complementary probes of dark energy josh frieman snowmass 2001
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Key Issues 1.Is there Dark Energy? Will the SNe results hold up? 2.What is the nature of the Dark Energy? Is it or something else? 3.How does w = p X / X evolve? Dark Energy dynamics TheoryTRANSCRIPT
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Complementary Probes of Dark Energy
Josh Frieman
Snowmass 2001
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•The History of 20th Century Cosmology is littered with `detections’ of which later evaporated.
•Man (and woman) cannot live by Supernovae alone.
•The implications of Dark Energy are so profound that the SNe Ia results must be confirmed/extended by multiple independent methods with:
* different systematic errors * different cosmological parameter degeneracies
•The Cosmic Microwave Background is not a panacea: it has limited sensitivity to Dark Energy.
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Key Issues
1. Is there Dark Energy? Will the SNe results hold up?
2. What is the nature of the Dark Energy? Is it or something else?
3. How does w = pX/X evolve? Dark Energy dynamics Theory
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Physical Effects of Dark EnergyDark Energy affects expansion rate of the Universe:
Huterer & Turner
Dark Energy may also interact: long-range forces
Carroll
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Physical Observables: probing DE
1. Luminosity distance vs. redshift: dL(z) m(z) Standard candles: SNe Ia
2. Angular diameter distance vs. z: dA(z) Alcock-Paczynski test: Ly-alpha forest; redshift correlations
3. Number counts vs. redshift: N(M,z) probes: *Comoving Volume element dV/dzd *Growth rate of density perturbations (z) Counts of galaxy halos and of clusters; QSO lensing
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Comoving Distance: r(z) = dx/H(x)
In a flat Universe:
Luminosity Distance: dL(z) = r(z)(1+z)
Angular diameter Distance: dA(z) = r(z)/(1+z)
Comoving Volume Element: dV/dzd = r2(z)/H(z)
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Sensitivity to Dark Energy equation of state
Volume element
Comoving distance
Huterer & Turner
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Warning
Constraint contours depend on priors assumed for other cosmological parameters
Conclusions depend on projected state of knowledge/ignorance
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Goliath, etal
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Projected SNAP Sensitivity to DE Equation of State
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SNAP Sensitivity to Varying DE Equation of State
w = w0 + w1z + ...
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Angular Diameter Distance
Hui, Stebbins, Burles
Transverse extent
Angular size
Intrinsically isotropic clustering: radial and transverse sizes are equal
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Lyman-alpha forest: absorbing gas along LOS to distant Quasars
Clustering along line of sight
Cross-correlations between nearby lines of sight
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Sloan Digital Sky Survey
Projected constraintsfrom redshift space clustering of 100,000 Luminous Red Galaxies(z ~ 0.4)
Matsubara & Szalay
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CMB Anisotropy:
Angular diameterDistance to last Scattering surface
Peak Multipole
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Evolution of Angular clustering as probe of Angular diameter
Cooray, Hu, Huterer, Joffre
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Volume Element as a function of w
Dark Energy More volume at moderate redshift
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Counting Galaxy Dark Matter Halos with the DEEP Redshift Survey
Newman & Davis Huterer & Turner
10,000 galaxies at z ~ 1 with measured linewidths (rotation speeds)
NB: must probe Dark matter-dominated regions
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Growth of Density Perturbations
Holder
Open or w > -1
Flat, matter-dominated
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Counting Clusters of Galaxies
Sunyaev Zel’dovich effect
X-ray emission from cluster gas
Weak Lensing
Simulations:
growth factor
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Haiman,Holder, Mohr
DetectionMassthresholds
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R ~ 25 (SDSS South)
R ~ 27.5
R ~ 30
Weak Lensing:
Optical Multi-bandSurveys of Varying Depth
Joffre, Frieman
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Expected ClusterCounts in a Deep, wideSunyaev Zel’dovich Survey
Holder, Carlstrom, etal
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Constraints from a 4000 sq. deg. SZE Survey
Mlim = 2.5 x 1014 h-1 Msun
Holder, Haiman, Mohr
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Weak Lensing:Number Cts of Background Galaxies
Mag
Num
ber (
per .
5 m
ags)
10
10
10
10
7
5
3
1
16 18 20 22 24 26 28
Points: HDFCurve: extrapolationFrom SDSS luminosityFunction w/o mergers
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R ~ 25 (SDSS South)
R ~ 27.5
R ~ 30
Weak Lensing
S/N > 5 for aperture mass
Assume NFWProfiles
Conservative on Number counts
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Abell3667
z = 0.05
Joffre,etal
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WL Detected Clusters dn/dz per sq.deg.
z
dn/d
z pe
r sq.
deg
. 100
10
1
.5 1 1.5 2.5 2 3
SDSS
R=27.5R=30
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R ~ 27.5; 20,000 sq. deg. (co-added LSST or 1-year wide-field SNAP)
R ~ 30; 16 sq. deg.
R ~ 25,200 sq. deg(SDSS south)
Number of ClustersdetectedaboveThreshold
Here,8 = 1(will marginalize over)
(nominal SNAP in SNe mode)
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SNe
Projected Constraints From ClusterWeakLensing
Large sky coverageis critical
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Cluster Weak Lensing:
Bring in Da Noise,Bring in Da Funk
(account for:projection effectsFuzziness in Mass limit,alsovariations in NFW concentration parameter)
Note: there is more information to be used than N(z)
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Weak Lensing: Large-scale shear
Convergence Power Spectrum
1000 sq. deg. to R ~ 27
Huterer
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Projected ConstraintsFrom Cosmic Shear
1000 sq.deg.R ~ 27
Caveat: systematics in low S/N regime
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halosClusters,shear
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Conclusions
Multiple probes of Dark Energy, including SNe, should mature over the next 5-10 years
Independent confirmation of Dark Energy is within sight
Good prospects for independent constraints on the nature of the Dark Energy, with varying systematics and nearly `orthogonal’ parameterdegeneracies