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
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
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Early-Universe Timeline
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
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 ,
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
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino density from BB photon density
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
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 !
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
CR Spectrum above a TeV
from Tom Gaisser
VLHC(100 TeV)2
50 Joules
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%
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
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
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)
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
The oscillation “box” from a Feynman graph
Where does the “mixing matrix” come in?
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>*
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
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 …
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?
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
0 decay limits on neutrino mass
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.
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
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Cosmic structure formation
WMAP 2dF/SDSS
*
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
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
WMAP data
The Universe at trecombination , ~ tequality
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
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
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.
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)
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.
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
A little HDM history
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino fits
Elgaroy and Lahav
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 ??
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Role of priors (Elgaroy and Kahav)
Elgaroy and Lahav
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Resonant Neutrino Annihilation Mean-Free-Path
Fig: Fargion, Mele, Salis
nDH/h70
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Escher’s “Angels and Devils”
The early Uni was denser, more absorbing.
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino mass-spectroscopy: absorption and emission
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Z-bursts
Mpc
TJW, 1982;Revival – 1997
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
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
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
The GZK puzzle
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Z-burst spectrum
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Fitted Z-burst (Emission) Flux
Gelmini, Varieschi, TJW
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Nu-mass limit for Z-burst fitted to EECRs
Gelmini, Varieschi, TJW
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
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
“clear moonless nights”
Blackout_14aug03.jpeg
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
See-saw (Leptogenesis to follow)
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)
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
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
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
The “Learned Plot”
Oscillation phase is. ( Lm2 / 4 E
Figureparameterizedby m2 / (eV)2
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
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)
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
AMANDA/IceCube event
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Flavor ratio Topology ratio Map
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Sensitivity of 1 flavor-projection to MNS parameters
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
pseudo-Dirac masses and cosmic neutrinos
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Z-burst schematic
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Neutrino Mass tomography in the Local Super-galactic Cluster
(Fodor, Katz, Ringwald)
SLAC Summer School 2004 Thomas J. Weiler, Vanderbilt University & CERN
Integrated Sachs-Wolfe effect