neutrino (mass) in cosmology
DESCRIPTION
Neutrino (Mass) in Cosmology. Thomas J. Weiler Vanderbilt University Nashville TN 37235, and CERN, Geneva, Switzerland. Early-Universe Timeline. Friedmann eqns, and energy partitions Omega. with “a” being the cosmic scale factor. So L behaves like a “matter” with 3p+ r < 0 !. - PowerPoint PPT PresentationTRANSCRIPT
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino (Mass) in Cosmology
Thomas J. Weiler
Vanderbilt UniversityNashville TN 37235,
and CERN, Geneva, Switzerland
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Early-Universe Timeline
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Friedmann eqns, and energy partitions Omega
So behaves like a “matter” with 3p+ < 0 !
Can relate (F1) parameters to today’s values to write
with “a” being the cosmic scale factor
Inflation and data OmegaK ~ 0
Omega=/crit,crit=6 protons/m3
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino Decoupling
Looking back, ’s last scattered at time t such that
DC ~ MeV, t ~ 1 s, z ~ 1010.
Coincidentally, TDC ~ TBBN ~ Te+e-vs. zeq = a0/aeq = Omegarad/Omegam ~ 4000, zrecomb ~ 1100.
Coincidentally, Teq~ Trecomb ~ eV ~ m
i.e. GF2 T5 ~ T2/MP ,
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino stat mech
HDM models tried (top-down)
Omega=1, i.e. each m~30eV
per flavor
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino density from BB photon density
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
n, n >> any other density
Rad
io
CM
B
Vis
ible
-ra
ys
CERN/Fermilab
x-ra
ysUV
IRCosmic-rays
TeV
-w
all
(after Ressell & Turner ‘90)
hadron wall?
no wall a’tall
sunSN87a NeutrinoIncognito
~CB
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino time
Liberated at T=Mev, t= 1 sec
Depends on energy (Lorentz boost)
Consider a 1020 eV neutrino.
Lorentz factor = 1021 for m = 0.1 eV.
Age of Uni is 1018 sec,
But age of is 1018/1021 sec = 1 millisecond !
And it doesn’t even see the stream of radiation rushing past it – untouched !
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
CR Spectrum above a TeV
from Tom Gaisser
VLHC(100 TeV)2
50 Joules
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
BBN limits on Nand asymmetry
Kneller & Steigman
Competing effects:1. Weak int’n rate equilibrates e+n p+e- , as n/p ~ exp[-mN/TDC] ;
So more e less neutrons less He/H2. Expansion rate (monotonic with N) decouples weak int’n;
So more N faster movie, earlier hotter TDC and more neutrons more He/H
H S H, S = So one extra species is S=0.08
Best fit is N=0.25, L=2.5%
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Compensation and LSND
Order 5% neutrino asymmetry -- to be contrasted with
10-9 baryon asymmetry
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Four roads to absolute neutrino mass(SN discounted)
1. Tritium decay
2. 0v decay
3. WMAP LSS
4. Z-bursts on the relic CB
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Tritium decay limits on neutrino massQ: Why tritium?A: It has a small Q-value, mT-(mD+mp+me)
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
The oscillation “box” from a Feynman graph
Where does the “mixing matrix” come in?
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
PMNS neutrino-mixing matrix
ijijijij
τττ
μμμ
eee
li
sandcwhere
cs
sc
iδecs
sccs
sc
UUU
UUU
UUU
U
sin,cos
0
010
0
00
010
001
0
0
001
100
0
0
1313
1313
2323
23231212
1212
321
321
321
Weak-interaction and mass “vectors” point differently:|nk>=Uki |ni>, or Uki = <ni | nk> = <nk | ni>*
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
e
Log m2
m1
m3
m2
m223 ~ 2.5 x 10-3 eV2
m212 ~ 7 x 10-5
eV2
It “probably” looks something like this
What we think we know about neutrino mass
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
e
Log m2
m1
m3
m2
It looks like this
m3
m2
m1
Or maybe …
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Naturalness may be over-rated
Or a bug with a light-emitting tush?
A rodent with a bill?Do these look natural?
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
0 decay limits on neutrino mass
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino parameters: fundamental to physics, and
a tool for astrophysics/cosmology
As an astro tool, useful NOW(e.g. Le = L = L ) ;
As a physics window, the view is unclear.
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
second task:decide whether contributeas Hot Dark Matter
[% of cr]
neutrino masses and cosmologyneutrino masses and cosmology
first task: bound mass
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Cosmic structure formation
WMAP 2dF/SDSS
*
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
COBE data
*The raw temperature map (top) has a large diagonal asymmetry due to our motion with respect to the cosmic microwave background -a Doppler shift.
*The temperature fluctuations after subtraction of the velocity contribution, showing primordial fluctuations and a large radio signal from nearby sources in our own galaxy (the horizontal strip).
*The primordial fluctuations after subtraction of the galaxy signal.
V
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
WMAP data
The Universe at trecombination , ~ tequality
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
2dF Galaxy Redshift Survey
Peak from horizon scale at teq
HDM contributes to suppression ofSmall scales
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Today k >
knr ~ (Omega/Omegam)1/2 Omegam
New length scale from neutrino mass
LSS WMAP
LSS formation is a battle between attractive gravity and repulsive pressure;
the battle-line is the “Jean’s length” (4G/vs2)1/2 ~ (4G/p)1/2 . The
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Thomas J. Weiler, Vanderbilt University & CERNSLAC Summer School 2004
Tegmark cosmic cinema - CDMhttp://www.hep.upenn.edu/~max/cmb/movies.html
Increasing the total density of matter (baryons + cold dark matter) pushes the epoch of matter-radiation equality back in time and moves the peak scale (the horizion size at that time) to the right.
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Thomas J. Weiler, Vanderbilt University & CERNSLAC Summer School 2004
Tegmark cosmic cinema - HDM
Increasing the density of massive neutrinos suppresses all scales smaller than a certain cutoff, which in turn shifts to the left as you increase the neutrino mass (and density)
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Thomas J. Weiler, Vanderbilt University & CERNSLAC Summer School 2004
Tegmark cosmic cinema – more HDM
If a CMB theorist gloats that he or she can measure the neutrino density, make sure to point out that galaxy surveys are much more sensitive.
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
A little HDM history
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino fits
Elgaroy and Lahav
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
SDSS (Seljak et al)
Increasing nu mass increases CMB spectrum,But decreases matter power spectrum ??
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Role of priors (Elgaroy and Kahav)
Elgaroy and Lahav
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Resonant Neutrino Annihilation Mean-Free-Path
Fig: Fargion, Mele, Salis
nDH/h70
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Escher’s “Angels and Devils”
The early Uni was denser, more absorbing.
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino mass-spectroscopy: absorption and emission
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Z-bursts
Mpc
TJW, 1982;Revival – 1997
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
-mass spectroscopyzmax=2, 5, 20 (top to bottom), n-=2(bottom-up acceleration)Eberle, Ringwald, Song, TJW, 2004
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Dips & sobering realism
hidden MX=4 1014 and 1016 GeV, to explain >GZK w/ Z-bursts;
mass = 0.2 (0.4) eV - dashed (solid);Error bars – per energy decade, by 2013,
for flux saturating present limits
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
The GZK puzzle
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Z-burst spectrum
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Fitted Z-burst (Emission) Flux
Gelmini, Varieschi, TJW
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Nu-mass limit for Z-burst fitted to EECRs
Gelmini, Varieschi, TJW
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Size mattersEUSO ~ 300 x AGASA ~ 10 x AugerEUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger
Exposure
1
10
100
1000
10000
Year
Expo
sure AGASA
HiResAugerEUSO
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
“clear moonless nights”
Blackout_14aug03.jpeg
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
See-saw (Leptogenesis to follow)
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Leptogenesis
Three Sakharov conditions for Violate baryon number (B-L conserved => Baryogenesis:
. B (=L) nonzero
2. Violate C and CP T (complex couplings)
3. Out of Thermal Equilibrium
(decouple at T > M so no Boltzmann suppression,
then decay at T < M when over-abundant)
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Extra-dimensions and neutrino mass
Right-handed “sterile” neutrinos may be our probe of extra-dimensions
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Summary:
Neutrinos are a splendid example of the interplay among particle physics,
astrophysics, and cosmology
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
The “Learned Plot”
Oscillation phase is. ( Lm2 / 4 E
Figureparameterizedby m2 / (eV)2
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino Decay -- Models, Signatures, and Reach
P(survive)= e –t/ = e –(L/E)(m/0
)
Beacom, Bell, Hooper, Pakvasa, TJW
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
The cosmic flavor-mixing thm
If theta32 is maximal (it is),And if Re(Ue3) is minimal (it is),
Then and equilibrate;
Further, if initial e flux is 1/3
(as from pion-muon decay chain),Then all three flavors equilibrate. e:: = 1 : 1 : 1 at Earth
(and deviations new physics)
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
AMANDA/IceCube event
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Flavor ratio Topology ratio Map
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Sensitivity of 1 flavor-projection to MNS parameters
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
pseudo-Dirac masses and cosmic neutrinos
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Z-burst schematic
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino Mass tomography in the Local Super-galactic Cluster
(Fodor, Katz, Ringwald)
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SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Integrated Sachs-Wolfe effect