neutrino mass from cosmology - slac indico (indico) · neutrino mass w m matter density a s...
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PINS, slac, July 16th 2019
Neutrino massFrom cosmology
Jia LiuNSF Fellow
Image credit: Tom Abel & Ralf Kaehler (KIPAC, SLAC)
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Neutrino Oscillation ImpliesNeutrinos Must Have Mass
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Normal InvertedΣmν>0.06 eV Σmν>0.1 eV
?0
Neutrino Mass from Oscillation Experiments
m2
2.5⨉10-3eV2Atmospheric / beam:
SK, MINOS, NOvA, T2K, IceCube
7.6⨉10-5eV2Solar:
SNO, KamLAND, Borexino
ν
3ν
2
ν1
ν3
ν2
ν1
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Standard Model
Fermions
1012eV
109eV
106eV
103eV
1 eV
10-3eV
10-6eV
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Mass generation mechanism?
CP Violation &Matter-antimatter asymmetry?
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Do RH neutrinos exist?
CP Violation &Matter-antimatter asymmetry?
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CP Violation &Matter-antimatter asymmetry?
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Current Constraints
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Electron kinetic Energy
Eve
nt C
ount
s
* 0νββ experiments (KamLAND-Zen, GERDA, etc.) are also sensitive to neutrino mass
-
Particle Experiments: Tritium Beta Decay
End pointmν = 0
End pointmν > 0
18keV
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Current Constraints (95% CL)Minimum mass: 0.06 eV (Normal), 0.1 eV (Inverted)
Particle experiment Troitsk beta decay (Assev+2011)
mνeeff < 2 eV
KATRIN projection: 0.2 eV
Cosmology CMB, CMB Lensing, BAO (Planck 2018)
Σmν < 0.12 eVLSST+DESI+CMB-S4 forecast: 0.03 eV
2018-2023 2022-2019-
~2027-
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Cosmic Neutrinos
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CMB :380,000 yrs after
the Big Bang
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CMB :380,000 yrs after
the Big Bang
C𝝂B :One second after
the Big Bang
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CMB :380,000 yrs after
the Big Bang
C𝝂B :One second after
the Big Bang
?
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IceCube collaboration / NSF / University of Wisconsin
Cosmic 𝝂.Difficult to detect due to their low energy
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PTOLEMY ExperimentPrinceton Tritium Observatory for Light, Early-Universe, Massive-Neutrino Yield
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PTOLEMY ExperimentPrinceton Tritium Observatory for Light, Early-Universe, Massive-Neutrino Yield
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Our Universe as the “Detector”
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Structure Formation
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Microwave sky seen by COBE
Extremely smooth density field
380,000 years after the Big Bang (z=1100)
Galaxy distribution measured by 2dF
Structures (galaxies, clusters) formed
Today
Structure Formation
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Massive Cosmic Neutrinos Suppress the Growth of Structure
With large thermal velocities, cosmic neutrinos suppress structure growth below their free-streaming length (e.g. ~110 Mpc for 0.1eV).
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Standard Model of Cosmology Massive Neutrinos
Credit: Katrin Heitmann
Massive Cosmic Neutrinos Suppress the Growth of Structure
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How do we measure the suppression
in data?
Galaxy Density Map(Sloan Digital Sky Survey)
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Two Point Correlation FunctionFourier Space: Power Spectrum
Measures clustering as a function of distance
Image: SDSS galaxies
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Matter Power SpectrumCosmic Scale Cluster/Galaxy
Suppression due to
massive neutrinos
Neutrino Mass
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Credit: Carlton Baugh
Galaxies: Biased Tracers of Matter Distribution
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Weak Gravitational Lensing:Sensitive to the Total Matter Distribution
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Weak Lensing of the CMB
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UNLENSEDCr
edit:
Bla
ke S
herw
in
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LENSEDCr
edit:
Bla
ke S
herw
in
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Σmν in the Next Decade
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Modeling Nonlinear Structure
Survey Systematics(photo-z, shape…)
AstrophysicalProcesses(Baryons, IA...)
Coordinating Joint Probes
Roadmap to pin down Σm𝜈
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Modeling Nonlinear Structure
Survey Systematics(photo-z, shape…)
AstrophysicalProcesses(Baryons, IA...)
Coordinating Joint Probes
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Modeling Nonlinear Structure Σm𝜈= 0.1eV
–– Linear Theory–– Nonlinear (Takahashi)–– Nonlinear (Bird)
Linear Regime:Analytical Linear Theory
Mildly Nonlinear:Perturbation Theory
Highly Nonlinear:Numerical
Simulations
Neutrino Effect
StrongestHere
10% errors in current nonlinear models(we need <1%!)
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MassiveNuSCosmological Massive Neutrino SimulationsJia Liu et al 2018 (https://arxiv.org/abs/1711.10524)
Σm𝜈 (eV)Neutrino Mass
𝛀 m M
atter
Densit
y
As Primordial Clustering Amplitude
Each of the 100 points is a high resolution simulation
(2 million core hours in total)
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Modeling Nonlinear Structure
Survey Systematics(photo-z, shape…)
AstrophysicalProcesses(Baryons, IA...)
Coordinating Joint Probes
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Modeling Nonlinear Structure
Survey Systematics(photo-z, shape…)
Coordinating Joint Probes
AstrophysicalProcesses(Baryons, IA...)
Dark matter Baryons
Illustris simulation
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Modeling Nonlinear Structure
Survey Systematics(photo-z, shape…)
AstrophysicalProcesses(Baryons, IA...)
Coordinating Joint Probes
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18,000 deg2
8.4m ugrizy
15,000 deg2 1.2m Optical/NIR
2,200 deg2(deep)2.4m NIR
16,000 deg2 1𝜇K-arcmin
28-230GHz(?)
16,000 deg2 6𝜇K-arcmin27-280GHz
Upcoming CMB and Galaxy Surveys
LiteBIRD
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Mishra-Sharma, Alonso, Dunkley 2018
CMB S4LSST Clustering
LSST Lensing
LSST
S4+LSST S4+DESIw
dark
ene
rgy
equa
tion
of s
tate
No experiment can do it alone
2021 2022 2023 2024 2025 2026 2027 2028 2029LSSTEuclid
WFIRSTSimons Observatory
CMB-S4
Galaxy CM
B
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Massive NeutrinosSuppress the structure growth
Summary
Massless
Massive
Must Combe Multiple Cosmological Probes
Mishra-Sharma, Alonso, Dunkley 2018
CMB S4LSST Clustering
LSST Lensing
LSST
S4+LSST S4+DESI
w da
rk e
nerg
y eq
uatio
n of
st
ate