understanding the properties of dark energy in the universehuterer/talks/pitt_2003.pdf · ¥ high...
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Understanding the Properties of
Dark Energy in the Universe
Dragan Huterer
Case Western Reserve University
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The Cosmic Food Pyramid
??
Radiation (
)Luminous Matter (
)
Baryonic Matter (
)
Dark Matter (
)
Dark Energy (
)
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Type Ia Supernovae
-20 0 20 40 60-15
-16
-17
-18
-19
-20
-20 0 20 40 60-15
-16
-17
-18
-19
-20
B Band
as measured
light-curve timescale “stretch-factor” corrected
days
MB
– 5
log(
h/65
)
days
MB
– 5
log(
h/65
)
Calan/Tololo SNe Ia
Kim, et al. (1997)
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Discovering SNe Ia
SupernovaDiscovery
(as seen from Hubble SpaceTelescope)
Difference
(as seen fromtelescopes on Earth)
3 Weeks Before
Supernova 1998baSupernova Cosmology Project
(Perlmutter, et al., 1998)
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Recent Supernova data
Supernova Cosmology Project
=0.3,
=0.7 =0.3,
=0.0 =1.0,
=0.0
m-M
(m
ag)
High-Z SN Search Team
0.01 0.10 1.00z
(m-
M)
(mag
)
! "$# ! "$% & '
() * +
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Parameterizing Dark Energy
"% & % & ) '
) ' , % &% &
' "# ( ' "% & ( ' (flat)
' ( '
'
# % & % & '
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Parameterizing Dark Energy
"% & % & ) '
) ' , % &% &
' "# ( ' "% & ( ' (flat)
' ( '
'
# % & % & '
may be varying:
* ( ' ' ( '
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Current Supernova Constraints
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Fine-Tuning Problems I: “Why Now ?”
DE is important only at
, since
% & #
"% &"#
( '
and )
100
105
1010
1015
1+z
10-60
10-40
10-20
100
1020
ρ (G
eV4 )
ρΛ
ρRAD
ρM
Λ dominates
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Fine-Tuning Problems II: “Why so small ?”
Refers to the vacuum energy, .
(recall
)
( ) ' () '
50 – 120 orders of magnitude discrepancy!
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A candidate: Quintessence
V
φ
100
102
104
106
108
1010
1012
z+1
-1.2
-0.8
-0.4
0.0
0.4
0.8
1.2
Equ
atio
n-of
-sta
te (
wQ
)
KE dominates
Q frozen
Q joins tracker sol.
100
102
104
106
108
1010
1012
z+1
10-50
10-40
10-30
10-20
10-10
ρ (G
eV4 )
Peebles & Ratra 1987, Caldwell, Dave & Steinhardt 1998
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Classical Tests
0.0 0.1 1.0 10.0 100.0 1000.0z
0.0
1.0
2.0
3.0
4.0
-dr/dw
r(z) w=-0.4
w=-1.0
0 1 2 3z
0
0.2
0.4
dV
/dΩ
dz
w=-0.4
-0.6
-0.8
-1.0
0.11.010.0z
0.1
1
δ(z)
/δ(to
day)
w=−1
w=−1/3
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Wish List
Goals:Measure
" % &,
Measure '
– equivalently, % & 'Measure any clustering of DE
Difficulties:
DE may cluster at scales
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Cosmological Tests of Dark Energy
Matter density
Vacuum density constant
CURRENT SN 1a
SNAP
Tegmark 2001
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Weak Gravitational Lensing
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Current Data and Constraints
0 0.5 1Ω
M
0.5
1
1.5
σ8
Refregier 2003, Bacon et al. 2003
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Weak Lensing and DE
1 10 100 1000 10000l
10−10
10−8
10−6
10−4
10−2
l(l+1
)Plκ /(
2π)
ΩX=0.70, w=−1.0ΩX=0.70, w=−0.5ΩX=0.65, w=−1.0
linear
Hu 1999, Huterer 2002, Refregier et al. 2003
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Weak Lensing and DE
1 10 100 1000 10000l
10−10
10−8
10−6
10−4
10−2
l(l+1
)Plκ /(
2π)
ΩX=0.70, w=−1.0ΩX=0.70, w=−0.5ΩX=0.65, w=−1.0
linear
0 1 2 3 4 5z
0
0.2
0.4
0.6
0.8
n(z)
0 0.2 0.4 0.6 0.8 1ΩM
−1.0
−0.8
−0.6
−0.4
−0.2
0.0
w
1 redshift bin2 bins10 bins
Hu 1999, Huterer 2002, Refregier et al. 2003
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Deeper and Wider
25 26 27 28 29depth (R−band mag)
0.00
0.01
0.02
0.03
0.04
0.05
σ(w)
σ(ΩX)
10 100 1000 10000sky coverage (deg
2)
0.00
0.02
0.04
0.06
0.08
0.10
σ(w)
σ(ΩX)
Huterer 2002
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Number Counts
0 0.5 1 1.5 2z
102
103
104
105
dN/d
z (
4000
deg
2 )
ΩM
=1, ΩDE
=0
ΩM
=0.3, ΩDE
=0.7, w=-1
w=-0.8
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Number Counts
Count clusters using X-ray, SZ, weaklensing...
Mass-observable relation
Haiman, Mohr & Holder 2001, Majumdar & Mohr 2003
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Cosmic Microwave Background Anisotropies
Bennett et al. 2003 (WMAP collaboration)
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CMB Sensitivity to Dark Energy
Peak locations are sensitive to dark energy (but not much):
1 10 100 1000 10000
l
0
1000
2000
3000
4000
5000
6000
7000
l(l+
1)C
l / (2
π) (
µK2 )
w = -1.0w = -0.5
Same as measurement of
with
fixed
End up constraining:
(Planck:
to
%)
Huterer & Turner 2001, Frieman et al. 2003
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SNe plus CMB
constant ' '
0 0.5 1 1.5 2 2.5z
MAX
0.1
0.2
0.3
0.4
0.5
0.6
σ w
SNeSNe + σΩ
M= 0.03
SNe + σΩM= 0.01
SNe + Planck SNe + Planck + σΩ
M= 0.01
0 0.5 1 1.5 2 2.5z
MAX
0.2
0.4
0.6
0.8
1
1.2
1.4
σ dw/d
z
SNeSNe + σΩ
M= 0.03
SNe + σΩM= 0.01
SNe + PlanckSNe + Planck + σΩ
M= 0.01
Frieman, Huterer, Linder & Turner 2003
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CMB-LSS cross-correlation
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CMB-LSS cross-correlation
−0.1 0.0 0.1 0.2 0.3⟨XT⟩/σXσT
0
50
100
150
Num
ber
of R
ealiz
atio
ns ΩΛ = 0.0ΩΛ = 0.5ΩΛ = 0.8
Boughn, Crittenden & Turok 1997
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CMB-LSS cross-correlation
−0.1 0.0 0.1 0.2 0.3⟨XT⟩/σXσT
0
50
100
150
Num
ber
of R
ealiz
atio
ns ΩΛ = 0.0ΩΛ = 0.5ΩΛ = 0.8
-0.5
0
0.5
1
1.5
2
wgT
(θ)
[µK
]
z ~ 0.57 z ~ 0.49
1 10
θ (degrees)
-1
-0.5
0
0.5
1
1.5 z ~ 0.43
1 10
z ~ 0.35
Boughn, Crittenden & Turok 1997, Scranton et al. 2003Understanding the Properties of Dark Energy in the Universe – p.23/37
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Strong Gravitational Lensing
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Strong Lensing Statistics
Required input:
Cosmology (
, , )Luminosity function (galaxies)or mass function (all halos)
Density profile of lenses
e.g. SIS:
or generalized NFW:
Magnification bias
1 1.2 1.4 1.6 1.8 2β
10-6
10-5
10-4
10-3
10-2
τ
Kochanek 1993, 1996, Cooray & Huterer 1999, Chae 2003,Davis, Huterer & Krauss 2003, Kuhlen, Keeton & Madau 2003
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Strong Lensing Statistics
Required input:
Cosmology (
, , )Luminosity function (galaxies)or mass function (all halos)
Density profile of lenses
e.g. SIS:
or generalized NFW:
Magnification bias
0.5 0.75 1 1.25 1.5 1.75 2β
1012
1013
1014
Mc /
(h-1
Msu
n)68% CL 95% CL
Huterer & Ma 2003
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Beyond
' '
' (
-1 -0.9 -0.8 -0.7 -0.6 -0.5w0
-1.0
-0.5
0.0
0.5
1.0
w’
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Beyond
' '
' (
-1 -0.9 -0.8 -0.7 -0.6 -0.5w0
-1.0
-0.5
0.0
0.5
1.0
w’
Principal Components of
0 0.5 1 1.5z
-0.5
0
0.5
e i(z)
1
2
3
4
49
50
Huterer & Starkman 2003
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Reconstruction of
( ' ( "$# ( ' ' '
"$# ( ' '
0 0.2 0.4 0.6 0.8 1z
−1.0
−0.8
−0.6
−0.4
−0.2
0.0
w(z
)
Huterer and Turner 1999; Chiba and Nakamura 1999, Weller & Albrecht 2002
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Requirements• Measure Ω and Λ• Measure w and w(z)
M
SCIENCE
• Sufficient (~2000) numbers of SNe Ia
• ...distributed in redshift
• ...out to z < 1.7
STATISTICAL REQUIREMENTS
Identified & proposed systematics:
• Measurements to eliminate / bound each one to +/-0.02mag
SYSTEMATICS REQUIREMENTS
SATELLITE / INSTRUMENTATION REQUIREMENTS
DATA SET REQUIREMENTS
• Discoveries 3.8 mag before max.• Spectroscopy with S/N=10 at 15 Å bins.• Near-IR spectroscopy to 1.7 µm.
•••
• ~2-meter mirror• 1-square degree imager• 3-channel spectrograph
(0.3 µm to 1.7 µm)
Derived requirements: • High Earth orbit • ~5 Mb/sec bandwidth
•••
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SuperNova/Acceleration Probe
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Mirror and Focal Plane
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SNAP SuperNovaAcceleration Probe
~2500 SNe Ia
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SNAP predicted constraints
No Big Bang
1 2 0 1 2 3
expands forever
-1
0
1
2
3
2
3
closed
recollapses eventually
Supernovae
CMB Boomerang
Maxima
Clusters
mass density
vacu
um
en
erg
y d
en
sity
(co
smo
log
ica
l co
nst
an
t)
open
flat
SNAP Target Statistical Uncertainty
network of cosmic strings w = –1/3
range of "Quintessence"
models
cosmological constant w = –1
90%95%
99%
68%
0.0
0.0 0.2 0.4 0.6 0.8 1.0
–0.2
–0.4
–0.6
–0.8
–1.0
ΩΜ = 1 − Ωu
equa
tion
of
stat
e w
= p
u /
ρu
Unknown Component,Ωu, of Energy Density
Flat Universe Constant w
Supernova Cosmology Project Perlmutter et al. (1998)
SNAP Satellite Target Statistical Uncertainty
Dark Energy
Understanding the Properties of Dark Energy in the Universe – p.33/37
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Weak Lensing with SNAP
0 0.1 0.2 0.3 0.4 0.5
ΩM
-1
-0.9
-0.8
-0.7
-0.6
-0.5
w
SNe
WL (PS)
WL (PS+BS)
SNe + WL (PS+BS)
-1.2 -1.1 -1 -0.9 -0.8w
0
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
dw
/dz
SNeWL (PS)
WL (PS+BS)
SNe + WL (PS+BS)
Understanding the Properties of Dark Energy in the Universe – p.34/37
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Understanding the Properties of Dark Energy in the Universe – p.35/37
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1
NASA-DOE
Joint Dark Energy Mission
Paul Hertz / NASA
Robin Staffin / DOE
Endorsed by
Raymond L. Orbach Edward J. Weiler
Director of the Office of Science Associate Administrator for Space Science
Department of Energy NASA
September 24, 2003 September 25, 2003Understanding the Properties of Dark Energy in the Universe – p.36/37
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Conclusions
Dark energy makes up
of energy density in the universe.It is smooth and has negative pressure.
We describe it via
and .
It affects cosmology by modifying the expansion rate
at recent times (
).
SNe Ia, weak lensing and number counts are most promising probes;variety of other methods can help.
Bright prospects with future wide-field surveys (SNAP, LSST, SPT,...)
But to understand DE, major insights will be needed from theorists.This will be especially hard if
!
Understanding the Properties of Dark Energy in the Universe – p.37/37