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)