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Carlo Baccigalupi, SISSA
Dark energy Carlo Baccigalupi, SISSA
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Outline Fighting against a cosmological constant
Parametrizing cosmic acceleration current bounds on dark energy “Classic” dark energy effects “Modern” effects from dark energy: the promise of lensing Future dark energy probes
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Fighting the cosmological constant
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Fighting the cosmological constant
geometry Gµν+Λg µν=8πTµν +Vgµν quantum vacuum
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Fighting the cosmological constant
Λ:???
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Fighting the cosmological constant
Λ:??? V:M4Planck ???
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Fighting the cosmological constant
Λ:??? |Λ-V|/M4Planck≲10-123 V:M4Planck ???
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Fighting the cosmological constant
Λ:??? percent precision |Λ-V|/M4Planck=10-123 V:M4Planck ???
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Why so small with respect to any other known energy scale in physics?
(Boh?)2 Why so small with respect to any other known energy scale in physics? Why comparable to the matter energy density today?
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Dark energy Energy density radiation matter dark energy 0.5 104 z
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Dark energy Energy density radiation matter cosmological constant 0.5
104 z Einstein 1916
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Dark energy Energy density radiation matter tracking quintessence 0.5
104 z Ratra & Peebles, 1988
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Dark energy Energy density radiation matter early quintessence 0.5 104
z Wetterich 1988
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Dark energy Energy density radiation matter 0.5 104 z
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Parametrizing cosmic acceleration is …
Energy density radiation matter dark energy 0.5 104 z
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…parametrizing cosmic density
ρ∝(1+z)3[1+w] constant w Energy density radiation matter 0.5 104 z
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Parametrizing cosmic density
ρ∝exp{3∫0z [1+w(z)]dz/(1+z)} variable w Energy density 0.5 104 z
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Parametrizing cosmic acceleration: modeling
w=w0-wa(1-a)=w0+(1-a)(w∞-w0) w w∞ -wa w0 -1 1 0.5 a=1/(1+z) Chevallier & Polarski 2001, Linder 2003
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Parametrizing cosmic acceleration: binning
w -1 1 0.5 a=1/(1+z) Crittenden & Pogosian 2006, Dick et al. 2006
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Parametrizing cosmic acceleration: binning versus modeling
Binning: model independent , many parameters Modeling: always a bias , but a minimal model exists , made by w0 and its first time derivative Sticking with one particular model in between may be inconvenient, better relating that to one of the two approaches above
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Present cosmological bounds: one bin
Large scale structure w CMB SNIa -1+10% -1 -1-10% 1 0.5 a=1/(1+z) See Spergel et al., 2006, and references therein
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Present cosmological bounds: one bin, or maybe two
Large scale structure w CMB SNIa -1+10% -1 -1-10% 1 0.5 a=1/(1+z) Seljak et al. 2005
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“Classic” dark energy effects: projection
z dz ∫ D= H0-1 [ΣiΩi(1+z)3(1+wi)]1/2 w D
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“Classic” dark energy effects: growth of perturbations
Cosmological friction for cosmological perturbations∝H w ρ H
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“Classic” dark energy effects: large scale clustering
Compton wavelength at present: few hundreds of Mpc Ma et al. 1999, Montesano, Master degree, 2007, in preparation
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The “modern” era Energy density radiation matter dark energy 0.5 104 z
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The “modern” era Matter radiation equivalence CMB last scattering
Energy density Dark energy matter equivalence Dark energy domination dark energy 0.5 103 104 z
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The “modern” era Structure formation Matter radiation equivalence
CMB last scattering Energy density Dark energy matter equivalence Dark energy domination dark energy 0.5 103 104 z
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The “modern” era: “slicing” dark energy
structure formation in dark energy cosmologies, from galaxy clusters to relevant fractions of the Hubble volume Measure H(z) and therefore ρ(z), looking for effects which are sensitive to slices in redshifts Baryon acoustic oscillations Weak lensing in the optical band from lensing induced ellipticity on background galaxies by lenses at different redshifts Complementary weak lensing studies on CMB
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The “modern” era: “slicing” dark energy
structure formation in dark energy cosmologies, from galaxy clusters to relevant fractions of the Hubble volume Measure H(z) and therefore ρ(z), looking for effects which are sensitive to slices in redshifts Baryon acoustic oscillations Weak lensing in the optical band from lensing induced ellipticity on background galaxies by lenses at different redshifts Complementary weak lensing studies on CMB
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Structure formation and dark energy
Linear theory rather well understood Dark matter N-body in progress Poor knowledge of the gas properties, indication that the dark energy effects are not negligible Maio et al. 2007, Mainini, Bonometto 2007, Dolag et al. 2004, Maccio et al. 2003, …
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The promise of lensing Energy density radiation matter dark energy 0.5
104 z
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The promise of lensing Energy density radiation matter dark energy 0.5
104 z
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The promise of lensing Energy density 0.5 1 1.5 z
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The promise of lensing matter Energy density dark energy 0.5 z
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The promise of lensing Lensing probability observer 1/2 source By geometry, the lensing cross section is non-zero at intermediate distances between source and observer In the case of CMB as a source, the lensing power peaks at about z=1
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Galaxy lensing zsource Lensing cross section zlens
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The promise of lensing CMB lensing galaxy shell galaxy shell
Energy density CMB lensing galaxy shell galaxy shell galaxy shell 0.5 1 1.5 z
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CMB lensing: a science per se
Lensing is a second order cosmological effect Lensing correlates scales The lensing pattern is non-Gaussian Statistics characterization in progress, preliminary investigations indicate an increase by a factor 3 of the uncertainty from cosmic variance Smith et al. 2006, Lewis & Challinor 2006, Lewis 2005, …
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Forming structures - lenses
Lensing B modes E Forming structures - lenses B Last scattering Seljak & Zaldarriaga 1998
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Forming structures - lenses
Lensing B modes E Forming structures - lenses B acceleration Last scattering Seljak & Zaldarriaga 1998
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Breaking projection degeneracy
Acquaviva & Baccigalupi 2006
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Present lensing lensing distortion on CMB is undetected
Galaxy lensing has been detected and found consistent with the predictions of the concordance model in cosmology Refregier et al. 2007, DUNE proposal
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Future lensing DUNE (Dark Universe Explorer) to be proposed in June within the Cosmic Vision Program, able to measure the dark energy abundance in a few bins between z=0 and 1, with percent accuracy CMB lensing within reach of the forthcoming detectors Refregier et al. 2007, DUNE proposal, Oxley et al and references, EBEx proposal
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Conclusions The strong theoretical embarrassement with dark energy is likely to survive the consistency of the redshift average behavior of its energy density with the cosmological constant A two decade battle against the cosmological constant is possibly beginning, depending on ESA/NASA funding directions, concrete news within the end of 2007 The lensing capability of measuring H(z) represents the core of future investigations on dark energy
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