cygnus 2013@toyama 2013/06/05 nagoya univ. h.uchida for xmass collaboration 1
TRANSCRIPT
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Status of XMASS experiment
Cygnus 2013@Toyama2013/06/05
Nagoya univ. H.Uchidafor XMASS collaboration
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Overview
2
835 kg, 100 kg Fiducial volume (FV)
80 cm, 642 PMTsφ
XMASS-II
25 ton, 10 ton FVφ2.5 m ・ Dark matter ・ pp solar neutrino ・ 0 2 n b decay
XMASS-1.5
5 ton,1 ton FV1.5 m, ~1000 PMTsφ
XMASS-I
・ Dark matter search
•A purpose of XMASS-I and 1.5 experiment is dark matter search.•Commissioning data was taken with XMASS-I at the Kamioka Observatory in Japan between Nov. 2010 and May. 2012. And now refurbishment work is on going.•XMASS-II has multi purpose of dark matter, pp solar neutrino and 0 2 decay.ν β
Y. Suzuki, hep-ph/0008296
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800kg detector
• XMASS is a single phase detector with ultra pure liquid xenon.
• Background is reduced by a self-shielding of liquid xenon.
• This detector has high light yield (~14p.e./keV) & low energy threshold (~0.3keVee).
• This detector is sensitive for electromagnetic signals.
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Detector configuration
10m
11m
~ 1.2m642PMTs
OFHC coppervessel
835kgliq. xenon
Water tank
Refrigerator
72 20inch PMTs (veto)
Elec. hut
4
700L reservoir
There is a this detector at Kamioka observatory.
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Source calibration
5
Steppingmotor
Linear and rotary motionfeed-through
Topphototube
~5m
Gatevalve
5
4mmf0.21mm f for 57Co source
Source rod with a dummy source
RI Energy [keV] [Hz] dia.[mm]
(1) Fe-55 5.9 350 5
(2) Cd-109 8(*1), 22, 25, 88 800 5
(3) Am-241 17.8, 59.5 485 0.21
(4) Co-57 59.3(*2), 122 40 0.21
(5) Cs-137 662 200 5(*1) Ka X-rays from the copper used for housing.(*2) Ka X-rays from the tungsten used for housing.
•Calibration sources are used for checking detector response.• The sources can be moved along the vertical axis in the detector.
•We can use one of five sources.•Right hand animation shows a procedure of calibration data taking. First, installation of a source to a calibration rod, opening the top PMT, and insertion of the rod.
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Calibration data
• Calibration data で real data を
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Real data MC
57Co calibration data (122keV)
4030
40
30
20
10
0-10
-20
-30
-40
4030
20
10
0-10
-20
-30
-400 10 20-10-20 0 10 20-10-20
y [cm]y [cm]z
[cm
]
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Background• Background level of XMASS-I is a few event/day/keV/kg [dru]
without fiducualization.• It is similar level with DAMA and CoGeNT.• The origin of BG for more than 5 keV were almost identified
(lower figure). Also for less than 5 keV, Gore-Tex may explain the events.
• Events originate at the inner surface must explain major part of the observed events..
77
Full volume
5 2010 15dru
[/da
y/ke
Vee/
kg]
● Black line: Real data ● Colored histogram: BG (MC)
Surface Cu 210Pb PMT Al 235U-231Pa 210Pb 232Th 238U-230Th PMT gamma Gore-Tex 210Pb Gore-Tex 14C
PMT 写真とアルミの位置の説明
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Light mass WIMP search
8
Full volume (835 kg) analysis6.70 days×835kg in 2012 Feb. 0.3 keVee threshold
Energy [keVee]
Coun
ts/d
ay/k
g/ke
Vee
0 0.5 1 1.5 20
1
2
3
4
5
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solar axion search
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Our data
ma=
50 keV
Max allowed
Axion is a hypothetical particle to solve the strong CP problemProduced in the Sun and detected in the detectorXMASS is suitable to search because of a large mass and low BG
Bremsstrahlung and Compton effect
gaee
gaee
Axio-electric effect
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WIMP-Xe129 inelastic scattering
他の非弾性散乱実験についての言及。
I127 を使った( DAMA 、 PICORON )?論文があるか見ておくこと。
Inelastic の図
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Reduction of surface background
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Optimization of the cut parameters
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Systematic error
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Upper limit for the inelastic cross section
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1.5
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Refurbishment
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Summary
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Back up
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Cross section of DM100GeV
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f
MR
fNv
MR
WI
TW
WIasI
3710758.3
= 3.758×10-37 ×6.74×100/0.3 = 8.4×10 34 ‐ cm2 (8.4×102pb)
(explanation of this function in backup slide)
NA of Xe129
# of events of no cut in DM100GeV MC are 82625.If these events occur in 55.6days,
Calculation of cross sectionDM100GeV:82625/835/0.264/55.6 = 6.74 event/kg(Xe129)/day
Scaled energy(13.9PE/keV)
Even
t/ke
V
When cross section is 8.4×102pb, inelastic events by DM100GeV occur 82625 events in 55.6days.
Even
t
Reconstructed R (cm)
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Cross section of DM200GeV
20
f
MR
fNv
MR
WI
TW
WIasI
3710758.3
= 3.758×10-37 ×6.74×200/0.5 = 1.0×10 33 ‐ cm2 (1.0×103pb)
(explanation of this function in backup slide)
NA of Xe129
# of events of no cut in DM200GeV MC are 82640.If these events occur in 55.6days,
Calculation of cross sectionDM200GeV:82640/835/0.264/55.6 = 6.74 event/kg(Xe129)/day
When cross section is 1.0×103pb, inelastic events by DM200GeV occur 82640 events in 55.6days.
Scaled energy(13.9PE/keV)
Even
t/ke
V
Even
t
Reconstructed R (cm)
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Cross section of DM400GeV
21
f
MR
fNv
MR
WI
TW
WIasI
3710758.3
= 3.758×10-37 ×6.70×400/0.53 = 1.9×10 33 ‐ cm2 (1.9×103pb)
(explanation of this function in backup slide)
NA of Xe129
# of events of no cut in DM400GeV MC are 82175.If these events occur in 55.6days,
Calculation of cross sectionDM200GeV:82175/835/0.264/55.6 = 6.70 event/kg(Xe129)/day
When cross section is 1.9×103pb, inelastic events by DM400GeV occur 82175 events in 55.6days.
Scaled energy(13.9PE/keV)
Even
t/ke
V
Even
t
Reconstructed R (cm)
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Reduction of best parameter set
22
Energy(keV)
# o
f eve
nts
Live time: 55 days
cut # of events(20-
100keV)
reduction
No cut 2094840 1
(1):pre-selection 1651610 0.79
(2) : (1) + volume cut
2877 1.4e-3
(3) : (2) + timing cut
417 2.0e-4
(4) : (3)+ band cut 7 3.3e-6cut # of events
(30-65keV)
reduction
No cut 990692 1
(1):pre-selection 779820 0.79
(2) : (1) + volume cut
1224 1.2e-3
(3) : (2) + timing cut
180 1.8e-4
(4) : (3)+ band cut 1 1.0e-6
Reconstructed R
# o
f eve
nts
Signal region
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Origin of BG in XMASS-I
2424
Al seal
Main BG source ( 5keV)≧
BG candidate (< 5keV) In refurbishment, Al seal will be covered by copper rings and GORE-TEX will be removed In XMASS-1.5, Al seal will be replaced with ultra pure one