Particle Physics at the Dark Frontier
Jocelyn Monroe, MIT 10th Anniversary of the Pappalardo Fellowships in Physics Symposium October 8, 2010
Monday, April 18, 2011 Standard Model of Cosmology
(NASA) Dark matter is ~25% of the universe.
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 ? ?#@! (NASA) We only understand 4% of the universe.
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Standard Model of Particle Physics (FNAL Public Affairs) Public (FNAL
Dark matter? None of the above.
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Dark Matter Candidates
strong e.m.
weak ? interaction
strengths HEPAP/AAAC DMSAG Subpanel (2007)
gravity
masses
neutrino electron t-quark Jocelyn Monroe ? October 8, 2010 Monday, April 18, 2011 Direct Detection Signal: χN ➙χN’
χ
Backgrounds: n N ➙ n N’ γ e- ➙ γ e-’ N ➙ N’ + α, e- ν N ➙ ν N’
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Direct Detection χ Signal: χN ➙χN’
χ
Backgrounds: n N ➙ n N’ γ e- ➙ γ e-’ N ➙ N’ + α, e- ν N ➙ ν N’
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Direct Detection χ Signal: χN ➙χN’
χ Heat
Backgrounds: n N ➙ n N’ γ e- ➙ γ e-’ N ➙ N’ + α, e- ν N ➙ ν N’
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Direct Detection χ Signal: χN ➙χN’
χ Heat
Ionization
Backgrounds: n N ➙ n N’ γ e- ➙ γ e-’ N ➙ N’ + α, e- ν N ➙ ν N’
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Direct Detection χ Signal: χN ➙χN’ Scintillation
χ Heat
Ionization
Backgrounds: n N ➙ n N’ γ e- ➙ γ e-’ N ➙ N’ + α, e- ν N ➙ ν N’
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 DRIFT IGEX WARP Newage Picasso ArDM COUPP ZeplinIII Ionization! CDMS Edelweiss Xenon100 LUX CoGeNT
DMTPC Heat!
ANaIs DEAP/CLEAN Scintillation! XMASS KIMS Dama/LIBRA CRESST
CRESSTII ROSEBUD
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Observable
1 bullet fired 1E3 J χ
lift an apple 1 meter 1 J χ
N 1E-7 J 1 flying mosquito
1E-11 J 1 nuclear fission
Recoil Nucleus Kinetic Energy 1E-16 J dark matter-induced nuclear recoil (100 keV)
1E-19 J 1 visible photon
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Measurement Tiny signals!
theorist:
what model explains this rate?
see a signal or set a limit?
experimentalist: Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Measurement Tiny signals!
theorist:
what model explains this rate?
see a signal or set a limit?
experimentalist: Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Measurement Tiny signals!
theorist:
what model explains this rate?
see a signal or set a limit?
experimentalist: Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 The Low Background Frontier
1 event/kg/day
1 event/100 kg/day
1 event/100 kg/100 days
(http://dmtools.brown.edu) Gaitskell, Mandic, Fillipini
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 χ χ χ χ Motivation for Directional Z Dark Matter Detection: ? PAMELA N N e+ e- FermiLAT DAMA/Libra ATIC
CRESST-II W. Seidel, IDM2010
COGENT arXiv:1002.4703ATIC CDMS 0912.3592v1
Recent anomalies... new backgrounds? dark matter? a definitive test of the astrophysical origin of a candidate dark matter signal.
Monday, April 18, 2011 The Dark Matter Wind “blows” from Cygnus
search for a dark matter source
Simulated Dark Matter Sky Map
simulated reconstructed dark matter sky map: search for anisotropy astro-ph/0609115
Unambiguous proof: Correlation of WIMP-induced nuclear recoil signal with galactic motion
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Directional Detection
0.18 recoiling 0.16 nucleus 0.14 0.12 0.1 0.08 Events /kg / day 0.06 0.04 0.02 0 Recoil020 Kinetic Energy (keV) 1 4060 0.60.8 80 0.20.4 LAB ) 100120 0 ! 140 -0.2 Cos( 160 -0.6-0.4 180200 -1-0.8
Daily direction modulation: asymmetry ~ 20-100% in forward-backward event rate. Spergel, Phys. Rev. D36:1353 (1988)
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Directionality Around the World
DRIFT: in Boulby (UK), wire readout, CS2 CF4 gas, negative ion drift, competitive kg-day exposure S. Burgos et al., Astropart. Phys. 28, 409 (2007)
NEWAGE: in Kamioka, μ-pattern gas detector readout, CF4 gas, first directional dark matter limit! K. Miuchi, et al., Phys.Lett.B654:58-64 (2007)
MiMAC-He3: (ILL) DMTPC: (Boston) above-ground R&D, in WIPP (US), He3 gas, MicroTPC CF4 gas, CCD readout, vector readout, A-dependence direction tag D. Santos, et al., J. Phys. Conf. Ser. 65, 021012 (2007) D. Dujmic, et al., NIM A 584:337 (2008)
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Principle 1. primary ionization encodes track direction via dE/dx profile χ
e- F 180Torr F
E - e 2. drifting electrons preserve dE/dx profile if diffusion is small 0V +3kV 3. avalanche multiplication in amplification region produces gain, scintillation photons
CCD camera 4. Recruit Pappalardo Fellows!
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Dark Matter Time Projection Chamber (DMTPC)
goal: directional dark matter detector with vector track reconstruction
Boston University S. Ahlen, H. Tomita**
MIT J. Battat, T. Caldwell*, C. Deaconu, D. Dujmic, W. Fedus, P. Fisher, S. Henderson**, A. Kaboth**, A. Lee, J. Lopez**, J. Monroe, E. Nardoni, T. Sahin*, G. Sciolla, R. Vanderspek, I. Wolfe, R. Yamamoto, H. Yegoryan*
Brandeis University H. Wellenstein. N. Skvorodnev *) undergraduate, **) graduate student
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 DMTPC circa 2006 D. Dujmic, et al., NIM A584:327-333 (2008)
neutron beam
CF4 gas 100-380Torr
1st head-tail measurement
Drift region: 2.6cm, E=580V/cm Amplification region: Anode: 5mm pitch, 100μm Ground: 2mm pitch, 50μm
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 DMTPC circa 2008 OLD (MWPC) Mesh Amplification Plane Pixel Number (Y)
CCD Pixel Number (X) readout ~28cm area NEW (Mesh) Pixel Number (Y) D. Dujmic et al., Astropart. Phys. 30 (2008) e- SS SS or Cu mesh Pixel Number (X) G10 20x smaller pitch, Resistive separators, dia=0.5mm, every 2.5cm 13x higher gain! Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Light readout DMTPC circa 2009 CCD (PMT) 1st long detector run & dark matter search!
“WIMP”
pixel Y calibration: -V neutron- induced
e- event F CCD image 0V +V Charge 0V readout pixel X
70
2 60
50
surface run Reduced Phi 40 -V 1D skymap 0 30
20 -2 Light readout 10 CCD (PMT) 0 50 100 150 200 E (keV) Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Light readout DMTPC circa 2009 CCD (PMT) 1st long detector run & dark matter search!
“WIMP”
pixel Y calibration: -V neutron- induced
e- event F CCD image 0V +V Charge 0V readout pixel X
70
2 60
50
surface run Reduced Phi 40 -V 1D skymap 0 30
20 -2 Light readout 10 CCD (PMT) 0 50 100 150 200 E (keV) Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Light readout DMTPC circa 2009 CCD (PMT) 1st long detector run & dark matter search!
“WIMP”
pixel Y calibration: -V neutron- induced
- event e r F E CCD image 0V +V Charge 0V readout pixel X r E 70 € 2 60 50
surface run Reduced Phi 40 -V 1D skymap 0 30 € 20 -2 Light readout 10 CCD (PMT) 0 50 100 150 200 E (keV) Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Light readout DMTPC circa 2009 CCD (PMT) 1st long detector run & dark matter search!
“WIMP”
pixel Y calibration: -V neutron- induced
e- event F CCD image 0V +V Charge 0V readout pixel X
70
2 60
50
surface run Reduced Phi 40 -V 1D skymap 0 30
20 -2 Light readout 10 CCD (PMT) 0 50 100 150 200 E (keV) Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Light readout DMTPC circa 2009 CCD (PMT) 1st long detector run & dark matter search!
“WIMP”
pixel Y calibration: -V neutron- induced
e- event F CCD image 0V +V Charge 0V readout pixel X
70
2 60
50
surface run Reduced Phi 40 -V 1D skymap 0 30
20 -2 Light readout 10 CCD (PMT) 0 50 100 150 200 E (keV) Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Backgrounds Alphas: edge crossing 20
15
10 Cf252 Data “WIMP” Data
Projected Range (mm) 5
0 0 200 400 600 800 Visible Energy (keV)
“Worms”: one hot pixel, large cluster rms
Cf252 Cf252 MC Data
Burn-In events: same position as sparks Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Recoil Candidates consistent with neutron background prediction:
10 α WIMP 15 search 8 window
6 10
C counts / 10 keV 4
Projected Range (mm) F 5 2
00 50 100 150 200 00 50 100 150 200 Recoil Energy (keV) Recoil Energy (keV)
surface neutron flux measurement: T. Nakamura, T. Nunomiya, S. Abe, K. Terunuma, and H. Suzuki, J. of Nucl. Sci. and Tech. 42 No. 10, 843 (2005). Rayleigh test of angular distribution: isotropy probability = 64% (first!) S. Ahlen et al., arXiv:1006.2928 Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 DMTPC c. 2010
2150 feet underground the Connex! where’s the dark matter?
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 October 2010 August 2010 Yamamoto Lab
PRELIMINARY Sept. 2010
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Physics is not for WIMPS!
MIT Physics Stats: 70+ faculty, 37 Pappalardo fellows, 4 nobel prize winners, 3 MacArthur Geniuses, etc., etc., AND 6 certified miners Monday, April 18, 2011 Progress in Directional Detection
-31 ) 10
NEWAGE limit 2 Newage directional (Kamioka) 10-32 results K. Miuchi et al., (cm p DMTPC 10L
Phys.Lett.B686:11-17 ! (2010) 10-34
DMTPC limit 10-36 (surface) S. Ahlen et al., arXiv:1006.2928 10-38
MSSM theory 10-40 102 103 WIMP mass (GeV)
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Progress in Directional Detection
-31 ) 10
NEWAGE limit 2 Newage directional (Kamioka) 10-32 results K. Miuchi et al., (cm p DMTPC 10L
Phys.Lett.B686:11-17 ! (2010) 10-34
DMTPC limit 10-36 (surface) S. Ahlen et al., arXiv:1006.2928 10-38
DMTPC projected MSSM theory sensitivity at WIPP, 10-40 2 3 1 year run, with 0 10 10 backgrounds WIMP mass (GeV)
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Progress in Directional Detection
-31 ) 10
NEWAGE limit 2 Newage directional (Kamioka) 10-32 results K. Miuchi et al., (cm p DMTPC 10L
Phys.Lett.B686:11-17 ! (2010) 10-34 DRIFT, DM2010 DMTPC limit 10-36 1D results (surface) COUPP, S. Ahlen et al., IDM2010 arXiv:1006.2928 10-38
DMTPC projected MSSM theory sensitivity at WIPP, 10-40 2 3 1 year run, with 0 10 10 backgrounds WIMP mass (GeV)
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Progress in Directional Detection
-31 ) 10
NEWAGE limit 2 Newage directional (Kamioka) 10-32 results K. Miuchi et al., (cm p DMTPC 10L
Phys.Lett.B686:11-17 ! (2010) 10-34 DRIFT, DM2010 DMTPC limit 10-36 1D results (surface) COUPP, S. Ahlen et al., IDM2010 arXiv:1006.2928 10-38
1m3 at WIPP MSSM theory 10-40 projected 3 102 10 sensitivity WIMP mass (GeV)
DMTPCino Next steps for DMTPC: low-background detector (Battat), funded! DMTPCino at WIPP (1m3) (Sciolla)
Monday, April 18, 2011 Directional Detection Future
3
-46 2 Eventually: large detector, 10 cm sensitivity, SuperK: sited at DUSEL? 40 x 40 x 40 m 3
SNO: 21 x 21 x 34 m 3 3 Observatory CMS: DMTPC 15 x 15 x 22 m 16 x 16 x 16 m
3 1 ton of CF4 MiniBooNE: @50Torr 6 x 6 x 6 m
detector size for 10-44 cm2 SI sensitivity
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Dark Frontier Horowitz et al, astro-ph/0302071 tonne scale, keV threshold, low background detectors have potential for first observations of...
12 ) 10 Supernova -1 11 pp 10 7 bin Be neutrinos in NC, flux and spectrum -1 10 13 s 10 N -2 109 15O 17 108 F 8B 40 107 with direction measurement: K geo- Flux (cm hep i 106 ) 105 -1 105 neutrinos, s 238 Solar 4 -2 U 10 4 10 235 CNO solar 3 U 10 3 10 232Th 102 neutrinos Flux (cm 40 i 102 K 10-1 1 10 Neutrino Energy (MeV) Geo 10 1
neutrino-nucleus coherent 10-1
elastic scattering of solar 10-2 neutrinos JM, P. Fisher, PRD76:033007 0.5 1 1.5 2 2.5 3 3.5 4 4.5 Anti-Neutrino Energy (MeV)
Jocelyn Monroe JM, E. Raymond, in preparation October 8, 2010 Monday, April 18, 2011 Directional detection is a powerful new way to search for dark matter.
Backgrounds make directional detection very attractive.
Huge progress experimentally in last few years: first directional experiment (DRIFT), first directional dark matter limit (NEWAGE), first observation of head-tail in low-energy nuclear recoils (DMTPC)
Dark matter telescope: transition from discovery to observatory.
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 DMTPC has had very significant support from the Pappalardo Fellowships Program
Thank Very You Much!
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Extra Slides
Monday, April 18, 2011 Spin-Dependent Cross Section Limits
current direct detection experiments
MSSM (http://dmtools.brown.edu) Gaitskell, Mandic, Fillipini
nb. does not show 20 Aug 2010 COUPP result ~0.1 pb
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011 Optimization how many events to detect the dark matter wind?
No background, 3-d vector read-out, ET = 20 keV
Detector Properties: detector resolution energy threshold background reconstruction (2D vs. 3D) vector or axial (A. M. Green, B. Morgan, astro-ph/0609115) reconstruction
Jocelyn Monroe October 8, 2010 Monday, April 18, 2011