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

XLIV Rencontres de Moriond EW March 13, 2009 Neutrino data and implications for θ 1 3 � Antonio Palazzo CSIC/IFIC, AHEP group, Valencia Based on work done in collaboration with : � G.L. Fogli, E. Lisi, A. Marrone, A.M. Rotunno 1

Ou Outl tlin ine � Introduction � The standard 3 ν framework � Re-charting a familiar territory � The leading mass-mixing parameters � Exploring an uncharted land � Hints of non-zero θ 13 � Future perspectives and conclusions � 2

The standard 3 ν framework � 3

The l he leptonic m c mix ixin ing � Dirac CP-violating phase unknown Explicit form: 4

The n he neu eutr trin ino ma o mass sp ss spectr trum � ? NH � NH IH � IH ν 3 + Δ m 2 ν 2 ν 2 δ m 2 ν 1 ν 1 - Δ m 2 sub-e sub-eV � ν 3 5

Experim Ex imen ental Sensi l Sensitivi vitie ies � lea eadin ding � Atmospheric, LBL (disapp) sub-lea sub-l eadin ding � Solar, KamLAND CHOOZ, MINOS (app) “fixed” by Atm + LBL � 6

The l he lea eadin ding g “a “atmo mosphe spheric” c” pa param ameters � Still dominated by Atm. data � Precision quickly increasing � Improvement expected � after each new � from MINOS � MINOS data release � 7 Fogli et al., Phys. ReV. D 78, 033010 (2008) [arXiv:0805.2517v3]

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

Spectacu Sp cularly c y confir nfirmed b d by KamLAND y KamLAND � 2008 Results Precisio cision m n mea easu surem emen ent � of sp of spectr tral dis l distortio ions ns � Osc. pattern observed � over one entire cycle � Determina inatio ion of n of δ m 2 � with h th hig igh p h precisio cision � 9

Solar + KamLAND c 2 ν Sol KamLAND cons nstr train aints � KamLAND do KamLAND domina inates � δ m 2 de determina inatio ion � In Interpl play of y of � Solar an Sol r and KamLAND d KamLAND � in de in determin inin ing θ 12 � Bu But sma t small t l tensio ension � amo among them is p g them is presen sent 10

The l he lea eadin ding g “sol solar” r” pa param ameters � Errors a Er s are l e lin inea ear, p , precisio cision e n era n a now en w entered � 11 Fogli et al., Phys. ReV. D 78, 033010 (2008) [arXiv:0805.2517v3]

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 3 ν gl glob obal ana l analyse yses: � In Interpl play in pinn y in pinnin ing do g down n θ 13 13 � In the past CHOOZ Excluded 3 ν global analyses have � first corroborated & then strengthened the CHOOZ upper bound � Now They seem capable to � go beyond the CHOOZ sensitivity � SK + LBL 13

he “ old old ” hin The int t � fr from a m atmo mosphe spheric da c data � 14

k ( ~ 1 wea weak ( 1 sigma sigma) p ) preferenc ence f e for r θ 13 13 >0 >0 � A possible source: excess of sub-GeV � electron-like events � partially explained by � 3 ν subleading effects � driven by the � “ solar ” splitting δ m 2 � In the past this “hint” � was not corroborated � by solar & KamLAND, � which systematically � preferred θ 13 = 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 G.L. Fogli, E. Lisi, A. Marrone, A.P., Prog. Part. Nucl. Phys. 57, 742 (2006) �

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 o 2008 08 � 20 2005 05 � 20 2008 08 � SNO SNO-II -II � SNO SNO-III -III � - Cen - Centr tral v l value l ue lowe wer than be r than before � be best fit of t fit of θ 12 � at a sl t a slig ightl tly l y lowe wer v r value ue � - Error r - Er r reduc duced w d when c hen combin mbined d � ran ange a e allowe wed f d for r θ 12 � app ppreci ciabl bly na y narrowe wed � w ~ sym (now symmetr tric) ) � 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 o give r e rise t ise to o � …w …which, ho h, howe wever, � a tensio a t ension w n with KamLAND… th KamLAND… � can be a c an be allevi viated f d for r θ 1 3 >0 >0 � = 0 θ 13 13 = > 0 θ 13 13 > Solar and KamLAND Solar prefer higher θ 12 12 prefer different values of θ 12 KamLAND prefers lower θ 12 12 12 No overlap at 1 σ level Disagreement reduced* 18 *See also Balantekin and Yilmaz, J. Phys. G. 35, 075007 (2008)

In Interpl play of Sol y of Solar an r and KamLAND d KamLAND � ~1.2 σ preference for θ 13 > 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 ola, a, Valle, a , arXi rXiv:0808. v:0808.201 2016 6 � preference for θ 13 >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 obal 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 θ 13 13 >0 a >0 at t � 1.6 sigma (90% CL) Solar and Kamland � prefer θ 13 >0 � only in combination: � synergy � 21

Status of the electron neutrino mixing ~ 0.667 ~ 0.307 ~ 0.016 22

27 27 th th F Feb 20 b 2009 09, � a n a new h ew hin int fr t from MINOS m MINOS ν e a app ppea earanc ance ? e ? � 13 = 0 � θ 13 t ~ 90% disf disfavored a d at 90% � The Col he Collabo boratio ion, , � conse nservativel ely, , � does n do s not a t attach an h any pa y particu cular � r rel elevanc ance t e to th o this f is fact � Howe Ho wever, c , combin mbinin ing g � their resu their r sults w ts with o th ours… s… � By courtesy of M. Sanchez � 23

…an o …an overall h l hin int a t at 2 sigma l t 2 sigma level em el emerges � St Statu tus a s as of Ma s of March 20 h 2009 09 � Hint 1 σ range 0.9 σ σ 1.2 σ σ 1.6 σ ~ 2 σ σ 24

Fu Futu ture p e persp spectives � 25

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 KamLAND 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 (Djurci (Dju 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”. � Low en Lo 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. SNO See t See talk b lk by y A. McDo McDona nald, a ld, at N t Neu eutr trin ino o Tel elescopes 20 s 2009 09. � A c A compl mplete 3 e 3 ν ana analysis inc ysis includin ding g subl sublea eadin ding e effects in ts induc duced b d by y “sol solar r Atm. pa param ameters” is e is expected fr d from the SK c m the SK col ollabo boratio ion. n. See t See talk b lk by M. y M. Nakaha ahata a at N t Neu eutr trin ino o Tel elescopes 20 s 2009 09. � MINOS 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. � Fir First da t data, u a, usin sing a sin g a singl gle de e detector, t , to be c o be col ollected be d before the en e the end of d of � D-CHOOZ 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. � Daya-Bay Fir First r t resu sults e ts expected in 2011 d in 2011 � 26

Wha hat we ma t we may e y expect fr t from m � Solar an Sol r and KamLAND d KamLAND � Strong Hint of θ 13 >0 upper bound new physics? confirmed K S K S K S ? 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. � * 1 σ 1 σ Global Global analysis analysis 2009 2009 Adapted from Huber et. al JHEP 0605, 072 (2006) � 28

Co Conc nclusio sions ns � - All da l data fit w a fit with thin the s in the stan anda dard 3 d 3 ν fr fram amew ework k � >0 - Thr - hree in ee inde depen enden dent h t hin ints of ts of θ 13 13 >0 - Glob - Gl obal 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: � 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

3 ν ana analysis inc ysis includin ding sub-l g sub-lea eadin ding LMA e g LMA effects ts � 31 G.L. Fogli, E. Lisi, A. Marrone, A.P., Prog. Part. Nucl. Phys. 57, 742 (2006) �