the cmb and neutrinos. we can all measure the cmb t cmb =2.725 +\- 0.001 k cmb approx 1% of tv...
TRANSCRIPT
The CMB and Neutrinos
We can all measure the CMB
TCMB=2.725 +\- 0.001 K
CMB approx 1% of TV noise!
400 photons/cc at 0.28 eV/cc
But no one has measured the neutrino background.
Neutrinos
Tn=1.945 K 3 known families, ~equal numbers of neutrinos and antineutrinos.
113 neutrinos/cc/family
When I say “neutrinos”….
0.05 eV<Smn<2.3 eV (95%cl)From atmospheric neutrinos at SuperK , nm nt
Tritium end point plus mass splittings. (Kraus et al., 2005)
From particle physics:
Neutrinos
Tn=1.945 K 3 known families, ~equal numbers of neutrinos and antineutrinos.
113 neutrinos/cc/family
0.05 eV<Smn<1.2 eV (95%cl)
WMAP aloneFrom atmospheric neutrinos at SuperK , nm nt
Neutrinos
Tn=1.945 K 3 known families, ~equal numbers of neutrinos and antineutrinos.
113 neutrinos/cc/family
0.05 eV<Smn<0.58 eV (95%cl)From atmospheric neutrinos at SuperK , nm nt
WMAP+BAO+H0
Neutrinos
Tn=1.945 K 3 known families, ~equal numbers of neutrinos and antineutrinos.
113 neutrinos/cc/family
0.05 eV<Smn<0.2 eV (95%cl)From atmospheric neutrinos at SuperK , nm nt
Expected from KATRIN (Franenkel, 2011)
Neutrinos
Tn=1.945 K 3 known families, ~equal numbers of neutrinos and antineutrinos.
113 neutrinos/cc/family
0.05 eV<Smn<0.06 eV (~95%cl)From atmospheric neutrinos at SuperK , nm nt
From Planck plus fine scale CMB polarization measurements (ACT, SPT….)
Cosmic Evolution
Us
Decoupling at z=1030
Decoupling surface
Cosmic Evolution
Cosmic Evolution
Cosmic Evolution
At decoupling
1972
WMAP at 61 GHz, 0.5 cm
The CMB at decoupling as seen through a Lambda-dominated spacetime (and through our galaxy).
Angular Power
Fundamental mode
rarefaction compression
“Acoustic peaks”
Model
compression
Spectrum
Silk damping tail
The Atacama Cosmology Telescope
~10X WMAP resolution
WMAP
148
GH
z21
8 G
Hz
277
GH
z
Pulse Tube
4He Fridge
3He Fridge
40K Shield
3K Shield
Window
1 m
DetectorsOptics
The Millimeter Bolometric Array Camera
Preliminary Power Spectrum
Silk damping tail
Number of relativistic species, NeffDunkley et al., 2011
The key to limiting Neff is to identify the increased damping at small angular scales in the CMB.
Silk damping tail
Hou et al., 2011Bashinsky & Seljak, 2004Jungman, Kamionkowski, Kosowsky, Spergel 1996
Neff
ACT+WMAP
ACT+WMAP+BAO+H0
Dunkley et al., 2011
WMAP
SPT+WMAP
SPT+WMAP+BAO+H0
Keisler et al., 2011
Komatsu et al., 2011
5.3 +/- 1.3
4.56 +/- 0.75
3.85 +/- 0.62
3.86 +/- 0.42
Compare today to that at decoupling. Greater relativistic means smaller rm/rr, enhanced potential evolution, and producing less cosmic structure.
Komatsu et al., 2009
e.g., Ichikawa et al., 2005
WMAP+BAO+SN, sum <0.58 (95%cl)
WMAP
Neutrino Mass #1
Neutrino Mass #2
Use the cosmic structure between us and the surface of last
scattering to lens the CMB, especially the small angles where
a massive neutrino inhibits the formation of structure.
Lensing is characteristically sensitive to mn
From Sudeep Das
Lensing smoothes out the peaks and alters the statistics of the CMB
Simulations
AAS, Jan 7 2010100 deg2
uK
AAS, Jan 7 2010
Simulations
100 deg2
uK
Lensing of CMB detected at 4s
Based on Hu & Okamoto estimator plus phase randomization.
Shape sensitive to neutrino mass.
And from SPT
van Engelen et al 2012
“Geometric Degeneracy”
CMB alone tells us we are on the “geometric degeneracy” line
closed
open
Assume flatness
WMAP7 only best fit LCDM
{Wbh2 = 0.0226 +/- 0.00057Wch2 = 0.1109 +/- 0.0056 h = 0.710 +/- 0.025 s8 = 0.801 +/- 0.030 t = 0.088 +/- 0.015 ns = 0.963 +/- 0.014
The Degeneracy
Sherwin et al. 2011
Lensing breaks the geometric degeneracy.
Lambda=0 excluded at 3.2 sigma from combination of WMAP and ACT.
Sherwin et al. 2011
Neutrino Mass #3
AAS, Jan 7 2010
Planck: sensitive to l=2000 in polarization
Can look through foregrounds in EE at l>2000.
Instruments & measurements underway by ACTPol, Polar, Polarbear, SPTPol.
Gravitational lensing turns E-modes into B-modes. Look for the effects of neutrinos in polarization.
Thank You