supernova neutrinos - fermilab · 3 θ 13 sin2 2θ 13
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SUPERNOVANEUTRINOSATFUTUREDETECTORS
CeciliaLunardini
ArizonaStateUniversity
RIKENBNLResearchCenter
RecontresdeBlois,June2011
20+yearsback:theimpactofSN1987A
Whatdidwelearn?
TheonlySNneutrinodata
Plot from: http://astro.berkeley.edu/~bmetzger/sn1987a.html
February 23, 1987: SN1987A
• ~ 1 Kt water/scintillator detectors – Inversebetadecay:anP‐νe+pn+e+
Biontaetal.,PRL58,1987,Hirataetal.,PRL58,1987,Alekseevetal.JETPLeV.45(1987)
FirstconfirmaPonoftheory
• Luminosity≈totalenergybudget– EnergyemiVedisofgravita-onalnature:
Lν≈GM2f/Rf–GM2
i/Ri~31053ergs✓(Rf~10Km)
• Energyspectrum:~FermiDirac(thermal)– E≈3.15T~15‐20MeV✓
• DuraPonofneutrinoburst~diffusionPme– Time≈(size2)/(meanfreepath)~10s✓
OpenquesPons
• Precision?– Timestructure(accrePon,cooling,)– OscillaPons(MSW,neutrino‐neutrino,..)– ModeldiscriminaPon(Eq.ofstate,neutrinotransport,…)
– Newphysics• Totalenergy?
– Allneutrinospecies• Whatistypical?
ThesituaPonnow:openinganewphase
Newfocusonsupernovae
• Solar,atmosphericfluxesdowntoprecisionphase(~10‐40%)– Timetoapproachmoredistant,morecomplexsources:supernovae,GRBs,DarkMaVer,…• Solar/atmosphericbecomebackgrounds!
• Newphaseofdetectorscoming– Larger(0.1–1Mt)&moresensiPve
ThenextgeneraPon
WaterCherenkov,0.3‐1MtHyperK,UNO,MEMPHYS,DeepTITAND
LiquidArgon,10‐100ktLANNDD,GLACIER
Liquidscin-llator,10‐50ktLENA,HanoHano
LANNDD
DUSEL
• Complementarydesigns:– Forneutrinochannel:He+Pb(HALO)
– Forall‐flavor:noblegasTPC(NOSTOS)
– Forluminosity:Km3ice/water(IceCUBE)
Giomataris & Vergados, Phys.Lett.B634,2006
http://www.snolab.ca/halo/detailedPhysics.html
IceCUBE coll. , arXiv:0908.0441
Lookingfarther…
• 1‐5Mtmass– ~fewMpcreach~1SNeverydecade!
Ando,Beacom&Yuksel,PRL95,2005
…andinmoredetailEventsforGalac=cSN(K.Scholberg,talkatNeutrino2006,SanteFe,NM)
Themesforthefuture:whatwillwelearn?
Timing Pons et al., Phys.Rev.Lett.86,2001
• LatePmeevoluPon(>10s)– newphasesofmaVer(quarkmaVer,…)
– BlackholeformaPon
– TransiPontotransparency(Eq.ofstate)
normal quark
• <1s:SASI(StandingAccrePonShockInstability)– OscillaPonsofshockfrontmodulatesneutrinoluminosity
– ProbeslargescaleconvecPon
Blondin,Mezzacappa&DeMarino,ApJ584Marek,Janka&Mueller,Astron.Astrophys.496,475(2009)T.Lund,A.Marek.C.L.,H.T.Janka&G.Raffelt,arXiv:1006.1889
νesensiPvity
Detectortype process Expectedmass Numberofevents(galac=cSN)
WaterCherenkov
νe(16O,16F)e‐ ~1Mt O(103)
LiquidArgon νe(40Ar,40K)e‐ <100Kt <O(103)
ScinPllator νe(12C,12B)e‐ <50kt <O(102)
Whyareνeimportant?
Duanetal.,PRL.100,2008C.L.,B.Mueller,H.T.JankaPRD,2008
• TotalenergyofSN– Eq.ofstate
• NeutronizaPon/deleptonizaPon– e‐(p,n)νe
• OscillaPoneffects– Neutrinomass
spectrum– flavormixings– progenitortype
P(νeνe)
Survivalofneutroniza-onburstinONeMgSne!
OscillaPons:spectraldistorPons
Harder spectrum! Depends on masses, mixings
p = survival probability
x= µ, τ
NeutrinooscillaPonsStar
vacuum Earth
• MaVereffects:– refracPonfrequency≈vacuumfrequency– Neutrino‐neutrino,neutrino‐electronscaVering
Neu
trino
-neu
trino
“hig
h” M
SW
“low
” (so
lar)
MS
W
“low
” (so
lar)
MS
W 103 g cm-3 10 g cm-3 108 g cm-3
UniqueofsupernovaeUniqueof
supernovae!
HighMSW:θ13resonantdependence
1ν2ν
3ν
13θSin2 2θ13<0.15
CHOOZ, PLB466, 1999 m
νe νµ ντ
• Uniqueresonance:sin2θ13~1inmaMerif:Δm2
31/2E~21/2GFρ/mN
• Realizedforρ~103gcm‐3
Dighe and Smirnov, Phys. Rev. D62, 2000 C.L. & A. Y. Smirnov, JCAP 0306, 2003
• SensiPvitydowntosin2 θ13~ 10-5 ! Survival probabilities,
normal hierarchy
Plot from Nakazato et al., Phys.Rev.D7 , 2008
Neutrino‐neutrino:spectralswaps
• Step‐likeprobabilityasfuncPonofenergy
• Workinprogress
Groups: Munich, San Diego, LANL, North Carolina S., Trieste, Bari, Orsay, Tata Inst., New Mexico U., Minnesota U., … Plot from Dasgupta et al., arXiv:1002.2943
• SPll,agalacPcSNmighttakeawhile…
ClipartfromM.Vagins
Diffuseflux:everythingandnow
• SumoverallSNeintheuniverse
• Now:alterna-vetoagalac-csupernova!– ConPnuousflux,nowai-ng-me
– mightbeeverydayphysicsinfuture!• ~20events/yearatMtwaterCherenkov
Plot from C.L., Phys.Rev.D75:073022,200
• Everything:probesthewholesupernovapopula-onoftheuniverse– What’stypical?– CosmologicalSNe– Diversity:Fe‐core,ONeMgcore,blackholecore,…
• increaseswithz– ~40%offluxfromz>0.5
CosmologicalrateofSNe
Horiuchi, Beacom & Dwek, 2009
Detection energy window total
Ando and Sato, Phys. Lett. B559, 113, 2003 C.Lunardini, arXiv:1007.3252
Example:failedSNe
• M>25‐40Msun,9‐22%ofcollapses– Tooraretoexpecta
galac-cone!
• Collapsedirectlyintoblackhole,noexplosion
• NeutrinoshoMerandmoreluminous• <E>≈20MeVforallflavors
SEOSLSEOS
Liebendörferetal.,ApJS,150,263,K.Sumiyoshietal.,PRL97,091101(2006),T.Fischeretal.,(2008),0809.5129,K.Nakazatoetal.,PRD78,083014(2008)
failedSNemaydominate!• 10‐100%effectondiffuseflux
– SpectraldistorPon
C.L., Phys. Rev. Lett., 2009, J. Keehn & C.L., arXiv:1012.1274
Failed
Total
S EoS, p=0.68, fNS=0.78
Wrapup
Thepost‐solarphase:supernovae,etc..
• ~2020‐….:DiscoverydiffuseSNneutrinoflux
– SNneutrinosbecomeeverydayphysics
– ComplementSN1987A– Cosmological
supernovae– Averagedoverwhole
SNpopulaPon
• Noprecision!
Thepost‐solarphase:supernovae,etc..
• ~…‐2100:PrecisionGalac-csupernova
– Allflavor‐detecPon
– ModeldiscriminaPon– Timing
– OscillaPoneffects– Newphysics
• Precision!
backup
6/1/11 34
Data(sparse)vstheory..
• Garching/ORNL• LawrenceLivermore• Arizona
Kamiokande
E/MeV IMB
Biontaetal.,PRL58,1987,Hirataetal.,PRL58,1987,PRD38,1988
sin2θ13=10-4
IMB
• ~1Ktwaterdetectors
LawrenceLivermore Totanietal.,Astrophys.J.496(1998)
Arizona Thompson,Burrows&Pinto,Astrophys.J.592(2003)
Garching Keil,Raffelt&Janka,Astrophys.J.590(2003)
5parametersfit,withoscillaPons,marginalized(C.L.,Astropart.Phys.,2006.)
68,90,99%CL
H2O
Foglietal.,JCAP0504:002,2005
• testtan2θ13downto10‐5!
HighMSW:θ13resonantdependence
Transition probability PH
C. L. and A. Y. Smirnov, Nucl. Phys. B 616, 307 (2001), JCAP 0306, 009(2003);
anP‐νesurvivalprobability(Pmeaveraged,constantinenergy)
AtwopopulaPonmodel:diffuseflux
C.L.,arXiv:0901.0568,Phys.Rev.LeV.,2009
Upperlimitsandbackgrounds
Energywindow
SuperKamiokande(Maleketal.,PRL,2003):
Reddashed:HomestakeSolid,grey:Kamioka
Time‐integratedfluxes
– Progenitor:M=40Msun,fromWoosley&Weaver,1995
Shenetal.(S)EoS
BH
NS
K.Nakazatoetal.,PRD78,083014(2008)
Laxmer‐Swesty.(LS)EoS
Largerenergywindow
• NSonly:– 12‐29MeV@Kamioka– 10–27MeV@Homestake
• NS+BH:– 12‐36MeV@Kamioka
– 10‐32MeV@Homestake
Reddashed:HomestakeSolid,grey:Kamioka
Strongercosmological(z>1)contribuPon
Blackholeforming:58%(32%)above10MeV(20MeV)
Neutron‐starforming:<30%(<15%)above10MeV(20MeV)
total
total
z=0‐1
failedSNemaydominate!
NS
BH
• Bestcase:“sPff”EoS,22%failedSNe,maximum
ClosetoSKlimit!
C.L.,arXiv:0901.0568,Phys.Rev.LeV.,2009,J.G.KeehnandC.L.,inpreparaPon
AnP‐nueflux
• Best:~100%enhancement
Total
NS
BH
WhataboutnearbyfailedSNe?
Hig
h ba
ckgr
ound
D=1 Mpc, M=1 Mt, S EoS
ExtragalacPcfailedSNeatMtdetectors
• 2‐3eventsfrom~4‐5Mpc– SEoS,20%failedSNe
• upto1perdecadeexpected!– ComparabletonormalSNe
Failed SNe Local rate from S. Ando, J. F. Beacom, and H. Yuksel (2005).
L. Yang & C.L., arXiv:1103.4628
• Upto~0.1yr‐1bursts(N≥2)canbedetected• ComparabletorateofnormalSNe!
normal
failed
Background:N≥2ok
• Invisiblemuons,atmosphericneutrinos– λ=1855yr−1(failed),λ=680yr−1(normal)
• AccidentalcoincidenceinΔt– ω2=λ2Δt,ω3=λ3Δt2(Δt=1s,10sforfailed,normal)