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![Page 1: (some) Future CMB Constraints on fundamental physics Alessandro Melchiorri Universita’ di Roma, “La Sapienza” MIAMI2010, Fort Lauderdale December 15th.](https://reader036.fdocuments.in/reader036/viewer/2022062315/56649f1b5503460f94c3084b/html5/thumbnails/1.jpg)
(some) Future CMB Constraints on fundamental physics
Alessandro Melchiorri Universita’ di Roma, “La Sapienza”
MIAMI2010, Fort Lauderdale December 15th 2010
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Komatsu et al, 2010, 1001.4538
New WMAP results from 7 years of observations
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How to get a bound on a cosmological parameter
DATA
Fiducial cosmological model:(Ωbh2 , Ωmh2 , h , ns , τ, Σmν )
PARAMETERESTIMATES
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New Measurements, More Parameters !
• Neutrino masses
• Neutrino effective number
• Primordial Helium
m
effN
PY
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Small scale CMB can probe Helium abundance at recombination.
See e.g., K. Ichikawa et al., Phys.Rev.D78:043509,2008R. Trotta, S. H. Hansen, Phys.Rev. D69 (2004) 023509
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Komatsu et al, 2010, 1001.4538
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Cosmological (Active) NeutrinosNeutrinos are in equilibrium with the primeval plasma through weak interaction reactions. They decouple from the plasma at a temperature
MeVTdec 1We then have today a Cosmological Neutrino Background at a temperature:
eVkTKTT 43/1
1068.1945.111
4
With a density of:
33,
32
1121827.0)3(
4
3 cmTnTgnkkfff
That, for a massive neutrino translates in:
eV
mh
eV
m
h
mnk
kk
c
kk
kk
5.925.92
1 22
,
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Normal hierarchy Inverted hierarchy
If neutrino masses are hierarchical then oscillation experimentsdo not give information on the absolute value of neutrino masses
Moreover neutrino masses can also be degenerate
catmospheri321 ,, mmmm
SOLAR nKAMLAND
ATMO. nK2K
123 mmm 312 mmm
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Testing the neutrino hierarchy
Inverted Hierarchy predicts:
∑𝑚𝑣>0.10𝑒𝑉Normal Hierarchy predicts:
∑𝑚𝑣>0.05𝑒𝑉
Degenerate Hierarchy predicts:
∑𝑚𝑣>0.15𝑒𝑉
we assume 𝑚❑2=0.0025𝑒𝑉 2
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Current constraints on neutrino mass from Cosmology (Fogli et al, 2010 in preparation).
Blue: WMAP-7Red: w7+SN+Bao+H0Green: w7+CMBsuborb+SN+LRG+H0
See also:M. C. Gonzalez-Garcia, Michele Maltoni, Jordi Salvado, arXiv:1006.3795Toyokazu Sekiguchi, Kazuhide Ichikawa, Tomo Takahashi, Lincoln Greenhill, arXiv:0911.0976Extreme (sub 0.3 eV limits):F. De Bernardis et al, Phys.Rev.D78:083535,2008, Thomas et al. Phys. Rev. Lett. 105, 031301 (2010)
[eV]
Current constraints (assuming LCDM):
Smn<1.3 [eV] CMB (but see Maria’s talk)
Smn<0.7-0.5 [eV] CMB+other
Smn<0.3 [eV] CMB+LSS (extreme)
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Blue: WMAP-7Red: w7+SN+Bao+H0Green: w7+CMBsuborb+SN+LRG+H0
Current constraints on neutrino mass from Cosmology (Fogli et al, 2010 in preparation).
Constraints weaken by 30-50%when «dark energy» is included.
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Komatsu et al, 2010, 1001.4538
Neutrino background.Changes early ISW.Hint for N>3 ?
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Gianpiero Mangano, Alessandro Melchiorri, Olga Mena, Gennaro Miele, Anze SlosarJournal-ref: JCAP0703:006,2007
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J. Hamann et al, arXiv:1006.5276
3 Active massless neutrinos+Ns massive neutrinos
3 Active massive neutrinos +Ns massless neutrinos
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Latest results from ACT, Dunkley et al. 2010 𝑁𝑒𝑓𝑓 =5.3±1.3
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PlanckSatellite launch14/5/2009
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Planck First Light Survey (September 2009). Experiment is working as expected
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Blue: current dataRed: Planck
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Galli, Martinelli, Melchiorri, Pagano, Sherwin, Spergel, PRD submitted, arXiv:1005.3808 2010
Let’s consider not only Planck but alsoACTpol (From Atacama Cosmology Telescope,Ground based, results expected by 2013)CMBpol (Next CMB satellite, 2020 ?)
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Galli, Martinelli, Melchiorri, Pagano, Sherwin, Spergel, PRD submitted, arXiv:1005.3808 2010
Blue: Planck DYp=0.01
Red: Planck+ACTpol DYp=0.006
Green: CMBPol DYp=0.003
Constraints on Helium Abundance
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Galli, Martinelli, Melchiorri, Pagano, Sherwin, Spergel, PRD submitted, arXiv:1005.3808 2010
Constraints on Neutrino Number
Blue: Planck DNn=0.18
Red: Planck+ACTpol DNn=0.11
Green: CMBPol DNn=0.044
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Galli, Martinelli, Melchiorri, Pagano, Sherwin, Spergel, PRD submitted, arXiv:1005.3808 2010
Constraints on Neutrino Mass
Blue: Planck DSmn=0.16
Red: Planck+ACTpol DSmn=0.08
Green: CMBPol DSmn=0.05
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Testing the neutrino hierarchy
Inverted Hierarchy predicts:
∑𝑚𝑛>0.10𝑒𝑉Normal Hierarchy predicts:
∑𝑚𝑛>0.05𝑒𝑉
Degenerate Hierarchy predicts:
∑𝑚𝑛>0.15𝑒𝑉
we assume 𝑚❑2=0.0025𝑒𝑉 2
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Constraints on Neutrino Masses from CMB
[eV]
Black: Planck
Red: Planck+New exp. 1000 bol.
Blue: Planck+New exp. 5000 bol.
Limits at 95% c.l.:
Combining a new CMB experiment to Planck coud improve the bounds on the neutrinomass by a factor 3. This would:Falsify Degenerate Hierarchy and Probe the Inverted Hierarchy
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Constraints on Neutrino Masses from CMB+Priors
Red: 1000 riv+ Prior 1% H0+ Priori 2% Wm
Blue: 1000 riv+ Prior 1% H0+ Priori 2% Wm
Red Dashed: 1000 riv+ Prior 0.5% H0+ Priori 1% Wm
Blue Dashed: 1000 riv+ Prior 0.5% H0+ Priori 1% Wm
Limits at 95% c.l.:
∑𝑚𝑛<0.057 𝑒𝑉
∑𝑚𝑛<0.054 𝑒𝑉
∑𝑚𝑛<0.040𝑒𝑉
∑𝑚𝑛<0.035𝑒𝑉With external priors on the Hubble parameterAnd the matter density also the NormalHierarchy can be probed: safe detection ofa neutrino mass.
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• Recent CMB measurements fully confirm L-CDM. • With future measurements constraints on new parameters related to laboratoryPhysics could be achieved.
In 2012 from Planck we will know:
- If the total neutrino mass is less than 0.5eV.- If there is an extra background of relativistic particles.- Helium abundance with 0.01 accuracy.
CONCLUSIONS
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