Neutrino (Mass) in Cosmology

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


Early-Universe Timeline

http://www.pbs.org/deepspace/tlbigbang.gif.map

http://www.pbs.org/deepspace/timeline/tl6.html







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


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 ,


Neutrino stat mech

HDM models tried (top-down)

Omega=1, i.e. each m~30eV

per flavor


Neutrino density from BB photon density


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


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 !


CR Spectrum above a TeV

from Tom Gaisser

VLHC(100 TeV)2

50 Joules


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%


Compensation and LSND

Order 5% neutrino asymmetry -- to be contrasted with

10-9 baryon asymmetry


Four roads to absolute neutrino mass(SN discounted)

1. Tritium decay

2. 0v decay

3. WMAP LSS

4. Z-bursts on the relic CB


Tritium decay limits on neutrino massQ: Why tritium?A: It has a small Q-value, mT-(mD+mp+me)


The oscillation “box” from a Feynman graph

Where does the “mixing matrix” come in?


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>*


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


e

Log m2

m1

m3

m2

It looks like this

m3

m2

m1

Or maybe …


Naturalness may be over-rated

Or a bug with a light-emitting tush?

A rodent with a bill?Do these look natural?


0 decay limits on neutrino mass


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.


second task:decide whether contributeas Hot Dark Matter

[% of cr]

neutrino masses and cosmologyneutrino masses and cosmology

first task: bound mass


Cosmic structure formation

WMAP 2dF/SDSS

*


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

http://www.damtp.cam.ac.uk/user/gr/public/images/cmbr_DMR.gif

http://www.pbs.org/deepspace/tlfuture.gif.map





http://www.damtp.cam.ac.uk/user/gr/public/images/cmbr_DMR.gif


WMAP data

The Universe at trecombination , ~ tequality

http://map.gsfc.nasa.gov/m_ig/030628/030628B_s.jpg

http://map.gsfc.nasa.gov/m_ig/030628/030628B_s.jpg


2dF Galaxy Redshift Survey

Peak from horizon scale at teq

HDM contributes to suppression ofSmall scales


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.


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)


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.


A little HDM history


Neutrino fits

Elgaroy and Lahav


SDSS (Seljak et al)

Increasing nu mass increases CMB spectrum,But decreases matter power spectrum ??


Role of priors (Elgaroy and Kahav)

Elgaroy and Lahav


Resonant Neutrino Annihilation Mean-Free-Path

Fig: Fargion, Mele, Salis

nDH/h70


Escher’s “Angels and Devils”

The early Uni was denser, more absorbing.


Neutrino mass-spectroscopy: absorption and emission


Z-bursts

Mpc

TJW, 1982;Revival – 1997


-mass spectroscopyzmax=2, 5, 20 (top to bottom), n-=2(bottom-up acceleration)Eberle, Ringwald, Song, TJW, 2004


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


The GZK puzzle


Z-burst spectrum


Fitted Z-burst (Emission) Flux

Gelmini, Varieschi, TJW


Nu-mass limit for Z-burst fitted to EECRs

Gelmini, Varieschi, TJW


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


“clear moonless nights”

Blackout_14aug03.jpeg


See-saw (Leptogenesis to follow)


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)


Extra-dimensions and neutrino mass

Right-handed “sterile” neutrinos may be our probe of extra-dimensions


Summary:

Neutrinos are a splendid example of the interplay among particle physics,

astrophysics, and cosmology


The “Learned Plot”

Oscillation phase is. ( Lm2 / 4 E

Figureparameterizedby m2 / (eV)2


Neutrino Decay -- Models, Signatures, and Reach

P(survive)= e –t/ = e –(L/E)(m/0

)

Beacom, Bell, Hooper, Pakvasa, TJW


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)


AMANDA/IceCube event


Flavor ratio Topology ratio Map


Sensitivity of 1 flavor-projection to MNS parameters


pseudo-Dirac masses and cosmic neutrinos


Z-burst schematic


Neutrino Mass tomography in the Local Super-galactic Cluster

(Fodor, Katz, Ringwald)


Integrated Sachs-Wolfe effect

Neutrino (Mass) in Cosmology

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