Presentation is loading. Please wait.

Presentation is loading. Please wait.

Gaitskell CDMS II Status + CDMS I / III / CryoArray Direct Detection of SUSY Cold Dark Matter Rick Gaitskell Brown University, Department of Physics see.

Published byEdwina Harris Modified over 9 years ago

Similar presentations

Presentation on theme: "Gaitskell CDMS II Status + CDMS I / III / CryoArray Direct Detection of SUSY Cold Dark Matter Rick Gaitskell Brown University, Department of Physics see."— Presentation transcript:

1

2 Gaitskell CDMS II Status + CDMS I / III / CryoArray Direct Detection of SUSY Cold Dark Matter Rick Gaitskell Brown University, Department of Physics see information at http://cdms.brown.edu/ http://gaitskell.brown.edu/

3 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell CDMS Collaboration Santa Clara University B.A. Young Stanford University L. Baudis, P.L. Brink, B. Cabrera, C. Chang, T. Saab University of California, Berkeley V. Mandic, P. Meunier, N. Mirabolfathi, W. Rau, B. Sadoulet, A. Lu University of California, Santa Barbara D.A. Bauer, R. Bunker, D.O. Caldwell, R. Ferril, R. Mahapatra, H. Nelson, J. Sander, C. Savage, S. Yellin University of Colorado at Denver M. E. Huber University of Minnesota P. Cushman, L. Duong, A. Reisetter Brown University R.J. Gaitskell, J.-P. Thompson, M. J. Attisha, L de Viveiros Case Western Reserve University D.S. Akerib, D. Driscoll, S. Kamat, T.A. Perera, R.W. Schnee, G.Wang Fermi National Accelerator Laboratory M.B. Crisler, R. Dixon, D. Holmgren Lawrence Berkeley National Laboratory J.H Emes, R.R. Ross, A. Smith National Institute of Standards and Technology J. Martinis Princeton University T. Shutt

4 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell STATUS: CDMS II - Cold & Running “First Dark” achieved 12 detectors - cold & checked out @ SOUDAN  6 Ge+6 Si  Cryo / DAQ / Electronics / Analysis operating Tower 1 - currently  calib  Prev. 1/2 year @ Stanford - b/g well understood 120 live days (50 kg-days Ge) Tower not changed -> Soudan Will be some improvement at depth — Need stats to study bg (Prelim looks good) Tower 2  All New detectors Some improvements made in b/g handling Not yet measured b/g for this tower Initial Goal @ SOUDAN  Similar run to Stanford: 50 Ge kg-days  Looking for Zero background (ZBG) >10 keV Expect very clean analysis Tower 1 Previously 1/2 year run @ Stanford Tower 2 (New dets)

5 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell Direct Detection: History & Future Oroville (88) [m = ?? GeV - if significantly better limit obtained at different mass] 90% CL Limit on Cross section for 60 GeV WIMP (scalar coupling) ~1 event kg -1 day -1 ~1 event kg -1 yr -1 ~1 event 100 kg -1 yr -1 LHC Not meant to be a complete list - see http://dmtools.brown.edu Different Colours Indicate Different Technologies NOW 020921.7.rjg [m=20 GeV] Homestake (87) H-M (94) H’berg-Moscow (98), IGEX (00) DAMA (96) UKDMC (96) [m=100 GeV] DAMA (98) DAMA (00) Gaitskell (astroph 0106200) CDMS SUF (99) CDMS SUF (02) Edelweiss (98) Edelweiss (01) ZEPLIN I Xe (02) Edelweiss (02) DRIFT II 1 kg CS 2 (T) ZEPLIN II+III 10 kg Xe (T) XENON / ZEPLIN 1t Xe (T) CDMS Soudan (T) 7 kg Ge+Si Cryodet Majorana Phase 1 (T) GENINO (T) 100 kg Ge Diode GENIUS (T) 100 kg Ge Diode CryoArray (T) 0.1-1 tonne Cryodet DRIFT III 100 kg CS 2 (T) Ge NaI Cryodet (T) Target Signal Liq Xe Gas CS 2

6 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell Latest & Greatest Limits on Scalar C-S for WIMPs Latest Edelweiss result (updated May 2003) ZEPLIN I result (announced Sept 2002) CDMS I result (updated June 2003) ZEPLIN I - Liq nat130 Xe Edelweiss - nat72 Ge CDMS I Final http://dmtools.brown.edu ~1 event kg -1 day -1

7 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell Detectors provide near-perfect event-by-event discrimination against otherwise dominant electron-recoil backgrounds 616 Neutrons (external source) 1334 Photons (external source) CDMS Background Discrimination Explanation of basics (…On-going improvements in rejection) Ionization Yield (ionization energy per unit recoil energy) depends strongly on type of recoil Most background sources (photons, electrons, alphas) produce electron recoils WIMPs (and neutrons) produce nuclear recoils Ionization Threshold 233 Electrons (tagged contamination) Particles (electrons) that interact in surface “dead layer” of detector result in reduced ionization yield, very good (>95%) against surface electron-recoil backgrounds bulk > 1 / 2 year’s background >> 1 / 2 year’s signal !! NOT A SIMULATION! >98%

8 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell CDMS II - Calibrations at Stanford ZIP Detector (250g Ge, or 100 g Si)  20,400 gamma events (5-100 keV) ~ 1 week continuous calibration with 60 Co source  = ~one count in 12 years of gamma background (assuming project background level of 0.25 counts/keV/kg/day at CDMSII Soudan. Calibration still Poisson stats/neutron background limited )  Sensitivity better than 1 WIMP per year per detector Neutrons (external source) Gammas (external source) Trigger Threshold 1334 gamma events, 616 neutron events 010402.3.rjg

9 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell 380  m Al fins 60  m wide Photolithographic patterning like CMOS but 1 big chip 37 cells per quadrant 7x4 array of W transition-edge sensors per cell, with Al “collector” fins covering only fraction of surface ZIP Detector Phonon Sensor Close-up A B C D

10 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell Am 241 :  14, 18, 20, 26, 60 kev Cd 109 + Al foil :  22 kev Demonstration of xyZIP Position Sensitivity Cd 109 :  22 kev i.c. electr 63, 84 KeV Delay Plot AD CB

11 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell Working at Soudan

12 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell STATUS: CDMS II - Cold & Running “First Dark” achieved 12 detectors - cold & checked out @ SOUDAN  6 Ge+6 Si  Cryo / DAQ / Electronics / Analysis operating Tower 1 - currently  calib  Prev. 1/2 year @ Stanford - b/g well understood 120 live days (50 kg-days Ge) Tower not changed -> Soudan Will be some improvement at depth — Need stats to study bg (Prelim looks good) Tower 2  All New detectors Some improvements made in b/g handling Not yet measured b/g for this tower Initial Goal @ SOUDAN  Similar run to Stanford: 50 Ge kg-days  Looking for Zero background (ZBG) >10 keV Expect very clean analysis Tower 1 Previously 1/2 year run @ Stanford Tower 2 (New dets)

13 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell 1 per minute in 4 m 2 shield Depth (mwe) Log 10 (Muon Flux) (m -2 s -1 ) Stanford Underground Facility 500 Hz muons in 4 m 2 shield Expected Backgrounds for CDMS II at Soudan On track for 0.0003 events/kg/keV/day at 15 keV? Depth of 2000 mwe reduces neutron background from ~1 / kg / day to ~1 / kg / year Also better neutron shielding

14 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell 1999 Ge BLIP Ge Ga peak from 71 Ge: decays Expected Backgrounds for CDMS II at Soudan On track for 0.0003 events/kg/keV/day at 15 keV? Depth of 2000 mwe reduces neutron background from ~1 / kg / day to ~1 / kg / year Also better neutron shielding Photon background is already 0.7 events /(kg keV day) x 10 -3 expected leakage, despite the shallow site (good enough with background subtraction)

15 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell BLIP5 single Z1+Z2+Z3 Ge electrons single Expected Backgrounds for CDMS II at Soudan On track for 0.0003 events/kg/keV/day at 15 keV? Depth of 2000 mwe reduces neutron background from ~1 / kg / day to ~1 / kg / year Also better neutron shielding Photon background is already 0.7 events /(kg keV day) x <10 -3 expected leakage, despite the shallow test site Electron background is 0.1 events /(kg keV day) x ~0.04 expected leakage, despite the shallow site (need ~2x improvement from depth, or improvement from depth, or better surface screening/cleaning)

16 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell Latest & Greatest Limits on Scalar C-S for WIMPs CDMS II Initial goal 20x improvement over CDMS I ZeroBG 50 kg-days Ge ZEPLIN I - Liq nat130 Xe Edelweiss - nat72 Ge CDMS I Final http://dmtools.brown.edu ~1 event kg -1 day -1 Initial Goal 2003 CDMS II 20x ZBG 50 kg-days

17 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell CDMS I (1995-2001)  SI upper limits now eclipsed by EDELWEISS, Zeplin I except at low WIMP mass.  CDMS data are incompatible with DAMA signal for standard WIMPs & halo.  Sensitivity limited by neutrons from muons interacting in surrounding rock. CDMS II (2000-2005)  12 detectors (1.5 kg Ge, 0.6 kg Si) cold @ Soudan Stanford discrimination tests of 6 dets exceeded performance expectations. Stanford b/g testing showed expected reduction of neutron background by factor of ~2.3 due to installation of internal moderator (agreement with MC predictions.)  “First Dark” achieved Apr 2003. Initial Goal ~50 kg-days Ge (similar to previous run @ Stanford, but no neutrons!) CryoArray (2006 - 2017 or so…)  Sensitivity to study WIMP physics down to s~10 -46 cm 2 (many events if higher s   Modest improvements over current results (shared): Discrimination:  already good enough,  within factor few. Backgrounds: x20 reductions vs CDMS II, 2-3x vs best current IGEX, H-M R. Abusaidi et al., Phys. Rev. Lett. 84, 5699 (2000). D.Abrams et al., Phys. Rev. D astro-ph/0203500 v3 D.Akerib et al. Phys. Rev Lett. hep-ex/03060001 - Final Stanford Analysis CDMS Conclusions

18 Gaitskell Backup Slides Q&A (Not Used in Talk)

19 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell CryoArray: A 3 rd Generation Experiment Based on extrapolation of CDMS technology/strategy Basic parameters/goals  1000 kg x 2 (live) years  ~100 WIMPs at 10 -45 cm 2 ~10 WIMPs at 10 -46 cm 2  ~10’s background events Excellent discrimination so need little background reduction  Internal ( ,  ) and external (n) Main challenge:  Increase mass (~100x) and manufacturability of detectors/cryo package  Maintain Performance Possible sites  Soudan (CDMS II) among shallower sites (n background problematic)  National Underground Facility Depth Shared resources (vetos, assembly, materials screening, fabrication???) 10 4 – 10 5 increase over present limits 10 2 – 10 3 increase over expts under construction

20 CDMS Dark Matter - Aachen EPS - 17 July 2003 Rick Gaitskell Photon background is very manageable  Current lower limit on discrimination already good enough if raw rate reduced to 13 mdru, ~2-3 times better than best levels reached so far (by IGEX, H-M) achieve via materials selection and simplification of structures (little mounting material)  Screening to 10 -10 g/g can reveal contamination source of such a background Electron background more worrisome, but certainly tractable  Need to screen & clean surfaces to 2.5 x 10 -2 counts/ (keV m 2 day), or to 10x better if rejection remains only 95% -- novel but appears to be doable Background Projections - CryoArray (1 ton) dru = 1 event keV -1 kg -1 day -1 see Schnee, Gaitskell & Akerib astro-ph/0208326 Energy Range 15-45 keV

Download ppt "Gaitskell CDMS II Status + CDMS I / III / CryoArray Direct Detection of SUSY Cold Dark Matter Rick Gaitskell Brown University, Department of Physics see."

Similar presentations

Status of XMASS experiment Shigetaka Moriyama Institute for Cosmic Ray Research, University of Tokyo For the XMASS collaboration September 10 th, 2013.

Status of XMASS experiment Shigetaka Moriyama Institute for Cosmic Ray Research, University of Tokyo For the XMASS collaboration September 10 th, 2013.
EDELWEISS-I last results EDELWEISS-II prospects for dark matter direct detection CEA-Saclay DAPNIA and DRECAM CRTBT Grenoble CSNSM Orsay IAP Paris IPN.

EDELWEISS-I last results EDELWEISS-II prospects for dark matter direct detection CEA-Saclay DAPNIA and DRECAM CRTBT Grenoble CSNSM Orsay IAP Paris IPN.
DMSAG 14/8/06 Mark Boulay Towards Dark Matter with DEAP at SNOLAB Mark Boulay Canada Research Chair in Particle Astrophysics Queen’s University DEAP-1:

DMSAG 14/8/06 Mark Boulay Towards Dark Matter with DEAP at SNOLAB Mark Boulay Canada Research Chair in Particle Astrophysics Queen’s University DEAP-1:
Background Reduction in Cryogenic Detectors Dan Bauer, Fermilab LRT2004, Sudbury, December 13, 2004 Detector Shielding Veto U/Th/K/Rn ,n U/Th/K/Rn.

Background Reduction in Cryogenic Detectors Dan Bauer, Fermilab LRT2004, Sudbury, December 13, 2004 Detector Shielding Veto U/Th/K/Rn ,n U/Th/K/Rn.
Background issues for the Cryogenic Dark Matter Search Laura Baudis Stanford University.

Background issues for the Cryogenic Dark Matter Search Laura Baudis Stanford University.
Possible merits of high pressure Xe gas for dark matter detection C J Martoff (Temple) & P F Smith (RAL, Temple) most dark matter experiments use cryogenic.

Possible merits of high pressure Xe gas for dark matter detection C J Martoff (Temple) & P F Smith (RAL, Temple) most dark matter experiments use cryogenic.
Listening for the Dark Harry Nelson UCSB.

Listening for the Dark Harry Nelson UCSB.
Dark Matter Overview Harry Nelson UCSB INPAC Oct. 4, 2003.

Dark Matter Overview Harry Nelson UCSB INPAC Oct. 4, 2003.
1 Edelweiss-II status Eric Armengaud (CEA), for the Edelweiss Collaboration Axion-WIMPs training workshop, Patras, 22/06/2007.

1 Edelweiss-II status Eric Armengaud (CEA), for the Edelweiss Collaboration Axion-WIMPs training workshop, Patras, 22/06/2007.
The XENON Project A 1 tonne Liquid Xenon experiment for a sensitive Dark Matter Search Elena Aprile Columbia University.

The XENON Project A 1 tonne Liquid Xenon experiment for a sensitive Dark Matter Search Elena Aprile Columbia University.
CDMS (Cryogenic Dark Matter Search) Long Duong (University of Minnesota) Trinity School Seminar Jan 14, 2004 Introductory remarks Outline of physics concepts.

CDMS (Cryogenic Dark Matter Search) Long Duong (University of Minnesota) Trinity School Seminar Jan 14, 2004 Introductory remarks Outline of physics concepts.
The Search for Dark Matter The Cryogenic Dark Matter Search (CDMS)

The Search for Dark Matter The Cryogenic Dark Matter Search (CDMS)
PANDAX Results and Outlook

PANDAX Results and Outlook
Search for Dark Matter at CJPL with PANDAX

Search for Dark Matter at CJPL with PANDAX
30 Ge & Si Crystals Arranged in verticals stacks of 6 called “towers” Shielding composed of lead, poly, and a muon veto not described. 7.6 cm diameter.

30 Ge & Si Crystals Arranged in verticals stacks of 6 called “towers” Shielding composed of lead, poly, and a muon veto not described. 7.6 cm diameter.
W. RauSNOLAB workshop 2009 S u p e r C D M S Wolfgang Rau Queen’s University CDMS Technology Analysis and Results SuperCDMS Detector R&D Underground TF.

W. RauSNOLAB workshop 2009 S u p e r C D M S Wolfgang Rau Queen’s University CDMS Technology Analysis and Results SuperCDMS Detector R&D Underground TF.
The crystal is made of either silicon or germanium. This is the same material from which transistors and solar cells are made. The sensors employ state-of-the-art.

The crystal is made of either silicon or germanium. This is the same material from which transistors and solar cells are made. The sensors employ state-of-the-art.
ZEPLIN II Status & ZEPLIN IV Muzaffer Atac David Cline Youngho Seo Franco Sergiampietri Hanguo Wang ULCA ZonEd Proportional scintillation in LIquid Noble.

ZEPLIN II Status & ZEPLIN IV Muzaffer Atac David Cline Youngho Seo Franco Sergiampietri Hanguo Wang ULCA ZonEd Proportional scintillation in LIquid Noble.
Status of the Cryogenic Dark Matter Search (CDMS) Experiment Bruno Serfass University of California, Berkeley for the CDMS Collaboration Rencontres de.

Status of the Cryogenic Dark Matter Search (CDMS) Experiment Bruno Serfass University of California, Berkeley for the CDMS Collaboration Rencontres de.
Dan Bauer Fermilab Users Meeting June 3, 2004 Status of Cold Dark Matter Searches Dan Bauer, Fermilab Introduction Scientific case compelling for cold.

Dan Bauer Fermilab Users Meeting June 3, 2004 Status of Cold Dark Matter Searches Dan Bauer, Fermilab Introduction Scientific case compelling for cold.

Similar presentations

Ads by Google