Ou Outl tlin ine Introduction The standard 3 framework - - PowerPoint PPT Presentation

XLIV Rencontres de Moriond EW

Neutrino data and implications for θ13 Antonio Palazzo

CSIC/IFIC, AHEP group, Valencia

March 13, 2009 Based on work done in collaboration with: G.L. Fogli, E. Lisi, A. Marrone, A.M. Rotunno

1

Ou Outl tlin ine

Re-charting a familiar territory The leading mass-mixing parameters Exploring an uncharted land Hints of non-zero θ13 Introduction The standard 3ν framework Future perspectives and conclusions

2

The standard 3ν framework

3

Dirac CP-violating phase

The l he leptonic m c mix ixin ing

unknown

Explicit form:

4

ν1

NH NH IH IH

ν2 ν3 ν3

The n he neu eutr trin ino ma

• mass sp

ss spectr trum

?

+Δm2 δm2

• Δm2

ν1 ν2 sub-e sub-eV

5

Ex Experim imen ental Sensi l Sensitivi vitie ies

Solar, KamLAND Atmospheric, LBL (disapp) CHOOZ, MINOS (app)

sub-l sub-lea eadin ding lea eadin ding

“fixed” by Atm + LBL

6

Precision quickly increasing after each new MINOS data release Still dominated by Atm. data Improvement expected from MINOS

Fogli et al., Phys. ReV. D 78, 033010 (2008) [arXiv:0805.2517v3]

The l he lea eadin ding g “a “atmo mosphe spheric” c” pa param ameters

7

Sol Solar r ν da data c a consis nsisten ent w t with MSW tr th MSW tran ansi sitio ions

“LMA LMA ”

8

Sp Spectacu cularly c y confir nfirmed b d by KamLAND y KamLAND

• Osc. pattern observed
• ver one entire cycle

Determina inatio ion of n of δm2 with h th hig igh p h precisio cision Precisio cision m n mea easu surem emen ent

• f sp
• f spectr

tral dis l distortio ions ns

2008 Results

9

2ν Sol Solar + KamLAND c KamLAND cons nstr train aints

KamLAND do KamLAND domina inates δm2 de determina inatio ion In Interpl play of y of Sol Solar an r and KamLAND d KamLAND in de in determin inin ing θ12 Bu But sma t small t l tensio ension amo among them is p g them is presen sent

10

Fogli et al., Phys. ReV. D 78, 033010 (2008) [arXiv:0805.2517v3]

The l he lea eadin ding g “sol solar” r” pa param ameters

Er Errors a s are l e lin inea ear, p , precisio cision e n era n a now en w entered

11

G.L Fogli, E. Lisi, A. Marrone, A.P., A.M. Rotunno arXiv:0806.2649 [hep-ph] PRL 101, 141801 (2008)

12

CHOO CHOOZ an Z and 3 d 3ν gl glob

• bal ana

l analyse yses: In Interpl play in pinn y in pinnin ing do g down n θ13

13

SK + LBL

CHOOZ Excluded

They seem capable to go beyond

the CHOOZ sensitivity

3ν global analyses have

first corroborated & then strengthened

the CHOOZ upper bound

In the past Now

13

The he “old

• ld” hin

int t fr from a m atmo mosphe spheric da c data

14

wea weak ( k (~1 1 sigma sigma) p ) preferenc ence f e for r θ13

13>0

>0

A possible source:

excess of sub-GeV electron-like events partially explained by 3ν subleading effects driven by the “solar” splitting δm2

G.L. Fogli, E. Lisi, A. Marrone, A.P., Prog. Part. Nucl. Phys. 57, 742 (2006)

In the past this “hint” was not corroborated by solar & KamLAND, which systematically preferred θ13 = 0

Bu But suc t such a tr h a tren end ha d has r recen entl tly c y chan hanged… d…

15

The n he new h ew hin int fr t from sol solar + KamLAND r + KamLAND

16

Sol Solar r ν da data: fr a: from 20 m 2005 t 05 to 20

• 2008

08

SNO SNO-III

• III
• Cen
• Centr

tral v l value l ue lowe wer than be r than before

• Er
• Error r

r reduc duced w d when c hen combin mbined d be best fit of t fit of θ12 at a sl t a slig ightl tly l y lowe wer v r value ue ran ange a e allowe wed f d for r θ12 app ppreci ciabl bly na y narrowe wed (now w ~ sym symmetr tric) )

SNO SNO-II

• II

20 2005 05

20 2008 08

appa pparen entl tly y a sma a small c l chan hange! e!

17

…b …but big en t big enoug ugh t h to g

• give r

e rise t ise to

a t a tensio ension w n with KamLAND… th KamLAND…

Solar and KamLAND

prefer different values of θ12

12

No overlap at 1σ level Solar prefer higher θ12

12

KamLAND prefers lower θ12

12

Disagreement reduced*

*See also Balantekin and Yilmaz, J. Phys. G. 35, 075007 (2008)

…w …which, ho h, howe wever, c can be a an be allevi viated f d for r θ13>0 >0

18

θ13

13 >

> 0 θ13

13 =

= 0

In Interpl play of Sol y of Solar an r and KamLAND d KamLAND

~1.2σ preference for θ13 > 0

19

Co Compa mpariso ison w n with o th othe ther e r exis istin ing ana g analyse yses

Sc Schwe hwetz tz, , Tortol

• la,

a, Valle, a , arXi rXiv:0808. v:0808.201 2016 6

preference for θ13>0 found at a slightly higher CL (~1.5 sigma) Co Consensu nsensus o s on the n the the sol+k the sol+kam h am hin int t

20

The gl he glob

• bal h

l hin int t

Co Combin mbinin ing a g all da l data we fin we find an o d an overall l preferenc ence f e for r θ13

13>0 a

>0 at t 1.6 sigma (90% CL)

21

Solar and Kamland prefer θ13>0

• nly in combination:

synergy

Status of the electron neutrino mixing

~ 0.307 ~ 0.667 ~ 0.016 22

27 27th

th F

Feb 20 b 2009 09, a n a new h ew hin int fr t from MINOS m MINOS νe a app ppea earanc ance ? e ?

By courtesy of M. Sanchez

θ13

13 = 0

disf disfavored a d at t ~ 90% 90% Ho Howe wever, c , combin mbinin ing g their r their resu sults w ts with o th ours… s…

23

The Col he Collabo boratio ion, , conse nservativel ely, , do does n s not a t attach an h any pa y particu cular r rel elevanc ance t e to th

• this f

is fact

0.9 σ

σ

1.2 σ

σ

1.6 σ

Hint 1σ range

St Statu tus a s as of Ma s of March 20 h 2009 09

~ 2 σ σ

24

…an o …an overall h l hin int a t at 2 sigma l t 2 sigma level em el emerges

Fu Futu ture p e persp spectives

25

MINOS SNO Atm.

Re Resu sults w ts with do th doubl uble s e statis istics e cs expected so d soon.

• n. See t

See talk b lk by M. y M. Sanche Sanchez. z.

• Lo

Low en w energy thr y threshold ana shold analysis (LET ysis (LETA) u ) unde derwa

• way. Incr

Increa ease sed NC s d NC statis istics cs. See t See talk b lk by y A. McDo McDona nald, a ld, at N t Neu eutr trin ino

• Tel

elescopes 20 s 2009 09.

• A c

A compl mplete 3 e 3ν ana analysis inc ysis includin ding g subl sublea eadin ding e effects in ts induc duced b d by y “sol solar r pa param ameters” is e is expected fr d from the SK c m the SK col

• llabo

boratio ion.

• n. See t

See talk b lk by M. y M. Nakaha ahata a at N t Neu eutr trin ino

• Tel

elescopes 20 s 2009 09.

• Fir

First da t data, u a, usin sing a sin g a singl gle de e detector, t , to be c

• be col
• llected be

d before the en e the end of d of th this y is yea

• ear. Fir

First r t resu sults c ts could be e ld be expected b d by the su y the summer of 2010 r of 2010.

• D-CHOOZ

Fir First r t resu sults e ts expected in 2011 d in 2011

Daya-Bay

New relevant information expected from:

New da ew data e a expected.

• d. Fu

Furthe thermo more, i , it ha t has been n s been noted tha d that in a m t in a multi-r i-rea eactor se setu tup o p one e e expects pa ts partial c l canc ancel ellatio ions of r ns of ran ando dom dis m distr trib ibuted e d errors s (Dju (Djurci cic e c et a t al., 0808.07 ., 0808.0747 [ 7 [he hep-e p-exp]). ]). P Possibl ssible impa e impact o t on the of n the of “S+K h S+K hin int”. t”.

KamLAND

26

θ13>0

confirmed

Strong

upper bound

?

S S K K K

Wha hat we ma t we may e y expect fr t from m Sol Solar an r and KamLAND d KamLAND

S

Hint of new physics?

27

Wha hat we ma t we may e y expect fr t from m rea eactor an r and a d accel elerator e r exp.

Adapted from Huber et. al JHEP 0605, 072 (2006) * Global analysis 2009 Global analysis 2009 28

1σ 1σ

Co Conc nclusio sions ns

• All da

l data fit w a fit with thin the s in the stan anda dard 3 d 3ν fr fram amew ework k

• Gl
• Glob
• bal h

l hin int n t now a w at the 2 sigma l t the 2 sigma level (95% C el (95% C.L.) .L.)

• Further data needed to clarify the issue
• If the trend persists:
• Thr

hree in ee inde depen enden dent h t hin ints of ts of θ13

13>0

>0 In the near future (~2 years) it is conceivable to envisage a scenario with several concurrent hints, each unable to provide decisive indication.

29

Ba Back-u k-up sl p slide des

30

3ν ana

analysis inc ysis includin ding sub-l g sub-lea eadin ding LMA e g LMA effects ts

G.L. Fogli, E. Lisi, A. Marrone, A.P., Prog. Part. Nucl. Phys. 57, 742 (2006) 31

“θ13 term” “δm2 term”

Constant density approximation

Excess of electron events induced by 3ν subleading effects

zero when both θ13=0 & δm2 = 0 “Interference term” *

multi-GeV sub-GeV

*O.L.G Peres and A.Yu. Smirnov , Nucl. Phys. B 456, 204 (1999); ibidem 680, 479 (2004)

32

Mixing angles in matter Order of magnitude

• f the potential

Expressions valid for

:

“Swapping” relations

33

Exact numerical examples

“θ13 term” dominant “δm2 term” dominant “Interference term” dominant (only in sub-GeV)

Fogli et al., Prog. Part. Nucl. Phys. 57, 742 (2006)

34

35

Model-independent consistency checks

SNO-II (2005) SNO-III (2008)

bo both a th alr lrea eady g y good …an d …and… n d… now e w even be en better r 1) “internal” consistency among SNO (CC,NC) and SK (ES) 2) consistency among NC measurement and Solar Model

36

Hig High-E sol h-E solar r (adi diabatic MSW) c MSW) KamLAND KamLAND (vacuu cuum) Di Differen ent r t rel elative sig e sign f n for ( r (θ12

12,

, θ13

13) in P

) in Pee

ee

• f Sol
• f Solar (h

r (hig igh-E do h-E domina inated) vs KamLAND d) vs KamLAND

Or Orig igin of the di in of the differen ent c t correl elatio ions ns +

• scil

cillatio ion pha n phase se

37

Sol Solar r ν’s p s probe tw

• be two di
• differen

ent r t reg egim imes

Hig High-E h-E

ma matter do domina inated

Low-E beha behavio vior is sim r is simil ilar t r to tha

• that p

t probe

• bed in KamLAND

d in KamLAND, so , so we e we expect an ana t an analogous c s compl mplem emen entarity of h ty of hig igh-E an h-E and ( d (fu futu ture) l ) low-E

• E

+

• Lo

Low-E

• E

averaged “v “vacuu cuum-l

• lik

ike”

• 38

Goswami and Smirnov, PRD 72, 053011 (2005)

Lo Low-E

• E

Hig High-E h-E (Bo (Borexin ino) (SNO SNO)

“Co Contr trastin ing” g” l low-E w

• E with h

th hig igh-E da h-E data a

39