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PICO 250-Liter Bubble Chamber Dark Matter Experiment Michael B PICO 250-liter Bubble Chamber Dark Matter Experiment Michael B. Crisler Fermi National Accelerator Laboratory 21 August 2013 M.B. Crisler SNOLAB Future Projects Workshop 1 PICO Collaboration C. Amole, M. Besnier, G. Caria, A. Kamaha, A. Noble, T. Xie M. Ardid, M. Bou-Cabo D. Asner, J. Hall D. Baxter, C.E. Dahl, M. Jin E. Behnke, H. Borsodi, C. Harnish, O. Harris, C. Holdeman, I. Levine, E. Mann, J. Wells P. Bhattacharjee, M. Das, S.J. Brice, D. Broemmelsiek, J.I. Collar, R. Neilson, S. Seth P.S. Cooper, M. Crisler, A.E. Robinson W.H. Lippincott, E. Ramberg, F. Debris, M. Fines-Neuschild, C.M. Jackson, M.K. Ruschman, M. Lafrenière, M. Laurin, L. Lessard, A. Sonnenschein J.-P. Martin, M.-C. Piro, A. Plante, O. Scallon, N. Dhungana, J. Farine, N. Starinski, V. Zacek R. Podviyanuk, U. Wichoski R. Filgas, S. Gagnebin, C. Krauss, S. Pospisil, I. Stekl D. Marlisov, P. Mitra I. Lawson, E. Vázquez Jáuregui D. Maurya, S. Priya PICASSO + COUPP = PICO New collaboration is PICO PICASSO Ongoing efforts with Superheated Droplet Detectors Committed to Geyser Chamber R&D through FY13 COUPP Ongoing efforts with COUPP-60 bubble chamber Committed to Fast-Compression Bubble Chamber R&D through FY13 M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 3 PICASSO + COUPP = PICO PICASSO focus on spin-dependent couplings Fluorine based fluids – C4F10 COUPP focus on simultaneous SI & SD couplings Fluorine and iodine - CF3I First Collaborative PICO Effort = PICO-2L: 2-liter C3F8 chamber at former COUPP-2L site Spin-dependent couplings + low mass SI M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 4 The Bubble Chamber Propylene Glycol fast compression Spin-indep (hydraulic fluid) Superheated CF3I target Spin-dep* Spin-dep C F –C F 3 8 4 10 Water Particle interactions (buffer) nucleate bubbles Cameras capture bubbles (target Data Logged, Chamber fluid) compressed after each event * This doesn’t work so well… M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 5 The Geyser Chamber hydraulic fluid Superheated target Spin-dep C3F8–C4F10 Particle interactions buffer nucleate bubbles fluid Cameras capture bubbles Data Logged, Chamber target compressed after each fluid event M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 6 The Geyser Chamber Idea: Add a cold condenser space at the top of the chamber volume Establish thermodynamic conditions so that bubbles rise to the top, condense, and the liquid falls back into the active volume Continuous operation without dead-time Eliminates the need for fast compression M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 7 Dark Matter Bubble Chamber Evolution Test tube COUPP 2kg PICO 0.01 COUPP 4kg PICO 0.1 PICO 1liter COUPP 60kg PICO 2liter PICO’ 2liter M.B. Crisler SNOLAB Future Projects PICO 250 liter 821 August 2013 Workshop The Physics of Bubble Nucleation Energy from particle interactions produces σ = surface tension P = liquid pressure “proto-bubbles” l Macroscopic bubbles arise from proto-bubbles Pv = vapor pressure with radius r > rc The energy threshold Eth is the energy required to produce a critical radius bubble Bubble nucleation requires ER > Eth and Surface energy Latent heat recoil path length < Rc Seitz “Hot Spike” Model Phys.&Fluids&1,&2&(1958) M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 9 The Physics of Bubble Nucleation Tune Temperature T and Pressure P for set nuclear recoil threshold. No sensitivity to electron recoils M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 10 The Bubble Chamber is a Threshold Device α-recoil We do not measure ER… dark matter ER …we measure dN dER dER Eth Eth …so bubbles initiated by recoiling α-decay daughters are counted along with dark matter candidate events. M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 11 The Physics of Bubble Growth PICASSO (Aubin et al., arXiv:0807.1536) Sound emission from a bubble peaks at rbubble ~ 10 um Clear acoustic signature for a single nuclear recoil α-decay results in separate nucleation sites ~ 40 µm α-decays are significantly louder Observable)bubble)~1)mm) ~40)μm) ~50)nm) Daughter)heavy)nucleus) Helium)nucleus) (∼100)keV)) (∼5)MeV)) M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 12 Acoustic Parameter (Amp • ω)2 (Normalized and position-corrected for each freq-bin) Measure of acoustic energy deposited in chamber Alphas are louder than neutrons M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 13 The Bubble Chamber fused silica inner vessel Flexible pressure balancing bellows Instrumented with Temperature, Pressure Transducers Fast Transient Pressure Transducer Piezo Electric Acoustic Transducers Immersed in hydraulic fluid within a stainless steel pressure vessel Hydraulic pressure controls the superheated fluid pressure Viewed by machine vision cameras M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 14 Bubble Chamber Operation Cycle M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 15 The Data Trigger frame 10 frames of Stereo Camera Images Synchronized measurements of Acoustic Traces P, T, and control parameters Pressure Growth 2.5 Mhz waveform digitizer for acoustics and fast pressure transducer. M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 16 Dark Matter Bubble Chambers Insensitive* to γ and β backgrounds Threshold device, integral distribution Event-by-event tagging of α-recoils Only background should be neutrons M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 17 Dark Matter Bubble Chambers Insensitive* to γ and β backgrounds * There is a catch here… Our γ and β rejection is not perfect, and the onset of gamma sensitivity limits the lowest viable operating threshold M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 18 Gamma Rejection Measurements Gamma rejection in C3F8 Gamma rejection in CF3I 10-10 ~ 12 keV 10-10 ~ 3 keV M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 19 Dark Matter Bubble Chambers Emin determines dark matter sensitivity For a velocity of 300 km/sec Eiodine = 63 keV so Emin = 12 keV is OK Efluorine = 9.5 keV so Emin = 12 keV is not OK Good sensitivity to fluorine recoils from dark matter requires a 2-3 keV threshold attainable only with C3F8 or C4F10 M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 20 NEW Explicit Confirmation of a sharp Bubble Nucleation Threshold for Iodine Recoils in CF3I Telescope trigger Acoustic signal -0.019 -0.018 -0.017 Time (s) Downstream pixel hits Upstream pixel hits Y position (mm) The Seitz Model works very well for iodine in CF3I Z position (mm) 1 cm diameter bubble chamber 12 GeV/c π- test beam M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 21 COUPP 4kg @ SNOLAB Excellent Rejection of Alpha Backgrounds in CF3I α rejection >98.9% α rejection > 99.3% 15 keV data COUPP-4 Dark Matter Sensitivity from CF3I was limited by backgrounds Neutrons 20 WIMP Anomalous* (CF3I related) candidates Not random in time Anomalous Background not yet understood M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 22 COUPP-60 at SNOLAB CF3I effort continues with COUPP-60 Operating since June 2013 >1000 kg-days Competitive for Spin-Independent M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 23 19 Problems with F response in CF3I …poor fluorine recoil nucleation efficiently NEW M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 24 Threshold and Efficiency: SRIM simulation* 19 12 15 keV F and C recoils in CF3I have tracks significantly longer than the critical radius for bubble formation …so fluorine recoils do not nucleate efficiently in CF3I fluorine recoils do nucleate efficiently in C3F8 M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 25 Gamma rejection sets the threshold. C3F8 for SD, low mass The 10-15 keV Threshold necessary for CF3I is kinematically unfavorable for 19F recoils Gamma rejection in C3F8 Gamma rejection in CF3I 10-10 ~ 12 keV 3 keV threshold Excellent Spin-dependent provides excellent 10-10 ~ 3 keV Plus Spin-Independent Low Mass sensitivity for 19F recoils M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 26 Dark Matter Sensitivity with C3F8 / CF3I −36 10 ] ] 2 2 −40 DAMA 10 bb) PICASSO 2012 PICASSO 2012 COUPP 2012 CoGent χχ → ) ( − −38 + W 10 CRESST K (soft) W PICO 2L − IceCube −42 Super χ → (χ 10 COUPP 2012 −K (hard) Super PICO 250L −40 CMS (A−V) CDMS 10 PICO 2L −44 proton cross section [cm nucleon cross section [cm − 10 C − 3 F XENON10/100 8 , 3 keV −60 PICO 250L COUPP , 3 keV F 8 −42 C 3 −46 PICO 250L SD WIMP 10 SI WIMP 10 I, 15 keV CF 3 1 2 3 4 1 2 3 10 10 10 10 10 10 10 WIMP mass [GeV/c2] WIMP mass [GeV/c2] M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 27 PICO-2L Focus on SD couplings low mass SI 2-liter C3F8 target Expect 3 keV threshold Installation in progress Physics this year M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 28 PICO 250-liter M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 29 250-L Bubble Chamber Design (1) Instrumentation, DAQ, Controls Synthetic Silica Inner vessel Bellows Assembly Optics, Photography Outer Pressure Vessel Hydraulic and Thermal Components M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 30 250-L Bubble Chamber Design (1) Instrumentation, DAQ, Controls Synthetic Silica Inner vessel Bellows Assembly Optics, Photography Outer Pressure Vessel Hydraulic and Thermal Components M.B. Crisler SNOLAB Future Projects 21 August 2013 Workshop 31 250-L Bubble Chamber Design (2) Shielding and Experiment Infrastructure Cleaning Infrastructure Assembly and Handling Fixtures Fluid purification Fluid handling Site Specific Engineering M.B.
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