Particle Physics with the Cosmic Microwave Background with SPT-3G - - PowerPoint PPT Presentation
Particle Physics with the Cosmic Microwave Background with SPT-3G Jessica Avva on behalf of the SPT-3G collaboration UC Berkeley Photo: Jason Galliccio The Early Universe: a Particle Physics Laboratory Neutrinos Atoms < 1% 4.6% Today
Jessica Avva on behalf of the SPT-3G collaboration UC Berkeley
Photo: Jason Galliccio
NASA/WMAP Science Team 2
Dark Matter 23% Dark Energy 72% Atoms 4.6% Neutrinos < 1%
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Neutrinos Photons Dark Matter + Atoms Dark Energy Redshift 109 105 1100 0
The universe is dark energy dominated
Today Energy Density (log scale)
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Neutrinos Photons Dark Matter + Atoms Dark Energy Redshift 109 105 1100 0 Energy Density (log scale)
The universe is dark energy dominated The universe is matter dominated
Today
Early Universe (~380,000 yrs after the BIg Bang)
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Neutrinos Photons Dark Matter + Atoms Dark Energy Redshift 109 105 1100 0
The universe is matter dominated The universe is radiation dominated
Early Universe (~380,000 yrs after the BIg Bang) Early Early Universe (~1 sec after the Big Bang
The universe is dark energy dominated
Today
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Energy Density (log scale)
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Observable: [~380,000 yrs after the Big Bang] The Cosmic Microwave Background Observable: [now] Galaxy Surveys, tracers of large scale structure
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Beginning: Neutrinos (CνB) were relativistic, dominant observable is their effect on the expansion history of the universe Now: CνB neutrinos are not relativistic, dominant
structure growth Observable: [~380,000 yrs after the Big Bang] The Cosmic Microwave Background Observable: [now] Galaxy Surveys, tracers of large scale structure
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Matter underdensity Matter overdensity
Neff corresponds to number of relativistic species in early universe - sensitive to number of neutrinos, sterile neutrinos, light dark matter, axions, etc. Standard Model prediction for 3 neutrinos = 3.046
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Matter underdensity Matter overdensity
Neff corresponds to number of relativistic species in early universe - sensitive to number of neutrinos, sterile neutrinos, light dark matter, axions, etc. Standard Model prediction for 3 neutrinos = 3.046
(typical overdensity / underdenisty size)
scale (map smoothed below this scale) More relativistic species and/or dark particles (larger Neff) = increased expansion rate = increased θs and θd
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Matter underdensity Matter overdensity
Neff corresponds to number of relativistic species in early universe - sensitive to number of neutrinos, sterile neutrinos, light dark matter, axions, etc. Standard Model prediction for 3 neutrinos = 3.046
(typical overdensity / underdenisty size)
scale (map smoothed below this scale) More relativistic species and/or dark particles (larger Neff) = increased expansion rate = increased θs and θd
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the CνB loses energy
and they become bound to large structures
energy, time of transition for when neutrinos become non-relativistic determines Σmν
Time
Now
Anderson 2018
NASA Goddard 10m diameter
Huang 1907.09621
8 arcmin diameter circle
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Observation Strategy: Observe the SPT-3G 1500 deg2 field every ~2 days for 6 years!
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Power Spectrum →Neff
Galaxy Clusters and Lensing Power Spectrum→Σmν
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Power Spectrum →Neff
Galaxy Clusters and Lensing Power Spectrum→Σmν
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Planck SPTpol SPT-3G forecast
Small angular scales Large angular scales
Daniel Dutcher
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SPT-3G EE Data
Using 2018 150 GHz data, SPT-3G is the most sensitive measurement of the CMB EE polarization spectrum from 700 < ℓ < 1700!
Daniel Dutcher
Neff
Characterize suppression
small angular scales
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Planck best-fit model
SPT-3G EE Data
Daniel Dutcher Characterize suppression
small angular scales
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Characterize peak locations at larger angular scales
Planck best-fit model
SPT-3G EE Data
https://arxiv.org/pdf/1907.04473.pdf
Standard Model Predicted value for 3 neutrino species: Neff = 3.046 Previous constraint from SPTpol + PlanckTT - 10 σ confirmation of CνB: Neff= 3.54 ± 0.54 (Henning et al, ΛCDM+Yp+Neff)
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Precision constraint of the energy density in relativistic and dark particles; search for deviations from Standard Model prediction
SPT-3G forecast ΔNeff = 0.1 (1𝜏) Planck constraint ΔNeff = 0.19 (1𝜏) Constraints and Forecasts for ΛCDM+Yp+Neff Cosmology
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Power Spectrum →Neff
Galaxy Clusters and Lensing Power Spectrum→Σmν
The CMB probes the evolution of structure over time CMB Lensing: Measure the distortions to the CMB power spectrum by intervening matter between us and the surface of last scattering Galaxy Clusters: Measure the abundance of galaxy clusters as a function of mass and redshift
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ESA and the Planck Collaboration
The CMB probes the evolution of structure over time CMB Lensing: Measure the distortions to the CMB power spectrum by intervening matter between us and the surface of last scattering Galaxy Clusters: Measure the abundance of galaxy clusters as a function of mass and redshift
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ESA and the Planck Collaboration
The CMB probes the evolution of structure over time Galaxy Clusters: Measure the abundance of galaxy clusters as a function of mass and redshift
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The CMB probes the evolution of structure over time CMB Lensing: Measure the distortions to the CMB power spectrum by intervening matter between us and the surface of last scattering Galaxy Clusters: Measure the abundance of galaxy clusters as a function of mass and redshift
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ESA and the Planck Collaboration
The CMB probes the evolution of structure over time CMB Lensing: Measure the distortions to the CMB power spectrum by intervening matter between us and the surface of last scattering
T: Gaussian random temperature field E (curl-free component): CMB has polarization follows gradient of temperature field. E modes should exist from primordial density fluctuations we see in T. B (curl component): Polarization that follows gradient of temperature
from just primordial density fluctuations we see in T.
Hu and Okamoto 2001 26
ESA and the Planck Collaboration
The CMB probes the evolution of structure over time CMB Lensing: Measure the distortions to the CMB power spectrum by intervening matter between us and the surface of last scattering
Hu and Okamoto 2001
CMB lensing potential: 2-d projection of the full 3-d gravitational potential between us and surface of last scattering
Adds non-gaussianity and polarization curl component
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ESA and the Planck Collaboration
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Neutrino oscillation experiments : Σmν ≳ 0.058 eV Inverted Hierarchy: two neutrinos with mν ≳ 0.058 eV, so Σmν ≳ 0.116 eV Assuming normal hierarchy and minimum value Σmν = 0.058 eV, SPT-3G could provide evidence against the inverted hierarchy. Assuming the inverted hierarchy, SPT-3G could rule out Σmν = 0 at 2 sigma .
Cosmological constraint on neutrino mass at level comparable to known lower limit (~60 meV) from oscillation experiments!
constraint : 𝜏(Σmν) ≅ 0.055 eV
+ Planck) constraint : 𝜏(Σmν) ≅ 0.06 eV
lensing + DESI BAO constraint : 𝜏(Σmν) ≅ 0.038 eV
Forecasted 30 % improvement over previous measurements!
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Neutrino oscillation experiments : Σmν ≳ 0.058 eV Inverted Hierarchy: two neutrinos with mν ≳ 0.058 eV, so Σmν ≳ 0.116 eV Assuming normal hierarchy and minimum value Σmν = 0.058 eV, SPT-3G could provide evidence against the inverted hierarchy. Assuming the inverted hierarchy, SPT-3G could rule out Σmν = 0 at 2 sigma .
Cosmological constraint on neutrino mass at level comparable to known lower limit (~60 meV) from oscillation experiments!
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SPT-3G : A great experiment for doing particle physics!
𝜏(Σmν) ≅ 0.038 eV ΔNeff = 0.1
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𝜏(Σmν) ≅ 0.038 eV ΔNeff = 0.1
SPT-3G : A great experiment for doing particle physics!
And other things too!
Constrain the H0 tension between CMB and supernovae methods Primordial gravitational waves
Time-variable mm-wave sky (blazars, AGN, GRB afterglows)
Constrain the dark energy equation of state
Galaxy Cluster physics
Evolution of early galaxies
Questions?
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Distance between objects Radiation dominated, w = 1/3 Matter dominated, w = 0 Comes from the solution to the Freidman Equations
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3.0, 2.2, and 8.8 µK-arcmin at 95, 150, and 220 GHz respectively
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