The XMASS Experiment searching for Dark Matter at …...The XMASS Experiment searching for Dark...
Transcript of The XMASS Experiment searching for Dark Matter at …...The XMASS Experiment searching for Dark...
The XMASS Experimentsearching for Dark Matter
at the Kamioka Observatory
Status and Previous Results
Kai Martens
Kavli IPMUThe University of Tokyo
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 2
Outline
- Kavli IPMU: a word about my institute
- Dark Matter: setting the stage
- Kamioka Observatory: the preeminent underground sciencelaboratory in Japan
- XMASS Experiment: - design
- results from first commissioning phase
- refurbishing
- the next step in the program
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 3
Kavli IPMU
one of the 5 original WPI centers:- founded Oct. 1, 2007- first institute in Todias Jan. 11, 2011- first Kavli institute in Japan May 10, 2012
best evaluations among WPI centers5 year “extension” to be decided soon...
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 4
The Kamioka Observatory:
KamLAND (Xe)
CANDLES
NEWAGEEGADS
Super-Kamiokande,(T2K)
XMASS
IPMULab
CLIO Legend:DM, , , GW
3km
to M
ozum
i
new: KAGRA
Tokyo
Nagoya
IPMU Lab:U, Th → HP-Ge ← few 100ppt
→ ICP-MS ← 1ppq*Kr → API-MS ← 1ppt*
* after concentration
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 5
The XMASS CollaborationKamioka Observatory, ICRR, University of Tokyo:
Y. Suzuki, M. Nakahata, S. Moriyama, M. Yamashita, Y. Kishimoto,
A. Takeda, K. Abe, H. Sekiya, H. Ogawa, K. Kobayashi, K. Hiraide, B. Yang,
K. Ichimura, O. Takachio, N. Oka, K. Nakagawa, M.Kobayashi
IPMU, University of Tokyo: K. Martens, J.Liu
Kobe University: Y. Takeuchi, K. Miuchi, K. Hosokawa, Y.Ohnishi
Tokai University: K. Nishijima
Gifu University: S. Tasaka
Yokohama National University: S. Nakamura, I. Murayama, K. Fujii
Miyagi University of Education: Y. Fukuda
STEL, Nagoya University: Y. Itow, K. Kobayashi, K. Masuda, H. Uchida, H. Takiya
Sejong University: Y.D. Kim, N.Y. Kim
KRISS: Y.H. Kim, M.K. Lee, K.B. Lee, J.S. Lee
40 collaborators, 10 institutions, 2 countries
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 6
Early Observations: Oort & Zwicky 1932: Jan Oort (Leiden, Netherlands):
“measures” matter in galactic disk near sun from motion of nearby stars: 1M
⊙/375ly3 > 2m
stars
→ dark matter
1933: Fritz Zwicky (Caltech, USA):
virial theorem: ΣT = ½ ΣU→ galaxies in Coma cluster too fast for cluster's gravitational potential
→ dark matter
Vera Rubin @ Carnegie Institutionof Washington:
rotation curves of galaxies1975 AAS meeting
1980 paper
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 7
New Scientist (2005/03/19): Michael Brooks: 13 things that do not make sense: Maybe we can't work out what dark matter is because it doesn't actually exist. That's certainly the way Rubin would like it to turn out. "If I could have my pick, I would like to learn that Newton's laws must be modified in order to correctly describe gravitational interactions at large distances," she says. "That's more appealing than a universe filled with a new kind of sub-nuclear particle."
@ Carnegie Institutionof Washington:
1975 AAS meeting 1980 paperA: expected curve
given luminous matterB: observed curve...
http://apod.nasa.gov/ apod/ap110219.html:inner part of NGC 2841 by HST
measured60 galaxies
viagas clouds
(H, He)[not stars!]
vf
Galactic Rotation Curves: Vera Rubin
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 8
Dark Matter: It's out there …
http://apod.nasa.gov/apod/ap060824.html
http://cosmicweb.uchicago.edu/filaments.html
blue: DM, red: hot gas
≈
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 9
So What Are We Looking For?
- gravitating: the only thing we know for sure...
- cold: → massive ← if particle (cold DM...)
- collisionless: → no E/M interaction→ no strong interactionat most: weakly interacting ???
(Rubin as in: Vera Rubin)
New Scientist (2005/03/19): Michael Brooks: 13 things that do not make sense: Maybe we can't work out what dark matter is because it doesn't actually exist. That's certainly the way Rubin would like it to turn out. "If I could have my pick, I would like to learn that Newton's laws must be modified in order to correctly describe gravitational interactions at large distances," she says. "That's more appealing than a universe filled with a new kind of sub-nuclear particle."
favorites are: neutralino, axion, Kaluza-Klein, gravitino
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 10
Dark Matter and the WIMP Miracle
WIMP denomination → weak interaction ...
WIMP decoupling after BB:
velocity averaged annihilation cross-section for GeV-TeV mass WIMPs:
<σv> = 3×10-26cm3/s → correct DM density
TeV ~ SUSY partners ???
but: LHC... ☹
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 11
WIMP Dark Matter Searches:Direct Detection
from proceedings Tev06:Search for WIMPs with CDMS and XENON
two types of interaction:- spin dependent (odd isotopes), smaller cross section- spin independent; σ ~ A2 (coherent: whole nucleus)
important for verification:different target materials
→ consistency!
CDM → massive → nuclear recoil (NR) 50keV
NR → ~10keV
ee
calibration sources are γ-sources...(ee)
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 12
The Current Situation: (WIMP hypothesis:)
compatible:- spectra:
CoGeNT/CRESST-II- modulations:
DAMA/CoGeNT
tension:- Xe vs. all of the above- modulation amplitude(halo assumptions...)
two regions of experimental focus:- low threshold...- low background...
Fig. 5 of 1310.8214:LUX 1st results (90% CL)
Xenon100 225d, 100dCDMS II, ZEPLIN-III, Edelweiss II
allowed regions:CDMS II Si (95%)
DAMA/LIBRACRESST !!
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 13
The XMASS ExperimentXe detector for weakly
interacting MASSive particlesXe -MASS detector Xe MASSive -detector
Exploiting Xenon:- high mass number → SI cross section- no long-lived radioactive isotope- good scintillation yield: ~ 46ph/keV- high density (liquid): 3g/cm3
- 48% odd isotopes (natural) → SD cross section- ββ candidate: 136Xe → 136Ba+2e–+2.48MeV
Ultimately: 10t fiducial volume multi-purpose detector:- neutrino mass: ββ- Dark Matter: WIMP limited by:- solar neutrinos: pp, 7Be
(the water tank in Hall C is designed to hold this...)
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 14
XMASS Progression:
100kg reference:arXiv:0912.2405
the PAST:100kg prototype,
(3kg fiducial), 30cmproof of principle
the current incarnation:Phase I
835kg WIMP detector(100kg fiducial), 80cm Ø
detector technologyadvantages:
- simple- scalable- self-shielding
ultimately: 24t (10t fid.) 2.5m Ø
24t, + ⊙
(10t fiducial)2.5m
the (far) future:
the next step:5 ton total, > 1.5ton fiducial
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 15
XMASS Physics:
Phase I:100/835 kg
main purpose:DM direct detectionχ + Xe → χ + Xe
Phase II:10/25 t
multi purpose:DM direct detection:χ + Xe → χ + Xe
pp and 7Be solar neutrinos:ν + e– → ν + e–
neutrinoless double-β decay:136Xe → 136Ba + 2e–
intermediate proposal:XMASS 1.5
to compete in the next roundof DM direct detection: ~1t hep/ph 0008296
Y. Suzuki
expected“singal”
rates [dru]:
low background speak:
dru(differential rate unit):
events / day / kg / keV
2ν2e– (2.38x1021y)
pp7Be10–6
10–4
χ m=50GeV
χ m=100GeV
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 16
Background Requirements:
WIMPs:
10-4 dru → cross sections down to a few times 10-45 cm2
solar neutrinos:
better than 10-5 druexpected rate in 10t: 14/d for pp + 6/d for 7Be
→ important considerations:- go underground (shielding against cosmogenic activation)- carefully select and monitor your materials for radio isotopes- shield your detector (against ambient radiation: 222Rn, n, γ)
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 17
Shielding Against Ambient Radiation
fast Neutron MC:
Xe
Watertank
fast neutrons:water tank
11m high (10m water)10m Ø
active: -veto
also
:h
all l
inin
g R
n r
etar
din
gR
n-”
po
or”
ou
tsid
e ai
r su
pp
ly
gamma radiation:xenon →
self-shielding:
inner pink circle: fiducial volume
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 18
Hall C in Kamioka: XMASS
Hall C: 15m,21m,15m (h,d,w)
water in tank:10m high
10m Ø
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 19
XMASS from the Outside In:
Outer Detector (OD):72 x 20inch PMTs (=SK)
calibrationport
Inner Detector(ID):642 PMTs
1100 kg LXe(total)
835 kg(inside PMTs)
100 kg(fiducial)
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 20
Inner Detector Structure:2nd
LAYER
FILLER
LXe in detector:1100kg
in sensitive volume:835kg
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 21
Building the Inner Detector 1:
photocathodecoverage:
62.4%
xenon insidethe photocathodes:
835 kg
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 22
Building the Inner Detector 2:
Feb
2010
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 23
Low BG PMT Development:
630 hexagonal + 12 round) PMTs:
Hamamatsu R10789: QE 28-39%+
XMASS photocathode coverage: 62.4%
BG: biggest worry → PMT
great development:
U < 1.0Th< 0.94K < 9.68Co = 4.47±0.34
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 24
Electronics:
new: FADCs
CAEN V17518 ch/board
bandwidth 500MHz,sampling rate 1GS/s
resolution 10bit1.2 μs window
Super-Kamiokande ATM:
12 bit ADC/TDCintegration: -100ns – +300ns
1.2 μs window
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 25
Xe Distillation: (85)Kr Removal
K.Abe et al, Astroparticle Physics
31(2009), p290
capacity of XMASS Xe distillation system:6kg/h; did 1 ton in ~ 1 week → (3.3±1.1)ppt
otherwise:extensive materials validationbefore construction:
IPMU Lab:U, Th → HP-Ge ← few 100ppt
→ ICP-MS ← 1ppq*Kr → API-MS ← 1ppt** after concentration
hall C distillation system:(used before filling detector)
experience:detector stable w/o:- routine getter operation- active Rn removal
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 26
XMASS Calibration System:
sourceexchange
“internal” γ calibration for XMASS:- 57Co (122keV) ← main anchor of energy scale
- 241Am (59.5keV), 109Cd (88keV), 55Fe (5.9keV)
“external” (hose)- 60Co, 137Cs- 252Cf neutron calibration (needs FADC)
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 27
57Co Calibration:reconstruction:
data MC
@ center:data vs. MC
W (59.3 keV)
57C
o (1
22 k
eV)
57C
o (1
36 k
eV)
center position setsenergy scale:
→ 13.8 p.e./keVee
energy resolution: 4% rms
position resolution (rms):center: 1.4 cm±20cm: 1.0 cm
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 28
Energy Scale Evolution
photoelectron yield is continually improvingeven after we stopped forcing circulation through hot getters!
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 29
Detector Stability
det
ect
or
stu
dy
det
ecto
rst
ud
y
tracking intrinsic background signals with our 57Co energy scale:
ratio
w/a
vera
ge →
46 keV 0.47%variablity: 1.1MeV 0.60%
1.3 MeV 0.36%
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 30
Extrapolating the Energy Scale
XMASSanalysisthreshold
nuclear recoil scintillation efficiency Leff
follows Xenon100 (arXiv 1104.2549):
57Co
55Fe
109Cd
241Am
above linear fit is used to interpolatekeV
ee energies between calibration
points (from internal gamma sources)and extrapolate to lower energies
dominantsystematic..
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 31
XMASS Unexpected BG: The Culprit:
the culprit:Al seal for PMT window:
238U and 210Pb found in raw material(not in secular equilibrium)
unexpected BG traced tosurface between PMTs:
β may deposit most energyinside the material
→ low energy signal...
early suspect:Gore-Tex (light barrier) under PMT rim:
may contain up to 6% modern carbonbut: no signal when measured in XMASS
(no longer needed after refurbishment)
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 32
Main BG Source: PMT Al Seal...shape assumed inoriginal MC production:
(full volume)
shape derived fromPMT inspection:
(full volume)
Surface 210PbPMT Al 235U-231PaPMT Al 210PbPMT Al 232ThPMT Al 238U-230ThPMT gammaDots: XMASS data
E > 5 keVee
:
BG understood!
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 33
The Good News: BG (Low), LY high(still optimizing: reduce leakage of surface events into FV)
but:
graph (- XMASS...)taken from:
E. Aprile(Princton 2010)
high light yield (LY) → low threshold → go for light WIMPs
(heavy WIMPs → large A → large cross section → to come)
XMASS full volume !!!
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 34
Light WIMPs:Full Volume, Low Threshold
playing to our strength:
full volume = 835kg4 hit threshold = 6.75 days(now standard after refurbishment)
backgrounds to be considered: cuts applied:
- no OD activity → ID trigger only- no afterpulse activity → timing RMS < 100ns- Cherenkov (40K in photocathode) → q(20ns)/q(total) < 0.6- ringing, radioactivity → ± Δt > 10ms
systematics to account for:L
eff, energy resolution & scale, trigger efficiency, cuts
our limit:maximally allowed
cross section:MC prediction < data
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 35
Cherenkov CutCherenkov light emission in PMT glass (40K, …)
Cherenkov photons emitted “immediately”:→ PMT timing resolution (~3.5ns)
scintillation events:→ time constant τ ~ 25ns (low energy γ and nucl. recoil)
cut parameter:
charge(first 20ns) charge(total)
keep < 0.6
efficiency varies with p.e. range: 40% – 70%
data MC
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 36
Trigger Threshold & Data Reduction
70%
30%
signal efficiency(MC)
w/fit
(for low threshold data used inlow-mass WIMP and axion searches)
LED data
6.7d low thresholddata
signal efficiency after all cuts →
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 37
XMASS Low Mass WIMP Result:
systematic contributions:(in order of declining importance)
- Leff
uncertainty *(solely responsible for red shaded)
- energy resolution
- trigger efficiency
- energy scale
- Cherenkov cut(all fit into thick red line...)
* following arXiv 1203.1589 (Xe100)
Phys. Lett. B719 (2013) 78; arXiv 1211.5404
limit by:SG ≤ BG
data
σS
I,χ-n
cm
2
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 38
Solar Axions through Axio-Electric:production in the sun:- g
aN: nuclear de-exitation (57Fe, line @ 14.4keV)
- gaee
: Bremsstrahlung, Compton
- gaγγ
: Primakoff effect
XMASSsolar axion limit:g
aee< 4.5x10-11in
dire
ct b
ound
fro
m s
olar
ν fl
ux detectionin XMASS: axio-electric
samestraightforward
limitevaluation
Phys. Lett. B724 (2013) 46arXiv: 1212.6153
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 39
Annual Modulation Analysis
136.1 days (2010/12-2012/5)835kg → 0.31 tythreshold (analysis): 1 keV
ee
fit functiont0, ω fixed!
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 40
Annual Modulation ResultStandard HaloModel
(from: 1209.3339)
difference:summer-winter
solid: summerdashed: winter
JPS fall 2013:XMASS 90% CL
CDMS II 2009Xenon100 2012
DAMA/LIBRA 2008
Energy [keVee
] →
rate
dif
fere
nce
[co
un
ts/k
g/k
eV/d
] →
fits on data→
solid line:best fit
dashed:90% UL
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 41
XMASS Pre-Refurbishment Highlightsvery successful technology:
→ highest photoelectron yield in the community: 13.8 PE/keVee
→ very low analysis threshold (without fiducialization)
→ very stable long-term operation without active circulation, i.e. without recirculating through hot getters !!
→ eminently scalable: no drift length limitations
→ first results despite unexpected background
but: surface/materials backgrounds need to be better controlled...
→ detector refurbishment: results to come...
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 42
XMASS Detector Refurbishment:
done: we are taking new data
what was done:
- Cu surface cleanup → electropolish to “rm -rf U* Th*”
- Cu ring to cover PMT Al seal
- cover Cu rings with electropolished Cu plate for a flat inner Cu surface (no crevasses...)
duller (lighting aside) brighter
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 43
Chemically ElectropolishedEtched
duller (lighting aside) brighter
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 44
XMASS 1.5background target: ~10-2 /ton/day/keV
(we have a lot of experience now...)
again: two analyses: - low threshold, full volume:
→ cover all “allowed regions” - 5keV threshold, fiducial volume:
→ reach SI cross section of< 10-46 cm2
start construction in 2014 !tank for active water shield is ready...
improved photocathode geometry:to intercept light from surrounding surface...
January 17, 2014 Kai Martens, Kavli IPMU, @ University of Utah 45
ConclusionsXMASS 800kg completed first commissioning phase:
- exceptional light yield: 13.8 PE/keVee
- backgrounds largely understood - detector refurbishment completed:
- serious reduction in Rn exposure during work- inner surface cleaned- inter-PMT spaces covered
→ data taking was resumed with:– refurbished detector– full FADC system
Results (from “old” detector): - light WIMP limit- axio-electric cross section limit- annual modulation analysis
Next: XMASS 1.5 (1 ton fiducial, 5 ton total)