cmb as a dark energy probe
DESCRIPTION
CMB as a dark energy probe. Carlo Baccigalupi. Outline. Fighting against a cosmological constant Parametrizing cosmic acceleration The CMB role in the current dark energy bounds “Classic” dark energy effects on CMB “Modern” CMB relevance for dark energy: the promise of lensing - PowerPoint PPT PresentationTRANSCRIPT
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CMB as a dark energy probeCMB as a dark energy probe
Carlo BaccigalupiCarlo Baccigalupi
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Outline Outline
Fighting against a cosmological constant Fighting against a cosmological constant Parametrizing cosmic accelerationParametrizing cosmic acceleration The CMB role in the current dark energy boundsThe CMB role in the current dark energy bounds ““Classic” dark energy effects on CMBClassic” dark energy effects on CMB ““Modern” CMB relevance for dark energy: the Modern” CMB relevance for dark energy: the
promise of lensingpromise of lensing Lensing B modes in CMB polarizationLensing B modes in CMB polarization Future CMB data and dark energyFuture CMB data and dark energy
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Fighting the cosmological constantFighting the cosmological constant
GGµµνν=8=8ππTTµµνν
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Fighting the cosmological constantFighting the cosmological constant
GGµµνν++ΛΛgg µ µνν=8=8ππTTµµνν +Vg+Vgµµνν
geometry
quantum vacuum
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Fighting the cosmological constantFighting the cosmological constant
ΛΛ:???:???
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Fighting the cosmological constantFighting the cosmological constant
ΛΛ:???:???
V:MV:M44PlanckPlanck
??????
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Fighting the cosmological constantFighting the cosmological constant
ΛΛ:???:???
V:MV:M44PlanckPlanck
??????
||ΛΛ-V|/M-V|/M44PlanckPlanck≲10≲10-123-123
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Fighting the cosmological constantFighting the cosmological constant
ΛΛ:???:???
V:MV:M44PlanckPlanck
??????
||ΛΛ-V|/M-V|/M44PlanckPlanck=10=10-123-123
percent precision
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(Boh?)(Boh?)22
Why so small with respect Why so small with respect to any other known energy to any other known energy scale in physics?scale in physics?
Why comparable to the Why comparable to the matter energy density matter energy density today?today?
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darkdark energyenergy
Dark energyDark energy
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cosmological constantcosmological constant
Dark energyDark energy
Einstein 1916
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tracking quintessencetracking quintessence
Dark energyDark energy
Ratra & Peebles, 1988
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early quintessenceearly quintessence
Dark energyDark energy
Wetterich 1988
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Dark energyDark energy
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Parametrizing cosmic acceleration is …Parametrizing cosmic acceleration is …
ρρ(z)(z)
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……parametrizing cosmic densityparametrizing cosmic density
ρρ∝∝(1+z)(1+z)3[1+w]3[1+w]
constant wconstant w
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Parametrizing cosmic densityParametrizing cosmic density
ρρ∝∝exp{3∫exp{3∫00z z [1+w(z)]dz/(1+z)}[1+w(z)]dz/(1+z)}
variable wvariable w
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a=1/(1+z)
w
0.51
Parametrizing cosmic acceleration: Parametrizing cosmic acceleration: modelingmodeling
w=ww=w00-w-waa(1-a)=w(1-a)=w00+(1-a)(w+(1-a)(w∞∞-w-w00))
-1
w0
-wa
w∞
Chevallier & Polarski 2001, Linder 2003
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a=1/(1+z)
w
0.51
Parametrizing cosmic acceleration: Parametrizing cosmic acceleration: binningbinning
-1
Crittenden & Pogosian 2006, Dick et al. 2006
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Parametrizing cosmic acceleration: Parametrizing cosmic acceleration: binning versus modelingbinning versus modeling
Binning: model independent Binning: model independent , many , many parameters parameters
Modeling: always a bias Modeling: always a bias , but a minimal , but a minimal model exists model exists , made by w, made by w00 and its first and its first time derivativetime derivative
Sticking with one particular model in Sticking with one particular model in between may be inconvenient, better between may be inconvenient, better relating that to one of the two approaches relating that to one of the two approaches aboveabove
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a=1/(1+z)
w
0.51
Present cosmological bounds: one binPresent cosmological bounds: one bin
-1
See Spergel et al., 2006, and references therein
-1+10%
-1-10%
CMBCMB
Large scale structureLarge scale structure
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a=1/(1+z)
w
0.51
Present cosmological bounds: one bin, Present cosmological bounds: one bin, or maybe twoor maybe two
-1
Seljak et al. 2005
-1+10%
-1-10%
CMBCMB
Large scale structureLarge scale structure
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““Classic” dark energy effects on CMB: Classic” dark energy effects on CMB: projectionprojection
D= H0-1
dz
[ΣiΩi(1+z)3(1+wi)]1/2∫0
z
w D
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““Classic” dark energy effects on CMB: Classic” dark energy effects on CMB: integrated Sachs-Wolfeintegrated Sachs-Wolfe
Cosmological friction for cosmological perturbations∝H
w ρ H
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The “modern” eraThe “modern” era
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The “modern” eraThe “modern” era
Dark energy matter equivalence
CMB last scattering
Matter radiation equivalence
103
Dark energy domination
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The “modern” eraThe “modern” era
Dark energy matter equivalence
CMB last scattering
Matter radiation equivalence
103
Dark energy domination
Str
uctu
re fo
rmat
ion
Str
uctu
re fo
rmat
ion
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The “modern” era: study the signatures The “modern” era: study the signatures of structure formation on the CMBof structure formation on the CMB
Beat cosmic variance by predicting the Beat cosmic variance by predicting the ISW effect from local and observed ISW effect from local and observed structuresstructures
Study lensed CMBStudy lensed CMB
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The “modern” era: study the signatures The “modern” era: study the signatures of structure formation on the CMBof structure formation on the CMB
Beat cosmic variance by predicting the Beat cosmic variance by predicting the ISW effect from local and observed ISW effect from local and observed structuresstructures
Study lensed CMBStudy lensed CMB
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The promise of lensingThe promise of lensing
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The promise of lensingThe promise of lensing
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The promise of lensingThe promise of lensing
1 1.5
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The promise of lensingThe promise of lensing
darkdark energyenergy
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The promise of lensingThe promise of lensing
By geometry, the lensing cross section is non-zero at By geometry, the lensing cross section is non-zero at intermediate distances between source and observerintermediate distances between source and observer
In the case of CMB as a source, the lensing power In the case of CMB as a source, the lensing power peaks at about z=1peaks at about z=1
Any lensing power in CMB anisotropy must be quite Any lensing power in CMB anisotropy must be quite sensitive to the expansion rate at the onset of sensitive to the expansion rate at the onset of accelerationacceleration
Lens
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prob
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ty
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The promise of lensingThe promise of lensing
Lens
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How lensing modifies the CMBHow lensing modifies the CMB
Most relevant on the angular scales Most relevant on the angular scales subtended by lenses, from the arcminute subtended by lenses, from the arcminute to the degreeto the degree
It makes the CMB non-GaussianIt makes the CMB non-Gaussian It smears acoustic peaks It smears acoustic peaks It activates a broad peak in the B modes of It activates a broad peak in the B modes of
CMB polarizationCMB polarization
Seljak & Zaldarriaga 1997, Spergel & Goldberg 1999, Hu 2000, Giovi et al. 2005
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How lensing modifies the CMBHow lensing modifies the CMB
Most relevant on the angular scales Most relevant on the angular scales subtended by lenses, from the arcminute subtended by lenses, from the arcminute to the degreeto the degree
It makes the CMB non-GaussianIt makes the CMB non-Gaussian It smears out acoustic peaks It smears out acoustic peaks It activates a broad peak in the B modes of It activates a broad peak in the B modes of
CMB polarizationCMB polarization
Seljak & Zaldarriaga 1997, Spergel & Goldberg 1999, Hu 2000, Giovi et al. 2005
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CMB angular power spectrumCMB angular power spectrum
Angle ≈ 200/l degrees
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Known CMB angular power spectrum: Known CMB angular power spectrum: WMAP first yearWMAP first year
Angle ≈ 200/l degrees
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Known CMB angular power spectrum: Known CMB angular power spectrum: WMAP third yearWMAP third year
Angle ≈ 200/l degrees
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CMB angular power spectrumCMB angular power spectrum
Angle ≈ 200/l degrees
Primordial power
Gravity waves
Acoustic oscillations
Reionization
Lensing
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Last scattering
Forming structures - lenses
EEBB
Lensing B modesLensing B modes
Seljak & Zaldarriaga 1998
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Forming structures - lenses
EEBB
Lensing B modesLensing B modes
acceleration
Last scattering
Seljak & Zaldarriaga 1998
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CMB lensing: a science per seCMB lensing: a science per se
Lensing is a second order Lensing is a second order cosmological effectcosmological effect
Lensing correlates scalesLensing correlates scales The lensing pattern is The lensing pattern is
non-Gaussiannon-Gaussian Statistics characterization Statistics characterization
in progress, preliminary in progress, preliminary investigations indicate an investigations indicate an increase by a factor 3 of increase by a factor 3 of the uncertainty from the uncertainty from cosmic variancecosmic variance
Smith et al. 2006, Lewis & Challinor 2006, Lewis 2005, …
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Lensing strength recording the cosmic Lensing strength recording the cosmic density at the onset of accelerationdensity at the onset of acceleration
Lens
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Lensing strength recording the cosmic Lensing strength recording the cosmic density at the onset of accelerationdensity at the onset of acceleration
Lens
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Cosmological constant
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Lensing strength recording the cosmic Lensing strength recording the cosmic density at the onset of accelerationdensity at the onset of acceleration
Lens
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Cosmological constant
darkdark energyenergy
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So let’s play…So let’s play…
Upgrade a Boltzmann code for lensing Upgrade a Boltzmann code for lensing computation in dark energy cosmologies computation in dark energy cosmologies (Acquaviva et al. 2004 experienced doing (Acquaviva et al. 2004 experienced doing that with cmbfast, lensing.f has to be that with cmbfast, lensing.f has to be substantially changed…)substantially changed…)
Get lensed CMB angular power spectra for Get lensed CMB angular power spectra for different dark energy dynamicsdifferent dark energy dynamics
Look at the amplitude of lensing B modesLook at the amplitude of lensing B modes
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Play…Play… SUGRA vs. Ratra-Peebles SUGRA vs. Ratra-Peebles
quintessencequintessence Check structure formation, linear Check structure formation, linear
perturbation growth rate, …perturbation growth rate, … Perturbations and distances Perturbations and distances
affected by geometry coherently…affected by geometry coherently… Effects sum up in the lensing Effects sum up in the lensing
kernelkernel
Acquaviva & Baccigalupi 2005
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Play…Play…
TT and EE spectra: slight TT and EE spectra: slight projection shiftprojection shift
BB amplitude: reflecting BB amplitude: reflecting cosmic density at cosmic density at structure formation/onset structure formation/onset of accelerationof acceleration
Acquaviva & Baccigalupi 2005
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Breaking projection degeneracyBreaking projection degeneracy
Acquaviva & Baccigalupi 2005
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Get serious…Get serious…
A Fisher matrix analysis indicates that a A Fisher matrix analysis indicates that a 1%-10% measuremtent on both w1%-10% measuremtent on both w00 and w and waa is achievable by having lensing B modes is achievable by having lensing B modes measured on a large sky area, few measured on a large sky area, few arcminute resolution, micro-K noisearcminute resolution, micro-K noise
New relevance for searching B modes in New relevance for searching B modes in CMB polarization?CMB polarization?
Independent check of the efficiency of the Independent check of the efficiency of the effect ongoing…effect ongoing…
Acquaviva & Baccigalupi 2005
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Forthcoming B modes huntersForthcoming B modes hunters Planck, marginal, large scale Planck, marginal, large scale
only)only) EBEx, sensitivity ok for lensing EBEx, sensitivity ok for lensing
B modes, north american flight B modes, north american flight in fall 2007in fall 2007
QUIET , sensitivity ok for QUIET , sensitivity ok for lensing B modeslensing B modes
Clover Clover BrainBrain …… Complete list available at Complete list available at
lambda.gsfc.nasa.govlambda.gsfc.nasa.gov Beyond Einstein, Cosmic Beyond Einstein, Cosmic
Vision…Vision…
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Conclusions Conclusions
CMB lensing sensitivity is at high redshifts CMB lensing sensitivity is at high redshifts The CMB is not a probe of the dark energy The CMB is not a probe of the dark energy
density redshift average, but can density redshift average, but can reasonably put two error bars on the dark reasonably put two error bars on the dark energy abundance at z=0 and 0.5energy abundance at z=0 and 0.5
Partner to other probes for constraining Partner to other probes for constraining the redshift behavior of the dark energythe redshift behavior of the dark energy
You do not know where systematics hit You do not know where systematics hit more, so keep it in your toolboxmore, so keep it in your toolbox