cryogenic dark matter search - uc berkeley cosmology group · 2010-10-22 · 0.9 ± .3 events –...

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Cryogenic Dark Matter Search Cryogenic Dark Matter Search Todd Doughty Todd Doughty Cosmology in Northern California Cosmology in Northern California Lawrence Berkeley National Laboratory Lawrence Berkeley National Laboratory October 22, 2010 October 22, 2010 Current Status & Future Plans Current Status & Future Plans

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Page 1: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

Cryogenic Dark Matter SearchCryogenic Dark Matter Search

Todd DoughtyTodd DoughtyCosmology in Northern CaliforniaCosmology in Northern California

Lawrence Berkeley National LaboratoryLawrence Berkeley National LaboratoryOctober 22, 2010October 22, 2010

Current Status & Future PlansCurrent Status & Future Plans

Page 2: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

Motivation for WIMP SearchMotivation for WIMP Search

● Significant Portion of Mass Density of Universe

● Convergence of Particle Physics & Cosmology

– Relic DM Density σDM

≈ σWF

Page 3: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

Three Types of SearchesThree Types of Searches

Production Production (LHC)(LHC)

Indirect Detection Indirect Detection (Fermi, Pamela)(Fermi, Pamela)

Direct DetectionDirect Detection(CDMS, XENON)(CDMS, XENON)

Page 4: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

Direct Detection MethodsDirect Detection Methods

ScintillationScintillation

IonizationIonization PhononsPhonons

DAMA/NaI, ZEPLIN I, CLEAN, KIMS

XENON, LUX, WARP, ArDM, ZEPLIN II + III

First generation experiments

CDMS, Edelweiss

CRESST, ROSEBUD

~100 eV / photon

~10 meV / phonon ~10 eV / carrier pair

(non-cryo: PICASSO, COUPP, SIMPLE)

Page 5: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

CDMS DetectorsCDMS Detectors

Page 6: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

CDMS DetectorsCDMS DetectorsCharge SignalCharge Signal

Page 7: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

CDMS DetectorsCDMS DetectorsCharge SignalCharge Signal

Phonon SignalPhonon Signal

Page 8: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

CDMS DetectorsCDMS DetectorsCharge SignalCharge Signal

Phonon SignalPhonon Signal

Transition Edge SensorTransition Edge Sensor

Page 9: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

CDMS DetectorsCDMS DetectorsCharge SignalCharge Signal

Phonon SignalPhonon Signal

Transition Edge SensorTransition Edge Sensor

Page 10: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

Background Discrimination● Each Event● Multiple Dimensions

– Ionization Yield

• 133Ba• 252Cf

Page 11: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

Background Discrimination● Each Event● Multiple Dimensions

– Ionization Yield

• 133Ba• 252Cf

Page 12: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

Background Discrimination● Each Event● Multiple Dimensions

– Ionization Yield– Phonon Timing

• 133Ba• 252Cf

approximate signal region

Page 13: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

CDMS II: Results

● Final Results – 2009– 2 events in NR Band– Estimate Leakage:

0.9 ± .3 events– 23% chance both

events not Wimps● Analysis can't be significant

evidence for Wimps, but neither event can be rejected

● Z. Ahmed et al., Science Vol. 327, no. 5973 (2010)

CDMS IIDAMA

CoGeNT

Xenon100

Edelweiss IIZeplin

Page 14: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP Detector

● Primary background– Surface Events

Page 15: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP Detector

● Primary background– Surface Events

● New Detector - IZIP – Interdigitated

Electrodes

Page 16: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP DetectorSide 1 Charge Electrode +2VSide 1 Charge Electrode +2V

PhononPhononRailRail0V0V

Side 2 Charge Electrode -2VSide 2 Charge Electrode -2V

Page 17: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP DetectorΧΧ

Page 18: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

ee--

IZIP Detector

hh++

hh++hh++

ee--ee--

Page 19: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP Detector

hh++ hh++hh++

ee--ee--ee--

Page 20: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP DetectorΧΧ

Page 21: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP Detector

hh++hh++hh++ee

--

ee--ee--

Page 22: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP Detector

hh++hh++hh++ee--

ee--ee--

Page 23: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP Detector

● Primary background– Surface Events

● New Detector - IZIP – Interdigitated

Electrodes

Page 24: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

IZIP Detector

● Primary background– Surface Events

● New Detector - IZIP – Interdigitated

Electrodes– 1000:1 rejection

Cd-109 – Surface EventsCd-109 – Surface Events

Page 25: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

Future Plans

● SuperCDMS Soudan– 10 kg Ge– 2 years

● SuperCDMS SNOLab– 100 kg Ge– 3 years

● GEODM DUSEL– 1.5 Tons Ge

Page 26: Cryogenic Dark Matter Search - UC Berkeley Cosmology Group · 2010-10-22 · 0.9 ± .3 events – 23% chance both events not Wimps Analysis can't be significant evidence for Wimps,

California Institute of TechnologyZ. Ahmed, J. Filippini, S.R. Golwala, D. Moore, R.W. Ogburn

Fermi National Accelerator LaboratoryD. A. Bauer, F. DeJongh, J. Hall, D. Holmgren, L. Hsu, E. Ramberg, R.L. Schmitt, J. Yoo

Massachusetts Institute of TechnologyE. Figueroa-Feliciano, S. Hertel, S.W. Leman, K.A. McCarthy, P. Wikus

NIST *K. Irwin

Queen’s UniversityP. Di Stefano *, N. Fatemighomi *, J. Fox *, S. Liu *, P. Nadeau *, W. Rau

Santa Clara UniversityB. A. Young

Southern Methodist UniversityJ. Cooley

SLAC/KIPAC *E. do Couto e Silva, G.G. Godrey, J. Hasi, C. J. Kenney, P. C. Kim, R. Resch, J.G. Weisend

SuperCDMS CollaborationSuperCDMS CollaborationStanford UniversityP.L. Brink, B. Cabrera, M. Cherry *, L. Novak, M. Pyle, A. Tomada, S. Yellin

Syracuse UniversityM. Kos, M. Kiveni, R. W. Schnee

Texas A&MJ. Erikson *, R. Mahapatra, M. Platt *

University of California, BerkeleyM. Daal, N. Mirabolfathi, A. Phipps, B. Sadoulet, D. Seitz, B. Serfass, K.M. Sundqvist, T. Doughty*, D, Speller*

University of California, Santa BarbaraR. Bunker, D.O. Caldwell, H. Nelson, J. Sander

University of Colorado DenverB.A. Hines, M.E. Huber

University of FloridaT. Saab, D. Balakishiyeva, B. Welliver *

University of MinnesotaJ. Beaty, P. Cushman, S. Fallows, M. Fritts, O. Kamaev, V. Mandic, X. Qiu, A. Reisetter, J. Zhang

University of ZurichS. Arrenberg, T. Bruch, L. Baudis, M. Tarka

* new collaborators or new institutions in SuperCDMS* new collaborators or new institutions in SuperCDMS