h is undervalued - university of chicagobackground.uchicago.edu/~whu/presentations/h014.pdf ·...
TRANSCRIPT
![Page 1: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/1.jpg)
Wayne HuSTSCI, April 2014
H0 is Undervalued
Eclipsing BinariesCMB
BAO
BICEP2?
Cepheids
MaserLensingTRGB
SBFSN
Ia
dark
ene
rgy
neut
rinos
inflation?
curv
atur
e
74
67
![Page 2: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/2.jpg)
The 1%
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∆H0=New Physics• H0: an end to end check of the standard cosmology when combined with the CMB
Planck 2013
![Page 4: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/4.jpg)
∆H0=New Physics• Standard ruler D(z*): sound horizon at recombination z*
• In flat ΛCDM, H0 only remaining parameter in D(z*) representing the density contributed by Λ - precisely predicted
Planck 2013
sound horizon calibrated[baryon/photon, matter/radiation]
![Page 5: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/5.jpg)
∆H0=New Physics• Compare precise predictions with H0 measurements• Any deviations indicate new physics during acceleration epoch or during recombination
Planck 2013
sound horizon calibrated[baryon/photon, matter/radiation]
D(z∗) =
∫ z∗
0
dz
H(z)
![Page 6: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/6.jpg)
∆H0=New Physics• Standard ruler D(z*): sound horizon at recombination z*
• Diffusion scale provides consistency check on sound horizon cali- bration: new physics at recombination, while BAO on acceleration
Planck 2013
consistency check
![Page 7: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/7.jpg)
Falsifying ΛCDM• CMB determination of matter density controls all determinations
in the deceleration (matter dominated) epoch
• Planck: Ωmh2 = 0.1426± 0.0025→ 1.7%
• Distance to recombination D∗ determined to 141.7% ≈ 0.43%
(ΛCDM result 0.46%; ∆h/h ≈ −∆Ωmh2/Ωmh
2)[more general: −0.11∆w − 0.48∆ lnh− 0.15∆ ln Ωm − 1.4∆ ln Ωtot = 0 ]
• Expansion rate during any redshift in the deceleration epochdetermined to 1
21.7%
• Distance to any redshift in the deceleration epoch determined as
D(z) = D∗ −∫ z∗
z
dz
H(z)
• Volumes determined by a combination dV = D2AdΩdz/H(z)
• Structure also determined by growth of fluctuations from z∗
![Page 8: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/8.jpg)
Value of Local Measurements• With high redshifts fixed, the largest deviations from the dark
energy appear at low redshift z ∼ 0
• By the Friedmann equation H2 ∝ ρ and difference between H(z)
extrapolated from the CMB H0 = 38 and 67 is entirely due to thedark energy density in a flat universe
• With the dark energy density fixed by H0, the deviation from theCMB observed D∗ from the ΛCDM prediction measures theequation of state (or evolution of the dark energy density)
pDE = wρDE
• Likewise current amplitude of structure, e.g. local clusterabundance, tests the smooth dark energy paradigm
![Page 9: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/9.jpg)
Forecasts for CMB+H0
• To complement CMB observations with Ωmh2 to 1%, an H0 of ~1% enables constant w measurement to ~2% in a flat universe
σ(lnH0) prior
σ(w
)
Planck: σ(lnΩmh2)=0.009
0.010.01
0.1
0.1
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New Physics?
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H0 is for Hints• Actual distance ladder measurements prefer larger value
Planck XVI
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Quantifying Tension• Predictions for H0 and the amplitude of structure from Planck in flat ΛCDM is 2-3+ σ in tension with measurements
Wyman, Rudd, Vanderveld, Hu (2013)
65 70 75 80
H0
0.0
0.2
0.4
0.6
0.8
1.0
P/P
max
0.8 0.9 1.0
S8
Planck vs Local: ΛCDM
![Page 13: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/13.jpg)
Dark Energy• Raising H0 inferred from Planck CMB measurements with dark energy requires phantom equations of state
Planck-CMB degeneracy
w
h0.6
-1.2
-1
-0.8
0.65 0.7 0.75
![Page 14: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/14.jpg)
Dark Energy• Raising H0 inferred from Planck CMB measurements with dark energy requires phantom equations of state
Planck-CMB degeneracy
w
h0.6
-1.2
-1
-0.8
0.65 0.7 0.75
![Page 15: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/15.jpg)
Dark Energy• Predicts larger BAO (θ) angular and radial (z) scale; larger SN=H0DA relative luminosity distance; larger linear growth
frac
tiona
l cha
nge
z0.01
-0.1
0
0.1
-0.05
0.05
0.1 1 10
∆lnH74
67
∆w=-0.23
![Page 16: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/16.jpg)
Dark Energy• Predicts larger BAO (θ) angular and radial (z) scale; larger SN=H0DA relative luminosity distance; larger linear growth
frac
tiona
l cha
nge
z0.01
-0.1
0
0.1
-0.05
0.05
0.1 1 10
∆lnH∆lnBAOθ
∆lnBAOz
tensionwith data!
∆w=-0.23
![Page 17: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/17.jpg)
Dark Energy• Predicts larger BAO (θ) angular and radial (z) scale; larger SN=H0DA relative luminosity distance; larger linear growth
frac
tiona
l cha
nge
z0.01
-0.1
0
0.1
-0.05
0.05
0.1 1 10
∆lnH∆lnBAOθ
∆lnGrow∆lnBAOz
tensionwith data!
∆w=-0.23
![Page 18: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/18.jpg)
Dark Energy• Predicts larger BAO (θ) angular and radial (z) scale; larger SN=H0DA relative luminosity distance; larger linear growth
frac
tiona
l cha
nge
z0.01
-0.1
0
0.1
-0.05
0.05
0.1 1 10
∆lnH∆lnBAOθ
∆ln(SN)
∆lnGrow∆lnBAOz
tensionwith data!
∆w=-0.23
![Page 19: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/19.jpg)
∆ΩK=0.012
Curvature• Predicts larger BAO (θ) angular and radial (z) scale; larger SN=H0DA relative luminosity distance; smaller linear growth
frac
tiona
l cha
nge
z0.01
-0.1
0
0.1
-0.05
0.05
0.1 1 10
tensionwith data!
alleviatetension
∆lnH∆lnBAOθ
∆ln(SN)
∆lnGrow
∆lnBAOz
![Page 20: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/20.jpg)
Neutrinos?
![Page 21: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/21.jpg)
Neutrinos• Hints of extra sterile neutrino species (~eV) in long-baseline and reactor anomalies• Potentially populated (partially?) in early universe• Changes expansion at recombination: age, sound horizon
![Page 22: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/22.jpg)
∆Neff=1
Neutrinos• Predicts same BAO (θ) angular and radial (z) scale; same SN=H0DA relative luminosity distance; same linear growth - change the ruler not the distance
frac
tiona
l cha
nge
z0.01
-0.1
0
0.1
-0.05
0.05
0.1 1 10
concord
make massivereduce growth
∆lnH
∆lnBAOθ ∆ln(SN)
∆lnGrow
∆lnBAOz
![Page 23: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/23.jpg)
ΛCDM∆Neff=1
l
l(l+1
)Cl/2
π
10
10-10
10-9
10-11
100 1000
Neutrinos• Predicts more damping of the CMB: sound horizon scales as conformal time η, random walk diffusion scale η1/2
![Page 24: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/24.jpg)
Gravitational Wave Excess• BICEP2 B-polarization inflationary gravitational waves (r=0.2) imply low multipole temperature excess that is not observed (r<0.1)
0 50 100 150 200 250 300
−0.01
0
0.01
0.02
0.03
0.04
0.05
BB
l
Pow
er (µ
K2 )
![Page 25: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/25.jpg)
Gravitational Wave Excess• BICEP2 B-polarization inflationary gravitational waves (r=0.2) imply low multipole temperature excess that is not observed (r<0.1)
![Page 26: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/26.jpg)
ΛCDM∆Neff=1
l
l(l+1
)Cl/2
π
10
10-10
10-9
10-11
100 1000
Neutrinos• Extra neutrino requires a blue-ward change in tilt, suppressing excess power at low multipoles
![Page 27: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/27.jpg)
Neu(trino) Concordance• Partially populated sterile, massive neutrinos change both the acoustic standard ruler and suppress structure and fixes both H0 and clusters
Wyman, Rudd, Vanderveld, Hu (2013)
65 70 75 80
H0
0.0
0.2
0.4
0.6
0.8
1.0
P/P
max
0.8 0.9 1.0
S8
Planck vs Local: ΛCDM
![Page 28: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/28.jpg)
Neu(trino) Concordance• Partially populated sterile, massive neutrinos change both the acoustic standard ruler and suppress structure and fixes H0, clusters and tensor excess
νrΛCDM: CMB predictions
Dvorkin, Wyman, Rudd, Hu (2014) [Zhang, Li, Zhang 2014]
![Page 29: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/29.jpg)
Neu(trino) Concordance• Partially populated sterile, massive neutrinos change both the acoustic standard ruler and suppress structure and fixes H0, clusters and tensor excess
νrΛCDM: CMB predictions
Dvorkin, Wyman, Rudd, Hu (2014) [Zhang, Li, Zhang 2014]
![Page 30: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/30.jpg)
Neu(trino) Concordance• Allows a fully populated extra sterile neutrino of 0.5eV
Sterile Neutrinos: >3σ stat
oscillation populatedmass=ms/∆Neff (eV)
∆Neff=1, 1 fully populated species
Dvorkin, Wyman, Rudd, Hu (2014) [Zhang, Li, Zhang 2014]
![Page 31: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/31.jpg)
Summary• ∆H0 from flat ΛCDM prediction indicates new physics
• Predictions from CMB are as precise as standard ruler calibration|∆h/h| ≈ |∆Ωmh
2/Ωmh2| ≈ 1.7% currently
• To test predictions require direct measurements at this precision
• New physics either additions to ΛCDM at recombination (standardruler) or during acceleration (distance-redshift)
• Consistency with damping tail, BAO distinguishes cases
Current mismatch between H0 ≈ 67 prediction and H0 ≈ 74
measurements may indicate extra relativistic species atrecombination
Simultaneously alleviates tension with BICEP2 inflationary tensordetection
If massive neutrino, also alleviates tension with cluster abundance
![Page 32: H is Undervalued - University of Chicagobackground.uchicago.edu/~whu/Presentations/H014.pdf · Wyman, Rudd, Vanderveld, Hu (2013) 65 70 75 80 H 0 0.0 0.2 0.4 0.6 0.8 1.0 P/P max 0.8](https://reader036.vdocuments.mx/reader036/viewer/2022062919/5f01c8d87e708231d40104fe/html5/thumbnails/32.jpg)
Summary• ∆H0 from flat ΛCDM prediction indicates new physics
• Predictions from CMB are as precise as standard ruler calibration|∆h/h| ≈ |∆Ωmh
2/Ωmh2| ≈ 1.7% currently
• To test predictions require direct measurements at this precision
• New physics either additions to ΛCDM at recombination (standardruler) or during acceleration (distance-redshift)
• Consistency with damping tail, BAO distinguishes cases
• Current mismatch between H0 ≈ 67 prediction and H0 ≈ 74
measurements may indicate extra relativistic species atrecombination
• Simultaneously alleviates tension with BICEP2 inflationary tensordetection
• If massive neutrino, also alleviates tension with cluster abundance