao/

A. Reid et al.
SDSS DR7

A. Reid et al.
SDSS DR7
Figure 2. Average likelihood contours recovered from the analysis of three
power spectra (top panel) and six power spectra (bottom panel) measured
from 1000 Log-Normal density fields. Contours are plotted for −2lnL =
2.3, 6.0, 9.2,correspondingtotwo-parameterconfidenceof68%,95%and
99% for a Gaussian distribution. Contours were calculated after increasing
the errors on the power spectrum band-powers as described inthetext.
Solid circles mark the locations of the likelihood maxima closest to the
true cosmology. We have plotted the likelihood surface as a function of
D V (z)/Mpc, forfixedr s (z d )=154.7Mpc,toshowdistanceerrorsif
the comoving sound horizon is known perfectly. The values of D V for our
input cosmology are shown by the vertical and horizontal solid lines.

the
als
the
one
the
con
0.0
low
(as
eff
BAO
SDSS DR7
~1M galaxies
is (
0.6
a 2
ban
add
bet
tain
Ω m
(Ω
WM
the
sin
on
ram
tio
pan
Wi
and
sio
the
ma
to
spe
the
ˆP h
tex
im

•
•
•
•
• systematics
(DETF)

SuMIRe
•
• 93
•
()
• 3000
•

SuMIRe
•
• 93
•
()
• 3000
•
HSC

SuMIRe
•
• 93
•
()
• 3000
•
HSC
PFS

Lens Barrel to complete Feb. 2011.
The HSC unit to complete Apr. 2011.
The unit to arrive at Subaru June 2011.
First light : October 2011.

Lens Barrel to complete Feb. 2011.
The HSC unit to complete Apr. 2011.
The unit to arrive at Subaru June 2011.
First light : October 2011.

HSC
≈300M galaxies

HSC

PFS
• 2000−3000
• HSC
• fiber positioner
•
• ≈3M galaxies

•

•
•

•
•
•

•
•
•
• 8

•
•
•
• 8
•

•
•
•
• 8
•
SuMIRe=Subaru Measurement of Images and Redshifts

(g/cm 2 )
4
3
2
1
–8
0
8
–8 0
8
2
3

137
100
70
85
3
1.8
COSMOS Survey

@IPMU
34
22
Big
Bang!
60
137

@IPMU
34
22
Big
Bang!
60
: 2000
137

@IPMU
60
34
22
Big
Bang!
: 2000
137

@IPMU
60
34
22
Big
Bang!
: 2000
137
!

@IPMU
60
34
22
Big
Bang!
: 2000
137
!

@IPMU
60
34
22
Big
Bang!
: 2000
137
!
3

@IPMU
60
34
22
Big
Bang!
: 2000
137
!
3
(8.2m)

ACT
2008 2009
2010
@IPMU
Δw~10%
Pan-
Starrs
BOSS
DES
2011
2011
2013
(σ(w pivot )σ(w a )) −1

ACT
2008 2009
2010
@IPMU
Δw~10%
Pan-
Starrs
BOSS
DES
2011
2011
2013
(σ(w pivot )σ(w a )) −1

ACT
2008 2009
2010
@IPMU
Δw~10%
Pan-
Starrs
BOSS
DES
2011
2011
2013
(σ(w pivot )σ(w a )) −1

Δw~3%
ACT
2008 2009
2010
@IPMU
Δw~10%
Pan-
Starrs
BOSS
DES
2011
2011
2013
(σ(w pivot )σ(w a )) −1

Δw~3%
ACT
2008 2009
2010
@IPMU
Δw~10%
Pan-
Starrs
BOSS
DES
2011
2011
LSST, JDEM, Euclid~x10
2013
(σ(w pivot )σ(w a )) −1

• 30

• 30
• 95

• 30
• 95
•

• 30
• 95
•

• 30
• 95
•
•

• 30
• 95
•
•
• 27

• 30
• 95
•
•
• 27
•

• optical frequency combredshift
1cm/sec
• 10
c t H0≈15 cm/sec
• TMT