Dark Matter Detection with Noble Liquids Aaron Manalaysay Physics - - PowerPoint PPT Presentation
Dark Matter Detection with Noble Liquids Aaron Manalaysay Physics Institute University of Zurich Rencontres de Rencontres de Moriond Moriond EW, La EW, La Thuile Thuile, , Aosta Aosta Valley, Italy, 18 March 2011 Valley, Italy, 18 March
Rencontres Rencontres de de Moriond Moriond EW, La EW, La Thuile Thuile, , Aosta Aosta Valley, Italy, 18 March 2011 Valley, Italy, 18 March 2011
2
Introduction Existing results Physics focus: low-mass WIMPs Ongoing and future experiments Prospects for constraining WIMP
Rencontres de Moriond EW: Dark matter detection with noble liquids
3
Zeplin I, II & III XENON10,100,1t LUX PANDAX LZS LZD ArDM WARP Dark Side MAX DARWIN CRESST ROSEBUD CDMS EDELWEISS COUPP PICASSO DAMA, KIMS, DEAP/CLEAN XMASS DRIFT, GERDA, PICASSO, CoGeNT CRESST I Charge Scintillation Vibration
Energy from a particle interaction goes where?
Talk by Steven Leman Talk by Fabiana Cossavella Talk by Ana Sofia Torrento Coello Talk by C Eric Dahl
He Ne Ar Kr Xe Rn
Rencontres de Moriond EW: Dark matter detection with noble liquids
4
Self shielding works High yield -> (~75, ~50 quanta/keV in LXe, LAr, respectively) means low thresholds 3-D position reconstruction capabilities Nuclear recoil discrimination (~10-3 in LXe, ~10-7 in LAr) Fast response (scintillation fast component at the ~few ns level) “Easy” cryogenics (boiling points: 165 K, 88 K for LXe and LAr, respectively) Extremely low attenuation of own scintillation light (compare with organic scintillators) LXe: Large nucleus (A~131) means large spin-independent cross section LXe: ~50% natural isotopes carry spin, giving spin-dependent sensitivity LXe: No long-lived radioisotopes LAr: Cheap and easily obtainable LAr: Capable of pulse shape discrimination
Rencontres de Moriond EW: Dark matter detection with noble liquids
5
Liquid Gas
Cathode Anode Grid Gate Grid
e- e- e- e-
PMT PMT PMT PMT PMT PMT PMT PMT
“ “S1 S1” ” “ “S2 S2” ” S1 S1 S2 S2
“S1 S1” ” = primary scintillation = primary scintillation
“S2 S2” ” = ionization signal = ionization signal “ “Dual-phase Time Projection Chamber (TPC) Dual-phase Time Projection Chamber (TPC)” ”
Rencontres de Moriond EW: Dark matter detection with noble liquids
e-
6
Rencontres de Moriond EW: Dark matter detection with noble liquids
7
Rencontres de Moriond EW: Dark matter detection with noble liquids
8
XMASS DARWIN MAX LZS ArDM WARP 100l WARP 2.3l LUX XENON1T XENON100 XENON10 Zeplin III Zeplin II Zeplin I DAMA LXe DEAP/CLEAN Green are those noble liquid experiments that have released DM results Dark Side * * * * * * * * * Four most-recent results * Four most-recent results PANDAX
Rencontres de Moriond EW: Dark matter detection with noble liquids
LZD
9
Collect background data Apply cuts to remove electronic
Look at the signal region
Rencontres de Moriond EW: Dark matter detection with noble liquids
10
arXiv:astro-ph/0701286
Exposure of 96.5 kg d, 55-100 keV ~10-42 cm2 sensitivity
Discrimination performed with BOTH ionization/scintillation ratio, AND pulse shape discrimination
WIMP search window Rencontres de Moriond EW: Dark matter detection with noble liquids
Dual-phase liquid argon TPC, operated at the Gran Sasso National Laboratory (LNGS, Assergi, Italy). First results released
11
Dual-phase liquid xenon TPC, operated at the Boulby mine (UK). 6.52 kg F.M. ~128 kg d exposure, 7 events in the signal region.
Rencontres de Moriond EW: Dark matter detection with noble liquids
12
Spin-Independent WIMP limits Spin-Independent WIMP limits ~10 ~10-43
cm2
2 sensitivity
sensitivity Spin-Dependent WIMP limits Spin-Dependent WIMP limits Inelastic WIMP limits Inelastic WIMP limits Currently Currently collecting more data with new collecting more data with new PMTs PMTs and and ~10 times lower background ~10 times lower background! !
Rencontres de Moriond EW: Dark matter detection with noble liquids
S-I results: V.N. : V.N.Lebedenko Lebedenko et al et al Phys.Rev.D Phys.Rev.D 80 80 (2009) 052010, (2009) 052010, arXiv arXiv:0812.1150 [ :0812.1150 [astro-ph astro-ph] ]
S-D results: V.N. : V.N.Lebedenko Lebedenko et al et al Phys.Rev. Phys.Rev.Lett Lett. . 103 103 (2009) 151302, (2009) 151302, arXiv arXiv:0901.4348 [ :0901.4348 [hep-ex hep-ex] ]
iDM results results: D.Yu. : D.Yu.Akimov Akimov et al et al arXiv arXiv:1003.5626v2 [ :1003.5626v2 [hep-ex hep-ex] 2010 ] 2010
13
Dual-phase liquid xenon TPC, operated at LNGS (Italy). 5.4 kg F.M. ~136 kg d exposure, 10 events in the signal region.
Rencontres de Moriond EW: Dark matter detection with noble liquids
14
Spin-Independent WIMP limits Spin-Independent WIMP limits ~5x10 ~5x10-44
cm2
2 sensitivity
sensitivity Spin-Dependent WIMP limits Spin-Dependent WIMP limits Inelastic WIMP limits Inelastic WIMP limits
XENON10 XENON10
Rencontres de Moriond EW: Dark matter detection with noble liquids
S-I results: : J.Angle J.Angle et al et al, Phys.Rev. , Phys.Rev.Lett Lett. . 100 100 (2008) 021303, (2008) 021303, arXiv arXiv:0706.0039 [ :0706.0039 [astro-ph astro-ph] ]
S-D results: : J.Angle J.Angle et al et al, Phys.Rev. , Phys.Rev.Lett Lett. . 101 101 (2008) 091301 (2008) 091301, , arXiv arXiv:0805.2939 [ :0805.2939 [astro-ph astro-ph] ]
iDM results results: : J.Angle J.Angle et al et al, Phys.Rev.D , Phys.Rev.D 80 80 (2009) 115005, (2009) 115005, arXiv arXiv:0910.3698 :0910.3698
15
Dual-phase liquid xenon TPC, operated at the LNGS (Italy). 40 kg F.M. ~156 kg d exposure, 0 events in the signal region. Still collecting data! (~2 tonne d blind!)
Rencontres de Moriond EW: Dark matter detection with noble liquids
16
Spin-Independent limits only for now, Spin-Independent limits only for now, at the ~3.5x10 at the ~3.5x10-44
cm cm2
2 level
level
Rencontres de Moriond EW: Dark matter detection with noble liquids
S-I results: : E. E.Aprile Aprile et al et al, Phys.Rev. , Phys.Rev.Lett Lett. . 105 105 (2010) 131302, (2010) 131302, arXiv arXiv:1005.0380 [ :1005.0380 [astro-ph astro-ph.CO] .CO]
E.Aprile Aprile et al et al, , arXiv arXiv:1103.0303 [ :1103.0303 [hep-ex hep-ex] ]
17
Rencontres de Moriond EW: Dark matter detection with noble liquids
18
CoGeNT CoGeNT Spectrum* Spectrum* DAMA/LIBRA Modulation Amplitude DAMA/LIBRA Modulation Amplitude!
!
*C.E. *C.E.Aalseth Aalseth et al et al, , arXiv arXiv:1002.4703v2 [ :1002.4703v2 [astro-ph astro-ph.CO] .CO]
! !R.
R.Bernabei Bernabei et al et al, , Eur Eur.Phys.J. .Phys.J. C67 C67 (2010) 39-49 (2010) 39-49
Possible signal Possible signal detection in the two detection in the two searches that searches that use no use no rejection of rejection of electromagnetic electromagnetic backgrounds backgrounds
Rencontres de Moriond EW: Dark matter detection with noble liquids
19
WIMP Mass [GeV/c WIMP Mass [GeV/c2
2]
] XENON100 XENON100’ ’s reported limit for low-mass s reported limit for low-mass WIMPs WIMPs depends strongly on how one depends strongly on how one reconstructs the reconstructs the energy scale. This energy scale. This reconstruction is quantified by the reconstruction is quantified by the parameter parameter “ “L Leff
eff”
” (the (the “ “effective effective Lindhard Lindhard factor factor” ”). ). L Leff
eff
quantifies the nonlinear relationship quantifies the nonlinear relationship between the energy of a nuclear recoil between the energy of a nuclear recoil and the average and the average number of number of scintillation photons it produces. scintillation photons it produces. Two limits based Two limits based
reconstructed reconstructed energy scales energy scales
Rencontres de Moriond EW: Dark matter detection with noble liquids
20
energy of nuclear recoil (NR)
measured signal in p.e.
quenching of scintillation yield for 122 keV due to drift field light yield for 122 keV in p.e./keV relative scintillation efficiency of NR to 122 keV at zero field quenching of scintillation yield for NR due to drift field V. V.Chepel Chepel et al et al, , Astropart Astropart.Phys. .Phys. 26 26 (2006) 58 (2006) 58 E. E.Aprile Aprile et al et al, Phys.Rev.C , Phys.Rev.C 79 79 (2009) 045807 (2009) 045807 A. A.Manzur Manzur et al et al, Phys.Rev.C , Phys.Rev.C 81 81 (2010) 025808 (2010) 025808
see A.Manalaysay, see A.Manalaysay, arXiv arXiv:1007.3746 [ :1007.3746 [astro-ph astro-ph.IM] .IM]
This discrepancy causes some tension in the field This discrepancy causes some tension in the field… …
Rencontres de Moriond EW: Dark matter detection with noble liquids
21
C.Savage, G. C.Savage, G.Gelmini Gelmini, P. , P.Gondolo Gondolo, K. , K.Freese Freese, , Phys.Rev.D Phys.Rev.D 83 83 (2011) 055002, (2011) 055002, arXiv arXiv:1006.0972 [ :1006.0972 [astro-ph astro-ph.CO] .CO]
C.Savage has done a thorough investigation C.Savage has done a thorough investigation
Leff on the
low-mass limits for low-mass limits for both XENON10 and both XENON10 and XENON100. XENON100.
Rencontres de Moriond EW: Dark matter detection with noble liquids
22
Rencontres de Moriond EW: Dark matter detection with noble liquids
What if we want to avoid What if we want to avoid L Leff
eff?
? Dual-phase Dual-phase TPCs TPCs also also measure measure
measurements of the nuclear recoil measurements of the nuclear recoil ionization yield in LXe are not only ionization yield in LXe are not only consistent with one another, they consistent with one another, they show a rise show a rise at low energies at low energies! !
plot from: A. plot from: A.Manzur Manzur et al et al, Phys.Rev.C , Phys.Rev.C 81 81 (2010) 025808 (2010) 025808
XENON10 XENON10’ ’s hardware trigger was based on s hardware trigger was based on the ionization signal. In one background the ionization signal. In one background run, the trigger threshold was at the single run, the trigger threshold was at the single electron level electron level! ! After fiducial cuts, there After fiducial cuts, there remained 4 events in 5.8 kg d above a remained 4 events in 5.8 kg d above a threshold of 1.6 threshold of 1.6 keV. keV.
See P.Sorensen et al, See P.Sorensen et al, arXiv arXiv:1011.6439 [ :1011.6439 [astro-ph astro-ph.IM] .IM]
23
Rencontres de Moriond EW: Dark matter detection with noble liquids
What if we want to avoid What if we want to avoid L Leff
eff?
? Dual-phase Dual-phase TPCs TPCs also also measure measure
measurements of the nuclear recoil measurements of the nuclear recoil ionization yield in LXe are not only ionization yield in LXe are not only consistent with one another, they consistent with one another, they show a rise show a rise at low energies at low energies! !
plot from: A. plot from: A.Manzur Manzur et al et al, Phys.Rev.C , Phys.Rev.C 81 81 (2010) 025808 (2010) 025808
XENON10 XENON10’ ’s hardware trigger was based on s hardware trigger was based on the ionization signal. In one background the ionization signal. In one background run, the trigger threshold was at the single run, the trigger threshold was at the single electron level electron level! ! After fiducial cuts, there After fiducial cuts, there remained 4 events in 5.8 kg d above a remained 4 events in 5.8 kg d above a threshold of 1.6 threshold of 1.6 keV keV
See P.Sorensen et al, See P.Sorensen et al, arXiv arXiv:1011.6439 [ :1011.6439 [astro-ph astro-ph.IM] .IM]
XENON10 S2-only (no discrimination)
See IDM2010 talk by P.Sorensen:
http://indico.in2p3.fr/contributionDisplay.py?sessionId=15&contribId=89&confId=1565
CoGeNT CoGeNT signal signal
24
XMASS DARWIN MAX LZS ArDM WARP 100l LUX XENON1T XENON100 Zeplin III DEAP/CLEAN Dark Side PANDAX Current and Current and next-ish next-ish generation noble liquid DM generation noble liquid DM searches searches Ultimate Ultimate generation generation ( (multi-tonne multi-tonne) )
Rencontres de Moriond EW: Dark matter detection with noble liquids
LZD DARWIN DARWIN MAX MAX
25
Rencontres de Moriond EW: Dark matter detection with noble liquids
M. M.Pato Pato, L.Baudis, G. , L.Baudis, G.Bertone Bertone, R.Ruiz, L. , R.Ruiz, L.Strigari Strigari, R. , R.Trotta Trotta, , arXiv arXiv:1012.3458 [ :1012.3458 [astro-ph astro-ph.CO] (accepted in PRD) .CO] (accepted in PRD)
The constraining power of three targets at the targets at the multi-tonne multi-tonne scale is scale is shown for three benchmark cases. shown for three benchmark cases.
Assumptions here: Assumptions here:
1 tonne Ge tonne Ge, 3 yr op , 3 yr op
5 tonne Xe tonne Xe, 1yr op , 1yr op
10 tonne Ar tonne Ar, 1 yr op , 1 yr op Fixed astrophysics Fixed astrophysics
These are the corresponding constraints if constraints if uncertainties in uncertainties in the the astrophysical models are also astrophysical models are also
parameter parameter degeneracies degeneracies) )
Including Including astrophysical astrophysical uncertainties uncertainties
26
Rencontres de Moriond EW: Dark matter detection with noble liquids
M. M.Pato Pato, L.Baudis, G. , L.Baudis, G.Bertone Bertone, R.Ruiz, L. , R.Ruiz, L.Strigari Strigari, R. , R.Trotta Trotta, , arXiv arXiv:1012.3458 [ :1012.3458 [astro-ph astro-ph.CO] (accepted in PRD) .CO] (accepted in PRD)
Assumptions here: Assumptions here:
1 tonne Ge tonne Ge, 3 yr op , 3 yr op
5 tonne Xe tonne Xe, 1yr op , 1yr op
10 tonne Ar tonne Ar, 1 yr op , 1 yr op
Or one can do a self-calibration Or one can do a self-calibration by by considering the considering the astrophysicals astrophysicals as free as free parameters parameters as well as well. . In this way, it may In this way, it may be possible to constrain be possible to constrain also the also the astrophysical parameters even better astrophysical parameters even better than they are currently measured. But than they are currently measured. But to do this requires signals in to do this requires signals in complementary complementary target nuclei. target nuclei.
27
and background reduction.
with current sensitivities at the level of a ~few 10-44.
depends strongly on the choice of energy scale, but can nonetheless exclude a large portion of parameter space favored by DAMA/LIBRA and CoGeNT.
stringent limits on low-mass WIMPs, excluding CoGeNT.
sensitivity and potentially be able to constrain both particle and astrophysical dark matter parameters.
Rencontres de Moriond EW: Dark matter detection with noble liquids
Thanks for your attention Thanks for your attention! !
28
Rencontres de Moriond EW: Dark matter detection with noble liquids
29
Rencontres de Moriond EW: Dark matter detection with noble liquids
Zeplin I, II & III XENON10,100,1t LUX PANDAX LZS LZD ArDM WARP Dark Side MAX DARWIN CRESST ROSEBUD CDMS, EDELWEISS, COUPP, PICASSO DAMA, KIMS, DEAP/CLEAN XMASS DRIFT, GERDA, CoGeNT CRESST I Charge Scintillation Vibration
Energy from a particle interaction goes where?
Backgrounds in these experiments are Backgrounds in these experiments are predominantly electronic recoils (gamma, beta), predominantly electronic recoils (gamma, beta), so we need need a technique for so we need need a technique for identifying/rejecting these interactions from a identifying/rejecting these interactions from a DM search. DM search.
30
+R +e- R* R++e- R2
+
R2
*
R**+ R +R 2R
Excitation Ionization
E
Scintillation wavelength (singlet/triplet times) LXe: 178 nm (3 ns / 27 ns) LAr: 125 nm (5 ns / 1.6 µs)
“R” = noble liquid atom
An applied E field can partially interrupt this step to collect these electrons
Rencontres de Moriond EW: Dark matter detection with noble liquids
31
+R +e- R* R++e- R2
+
R2
*
R**+ R +R 2R
Excitation Ionization
E
Scintillation wavelength (singlet/triplet times) LXe: 178 nm (3 ns / 27 ns) LAr: 125 nm (5 ns / 1.6 µs)
“R” = noble liquid atom
Nuclear recoil discrimination uses the Nuclear recoil discrimination uses the ratio of electrons/photons, and/or ratio ratio of electrons/photons, and/or ratio
e/ph e/ph ratio ratio gives electronic recoil rejection at gives electronic recoil rejection at the level of ~99.5-99.9%. the level of ~99.5-99.9%. In liquid argon, In liquid argon, combining that with the sing/trip ratio combining that with the sing/trip ratio gives 99.99999-99.999999% rejection! gives 99.99999-99.999999% rejection!
Rencontres de Moriond EW: Dark matter detection with noble liquids
32
Dual-phase liquid argon TPC, operated at the Gran Sasso National Laboratory (LNGS, Assergi, Italy). First results released 2007. 3.2 kg F.M., 100 kg d exposure.
Rencontres de Moriond EW: Dark matter detection with noble liquids