Indirect WIMP detection with neutrinos in Hyper-K Yusuke Koshio - - PowerPoint PPT Presentation
Indirect WIMP detection with neutrinos in Hyper-K Yusuke Koshio for Hyper-K astrophysics working group Kamioka observatory, ICRR, Univ. of Tokyo Cosmic Frontier Workshop SLAC - March 7, 2013 Neutrinos generated by WIMP annihilation Trap
for Hyper-K astrophysics working group Kamioka observatory, ICRR, Univ. of Tokyo Cosmic Frontier Workshop SLAC - March 7, 2013
Sun χ" χ" Earth ν" µ"
A.Gould, ApJ, 388, 338 (1992)
Trap inside the sun
χ χ W, b,τ...→ν W, b,τ...→ν
Preliminary IceCube/DeepCore Limit IDM 2012 / arXiv:1212.4097 Preliminary Super-K Limit Neutrino 2012 / arXiv:1210.4161
Prelim Super-K 2012 (bb) Prelim Super-K 2012 (ττ)
K i m s 2 1 2
Preliminary
39.3m 41.4m
Cherenkov light charged particle neutrino Outer
Fiduial vol. : 0.0225 Mton
2km 3km 1km
(2700mwe)
Atotsu Mozumi
Ikeno-yama
Kamioka-cho, Gifu Japan
~11000 Inner PMTs
Super-Kamiokande IV Run 999999 Sub 0 Event 209 10-02-17:16:23:39 Inner: 3136 hits, 6453 pe Outer: 3 hits, 2 pe Trigger: 0x03 D_wall: 1218.7 cm e-like, p = 701.5 MeV/c Charge(pe) >26.7 23.3-26.7 20.2-23.3 17.3-20.2 14.7-17.3 12.2-14.7 10.0-12.2 8.0-10.0 6.2- 8.0 4.7- 6.2 3.3- 4.7 2.2- 3.3 1.3- 2.2 0.7- 1.3 0.2- 0.7 < 0.2 260 520 780 1040 1300 0 mu-e decays 500 1000 1500 2000 260 520 780 1040 1300 Times (ns)e"like
Super-Kamiokande IV Run 999999 Sub 0 Event 454 10-02-15:01:25:39 Inner: 2208 hits, 9333 pe Outer: 10 hits, 9 pe Trigger: 0x03 D_wall: 1479.4 cm mu-like, p = 1154.7 MeV/c Charge(pe) >26.7 23.3-26.7 20.2-23.3 17.3-20.2 14.7-17.3 12.2-14.7 10.0-12.2 8.0-10.0 6.2- 8.0 4.7- 6.2 3.3- 4.7 2.2- 3.3 1.3- 2.2 0.7- 1.3 0.2- 0.7 < 0.2 172 344 516 688 860 0 mu-e decays 500 1000 1500 2000 172 344 516 688 860 Times (ns)µ!like
νe""+"n"!""e%""+"p" νµ""+"n"!""µ%""+"p"
QECC interaction
✓Good Particle ID ✓Conserve the neutrino direction
from the Sun
✓Good energy reconstruction
Preliminary IceCube/DeepCore Limit IDM 2012 / arXiv:1212.4097 Preliminary Super-K Limit Neutrino 2012 / arXiv:1210.4161
Prelim Super-K 2012 (bb) Prelim Super-K 2012 (ττ)
K i m s 2 1 2
Preliminary
Event category
✓Upward going muons (Upmu)
νμ μ
through
μ
stopping
✓Contained events
νμ ν ν
Fully (FC) Partially (PC)
sensitive to low-mass
K.Choi, Neutrino 2012 Preliminary
No significant excess from the Sun
☜ fro Reconstructed angular spectrum of
Total vol. : 0.99 Mton Fiducial vol. : 0.56 Mton Photo-sensors : 99,000 PMTs
LoI : arXiv 1109.3262
10
10
10
10
10
10
10
10
10
10
2
10
3
10
4
Gaitskell,Mandic,Filippini
arXiv 1109.3262
KIMS PICASSO AMANDA(bb) AMANDA(WW) IceCube(bb) IceCube(WW) SK(bb) SK(WW) HK 5years (bb) HK 5years (WW) IceCube+DeepCore Scale from the SK upmu results
(LoI)
10
10
10
10
10
10
10
10
10
10
2
10
3
10
4
Gaitskell,Mandic,Filippini
KIMS PICASSO AMANDA(bb) AMANDA(WW) IceCube(bb) IceCube(WW) SK(bb) SK(WW) HK 5years (bb) HK 5years (WW, ττ) IceCube+DeepCore Adding the FC+PC sample can extend the sensitivity direct to lower mass region.
Preliminary
5yrs Hyper to
!"
#$%#&'
($%)*+' ",-, ./0,!!1$%2342' 1 5 . . $ % 2 3 4 3 ' /6*07&*$%2342' !7#*89$%2344' !7#*89$2342 :;#*89$<;8= 43> 432 433 434 432 43?
PINGU 5yrs
HK HK PINGU PINGU
Preliminary
results (FC+PC+upmu) to Hyper-K.
interesting WIMP mass region suggested by the direct search experiments.
favorable to other indirect searches for WIMP masses below ~20-50 GeV.
π0 γ γ π+ π-
π- π-
π+ π+ π+ π+ π+ π+
π- π-
π+ π+ π+
Possible annihilation channels:
qq,gg,cc,ss,bb,tt,W+W-, ZZ, τ+τ-,μ+μ-, νν, e+e-,γγ
few neutrinos some “high energy” neutrinos in decays ⇒ basis of present day searches
dominant decay into hadrons Charged pions at rest producing neutrinos up to E=52.8MeV
π+ → µ+νµ µ+ → e+νe¯ νµ
log[dN/dE] neutrino energy (MeV)
29.8MeV 52.8MeV
arXiv 1210.4161 by C.Rott Decay At Rest
μ e e e
T < 50 MeV
“reactor + solar” “atm. muon neutrinos” “atm. electron neutrinos” “μ/π production from
“invisible muon”
μ e
T > 200 MeV
“visible short muon track”
NC
Phys.Rev. D85 (2012) 052007
can provide a way to discriminate against this background
p n e +
νe!
γ
Gd
(8MeV)
~20μsec Use a delayed coincidence signal
Kamioka underground observatory
Super-Kamiokande
50m
control room experimental hole
P M T c a b l e
コントロール室 実験室 ガドリニウム実験室全体図
セットアップ トンタンク 信号ケーブル、 ケーブル （ノイズが乗らないことは を用い て確認済み） コントロール室
Electronics and computer
Evaluating Gadolinium’s Action on Detector Systems
200#ton#water#tank# Main#water# circula1on#system 15m3#tank
With PMTs, cables, black sheet and etc.
R&D for Gd in SuperK (GADZOOKS!)
Kamioka underground observatory
Super-Kamiokande
50m
control room experimental hole
P M T c a b l e
コントロール室 実験室 ガドリニウム実験室全体図
セットアップ トンタンク 信号ケーブル、 ケーブル （ノイズが乗らないことは を用い て確認済み） コントロール室
Electronics and computer
Evaluating Gadolinium’s Action on Detector Systems
200#ton#water#tank# Main#water# circula1on#system 15m3#tank
With PMTs, cables, black sheet and etc.
R&D for Hyper-K (Gd option)
APD Photo tube (cathode)
M.Yokoyama, this afternoon session
1 10 100 mχ [GeV] 10−4 10−3 10−2 10−1 1 101 102 103 σSD
χP [pb = 10−36 cm2]
DAMA EVAPORATION
SUPER−K (2012) ICECUBE (2012) bb − W+W−, τ+τ− THIS WORK PICASSO (2012) KIMS (2012) SIMPLE (2012)
Super-K 4yrs Hyper-K 4yrs + Gadolinium best case
above lines is excluded
Preliminary ky , C + HK 5years
higher intensity ν by upgraded J-PARC
Hyper-K Sun Supernova
x25 Larger ν Target & Proton Decay Source
Proton Decays
ν ν ν ν x2 (year
x50 of T2K for !CP
18
第1回: 2012年8月23,24 第 回 年 月
36
http://indico.ipmu.jp/indico/conferenceTimeTable.py?confId=7
第 回 年 月 第2回: 2013年1月14,15
36
http://indico.ipmu.jp/indico/conferenceTimeTable.py?confId=10 1st : 2012 Aug. 2nd : 2013 Jan. Start up an international working group (~100 researchers) < List of R&D >
etc.
for indirect WIMP search.
reconstruction.
mass region less than 50GeV.
unique prospects for Hyper-K.