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XMASS, Status of 800 kg detector design. Ko Abe for the XMASS collaboration Kamioka Observatory, ICRR, University of Tokyo. 1. Introduction. Solar neutrino. What’s XMASS. Multi purpose low-background experiment with liq. Xe. X enon MASS ive detector for solar neutrino ( pp/ 7 Be )
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XMASS, Status of 800 kg detector design Ko Abe for the XMASS collaboration Kamioka Observatory, ICRR, University of Tokyo
1. Introduction Solar neutrino • What’s XMASS Multi purpose low-background experiment with liq. Xe • Xenon MASSive detector for solar neutrino (pp/7Be) • Xenon neutrino MASS detector (bb decay) • Xenon detector for Weakly Interacting MASSive Particles (DM search) Dark matter Double beta
Why liquid xenon • Large Z (=54) Self-shielding effect • Large photon yield (~42 photons/keV ~ NaI(Tl)) Low threshold • High density (~3 g/cm3) Compact detector (10 ton: sphere with diameter of ~2m) • Purification (distillation) • No long life radioactive isotope • Scintillation wavelength (175 nm, detected directly by PMT)
pp & 7Be solar n Target for 800kg : Dark Matter search g tracking MC from external to Xenon External g ray BG: 20cm fiducial volume, 100kg U-chain gamma rays Blue : g tracking Pink : whole liquid xenon Deep pink : fiducial volume Expected dark matter signal (assuming 10-42 cm2, Q.F.=0.2 50GeV / 100GeV,) • Dark matter search • With liquid xenon ~1ton, reduce BG below 100 keV to 10-4/day/keV/kg by self shielding. • Search the signal from dark matter in low energy region.
Expected sensitivities XMASS FV 0.5 ton year Eth = 5 keVee~25 p.e., 3s discovery w/o any pulse shape info. 10-4 • Large improvements will be expected Two order higher than experimental results so far. DAMA CRESTT Edelweiss ZEPLIN1 10-6 CRESTTII CDMSII Cross section to nucleon [pb] ZEPLIN2 Edelweiss2 XENON100 10-8 XMASS 800kg SuperCDMS phase A 10-10 Plots except for XMASS: http://dmtools.berkeley.edu Gaitskell & Mandic ~10-45 cm2
Status of 800 kg detector • Basic performances have been already confirmed using prototype detector • Method to reconstruct the vertex and energy • Self shielding power • BG level • Detector design is going using MC • Structure and PMT arrangement (812 PMTs) • Event reconstruction • BG estimation • New excavation will be done soon
Design of 800kg 1 detector • 60 triangles • 10 PMT/triangle x 60 = 600 PMTs • + 212 PMTs in triangle boundary region • Total 812 PMTs • Photo coverage 67.0% • Center to photocathode ~45cm • Fiducial vloume is 25cm from center. • PMTs are inside liquid xenon.
Resolution of event reconstruction and BG estimation from MC • In current design, performance of detector was estimated using Geant4 MC. • Resolution of position. • BG from PMTs • Resolution • Using signals from the PMTs, vertex position is calculated so as to maximize likelyhood. • At boundary of fiducial volume 10keV ~3cm 5keV ~5cm Fiducial volume 12 10 8 DR_reconstructed(cm) 5keV 6 4 10keV 50keV 2 100keV 500keV 1MeV 0 5 10 15 20 25 30 35 40 R(cm)
Background from PMT 238U dru(day-1kg-1keV-1) All volume 5cm self shield 40cm from center 10cm shield 35cm • 1.8 x 10-3 Bq/PMT • <100keV • 5cm shield ~10-3 dru • 10cm shield ~10-4dru • 20cm shield ~10-5 dru 20cm shield 25cm 10-5 10-4 10-3 10-2 10-1 1 Reconstructed Energy(keV)
Background from PMT 60Co All volume 5cm self shield 39.5cm from center dru(day-1kg-1keV-1) 10cm shield 34.5cm 20cm shield 24.5cm • 5.5 x 10-3 Bq/PMT • <100keV same level as 238U • We can achieve 10-5 dru level 10-5 10-4 10-3 10-2 10-1 1 Reconstructed Energy(keV)
Design of 800 kg Detector 2 Water shield for ambient g and fast neutron • Ambient background g and neutron is another large background source. • To reduce these background, use thick water shield. • Estimated how thick shield is needed with simple simulation. Generation point of g or neutron wa Configuration of the estimation Liq. Xe • Put 80cm diameter liquid Xe ball • Assume copper vessel (2cm thickness) • Assume several size of water shield 50, 100, 150, and 200cm thickness for liquid Xe water MC geometry
g attenuation g attenuation by water shield 104 103 102 More than 200cm water is needed to reduce the BG to the PMT BG level Detected/generated*surface [cm2] 10 1 PMT BG level 10-1 10-2 0 100 200 300 Thickness of shield [cm]
Reach points of fast neutron Reach points before thermalized Generation:107 water: 200cm, energy: 10MeV • Fast n flux @Kamioka mine: • (1.15+0.12) x10-5 /cm2/sec - • Assuming all neutron’s energies are 10 MeV very conservatively water Z [cm] Liq. Xe < 2 x 10-4 counts/day/kg 200cm of water is enough to reduce the fast neutron X [cm]
Summary • XMASS 800kg detector • 1 ton liquid xenon, 90cm diameter, 60 triangles, 812 PMTs • BG level 10-4 dru(day-1kg-1kev-1) • Dark matter search 10-45 cm2 • Detector design by simulation • Resolution of event reconstruction • 10keV ~3cm 5keV ~5cm at boundary of fiducial volume • Background from PMT • 238U, 60Co ~10-5 dru insidefiducial volume • Water shield for ambient g and fast neutron • 200cm shield is enough
All volume 5cm shield 10cm shield 20cm shield • In the event which interacted close to the wall, photons emitted toward wall are difficult to detect. Current reconstruction algorithm tend to reconstruct such events more inner region. Energy (keV) • Use 20cm outer region as shield fiducial, the effect from these events are not large, we can keep BG as ~10-5dru. • BG level target of 800kg detector ~10-4dru photon PMT PMT
New excavation @Kamioka mine New excavation for XMASS and other underground experiment will be made soon ~5 m ~20 m ~15 m
Initial energy spectrum from the rock • g attenuation 104 g attenuation by water shield 103 Deposit energy spectrum (200cm) 102 Detected/generated*surface [cm2] 10 1 PMT BG level 10-1 More than 200cm water is needed to reduce the BG to the PMT BG level 10-2 0 100 200 300 Thickness Distance [cm]
Key idea of XMASS: self-shielding effect for low energy events External g ray from U/Th-chain g tracking MC from external to Xenon All volume 20cm wall cut 30cm wall cut (10ton FV) U-chain gamma rays BG normalized by mass Large self-shield effect Large self-shield effect 0 1MeV 2MeV 3MeV Blue : g tracking Pink : whole liquid xenon Deep pink : fiducial volume Background are widely reduced in < 500keV low energy region
Expected sensitivities XMASS FV 0.5 ton year Eth = 5 keVee~25 p.e., 3s discovery w/o any pulse shape info. 10-4 106 • Large improvements will be expected Two order higher than experimental results so far. DAMA CRESTT 104 Edelweiss Edelweiss Al2O3 ZEPLIN1 10-6 Tokyo LiF 102 CRESTTII CDMSII Modane NaI Cross section to nucleon [pb] CRESST ZEPLIN2 Edelweiss2 XENON100 1 UKDMC NaI 10-8 XMASS(Ann. Mod.) NAIAD 10-2 XMASS 800kg SuperCDMS phase A XMASS(Sepc.) 10-10 10-4 Plots except for XMASS: http://dmtools.berkeley.edu Gaitskell & Mandic