The CoGeNT Dark Matter experiment
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1 The CoGeNT Dark Matter experiment Michael G. Marino 23 May
2 Outline Physics CoGeNT - Experiment + Technology Analysis, recent results Michael G. Marino 2 Neutrinos/DM 24 May 2012
3 Outline Physics CoGeNT - Experiment + Technology Analysis, recent results Michael G. Marino 3 Neutrinos/DM 24 May 2012
4 Dark matter What we know... Michael G. Marino 4 Neutrinos/DM 24 May 2012
5 Dark matter What we know... Normal Matter 5 % Dark Energy 72 % Dark Matter 23 % Michael G. Marino 4 Neutrinos/DM 24 May 2012
6 Dark matter: direct observation Green - mass contours from gravitational lensing Colors - X-rays from hot gas Picture of two colliding galaxy clusters Fig from Clowe et al., Astrophys J. Letters 648 (2006) L109 Michael G. Marino 5 Neutrinos/DM 24 May 2012
7 What about signals? Convincing signatures could include: Preferred scattering direction mass peak (non-wimp) } sensitivity Annual rate modulation P. Fisher with PPC/CoGeNT Michael G. Marino 6 Neutrinos/DM 24 May 2012
8 Annual Rate modulation Interaction rate dependent on relative velocity between detector and DM Figure: Michael G. Marino 7 Neutrinos/DM 24 May 2012
9 Outline Physics CoGeNT - Experiment + Technology Analysis, recent results Michael G. Marino 8 Neutrinos/DM 24 May 2012
10 Point-Contact Detectors P-type Point-Contact (P-PC) Germanium Geometry: low-capacitance, noise; long charge drift times Luke et al., IEEE trans. Nucl. Sci. 36, 926(1989). Michael G. Marino 9 Neutrinos/DM 24 May 2012
11 Point-Contact Detectors P-type Point-Contact (P-PC) Geometry: low-capacitance, noise; long charge drift times Michael G. Marino 10 Neutrinos/DM 24 May 2012
12 Detector Signals t [ns] 3!10 Channel: 4, Time (s): ADC ϒ, χ ADC ADC counts Channel: 0, Time (s): Channel: , Time (s): Unshaped: Pulse-shape analysis Shaped: Trigger, energy t [ns] 3! Time (μs) 400 t [ns] 0 Channel: 2, Time (s): Michael G. Marino 11 Neutrinos/DM 24 May 2012 C !10 3!10
13 CoGeNT Coherent Germanium Neutrino Technology (and then Dark Matter) Located underground (2100 meters water equivalent) to reduce background from cosmic ray muons Michael G. Marino 12 Neutrinos/DM 24 May 2012
14 grey vertical wall Slide: J. Orrell Michael G. Marino 13 Neutrinos/DM 24 May 2012
15 Initial deployment (previous detector) Pictures: J. Orrell, E. Fuller Michael G. Marino 14 Neutrinos/DM 24 May 2012
16 E. Fuller, J. Orrell Michael G. Marino 15 Neutrinos/DM 24 May 2012
17 Outline Physics CoGeNT - Experiment + Technology Analysis, recent results Michael G. Marino 16 Neutrinos/DM 24 May 2012
18 Extracting Physics What we have: Energy, Time data over two channels: High Energy 3 10 Events kev kev Low energy Energy (kev) Events Energy (kev) 4 Dec Mar live days, 458 days span Michael G. Marino 17 Neutrinos/DM 24 May 2012
19 Extracting Physics Energy spectrum (e.g. WIMP exclusion) PRL 106, (2011) Time (+ energy) spectrum (modulation) Subtraction analysis (U Chicago) 2-D ML fit analysis (U Washington) Michael G. Marino 18 Neutrinos/DM 24 May 2012
20 High Energy Peaks are from High Energy 65Zn 68Ga 68Ge electron-capture of cosmogenic Mn 55Fe isotopes in the 49V detector. 58Co 73As Each have K- Events 10 2 capture lines 10 (higher energy) Energy (kev) Michael G. Marino 19 Neutrinos/DM 24 May 2012
21 Low Energy Peaks are from electron-capture Low energy 220 of cosmogenic isotopes in the detector.... and associated Events L-capture lines (low energy) Energy (kev) Michael G. Marino 20 Neutrinos/DM 24 May 2012
22 Low Energy Peaks are from electron-capture Low energy 220 of cosmogenic isotopes in the detector.... and associated Events Zn 68Ge All the rest L-capture lines (low energy) Energy (kev) Michael G. Marino 20 Neutrinos/DM 24 May 2012
23 Time analysis 2-D time vs. energy analysis Simultaneous Max-likelihood fit over 2 channels Constrain L/K electron-capture peaks by their well-measured ratios Add oscillation PDF in low-energy channel Michael G. Marino 21 Neutrinos/DM 24 May 2012
24 2-D Model Visualization Michael G. Marino 22 Neutrinos/DM 24 May 2012
25 Crosscheck: Lifetimes 250 Expected Lifetime (days) Measured 50 Prelim 0 58 Co 68 Ge 51 Cr 73 As 65 Zn Michael G. Marino 23 Neutrinos/DM 24 May 2012
26 Prelim Model with Oscillation Raw data Livetime corrected Prelim NULL Model Michael G. Marino 24 Neutrinos/DM 24 May 2012
27 Phase vs. Period Best fit point: Phase σ 2 σ Phase: 49.9 d (Min ~23 Oct) Period: d Prelim Period (Years) Michael G. Marino 25 Neutrinos/DM 24 May 2012
28 Significance Relative counts / ndf 93.3 / 40 norm ± k ± Prelim Fit to χ2 dist *(ln L - ln L max (A=0)) max Generate many toy models of NULL hypothesis, fit to signal + background, calc: 2 (log L(B) max log L(B = 0)) Michael G. Marino 26 Neutrinos/DM 24 May 2012
29 Fit summary ML fit (Prelim) Min 23 Oct, Period: d, Ampl: 17.7 ± 6.5%, significance 94.6% Subtraction (U Chicago, arxiv: ) Min 16 Oct ± 12 d, period 347 ± 29 d, Ampl: 16.6 ± 3.8%, significance 99.4% But what is it? Michael G. Marino 27 Neutrinos/DM 24 May 2012
30 Muon modulation MINOS muon flux modulation measured in Soudan Approximately +/-1.5% Peaks three months after best fit to present CoGeNT data. A 1.5% modulation of the estimated 339 +/- 68 muon-induced events in shielding predicts a modulation of 5 events in the kevee energy range The CoGeNT data set contains 2124 events in the kevee energy range. A 5 event modulation of muon induced events could only produce a 0.2% modulation effect in the CoGeNT data set. Courtesy Alec T. Habig Slide: M. Kos, PNNL Michael G. Marino 28 Neutrinos/DM 24 May 2012
31 Radon Modulation Radon levels modulate underground Measured by MINOS Modulation out of phase! Also: Look at data out to 300 kev Infer the maximum number of events due to Rn in the data 2.8 events in kev Prelim CoGeNT Data Slide: M. Kos, PNNL Michael G. Marino 29 Neutrinos/DM 24 May 2012
32 Summary Recent CoGeNT data consistent with an annual modulation at low energies, PRL 107 (2011) , this is confirmed by two fully independent analyses Background analyses suggest muons and Rn can not account for this modulation, still investigating other possibilities Longer paper in preparation detailing analysis Detector is back up and running, data not yet analyzed, planned to open June 2012 Michael G. Marino 30 Neutrinos/DM 24 May 2012
33 CoGeNT collaboration C.E. Aalseth, 1 P.S. Barbeau, 2 J. Colaresi, 3 J.I. Collar, 2 J. Diaz Leon, 4 J.E. Fast, 1 N. Fields, 2 T.W. Hossbach, 1, 2 M.E. Keillor, 1 J.D. Kephart, 1 A. Knecht, 4 M.S. Kos, 1 M.G. Marino, 4 H.S. Miley, 1 M.L. Miller, 4 J.L. Orrell, 1 D.C. Radford, 5 J.F. Wilkerson, 6 and K.M. Yocum 3 (CoGeNT Collaboration) 1 Pacific Northwest National Laboratory, Richland, WA 99352, USA 2 Kavli Institute for Cosmological Physics and Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA 3 CANBERRA Industries, Meriden, CT 06450, USA 4 Center for Experimental Nuclear Physics and Astrophysics and Department of Physics, University of Washington, Seattle, WA 98195, USA 5 Oak Ridge National Laboratory, Oak Ridge, TN 37831, USA 6 Department of Physics and Astronomy, University of North Carolina, NC 27599, USA Michael G. Marino 31 Neutrinos/DM 24 May 2012
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