Can the DAMA annual modulation be explained by Dark Matter?

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1 Can the DAMA annual modulation be explained by Dark Matter? Thomas Schwetz-Mangold MPIK, Heidelberg based on M. Fairbairn and T. Schwetz, arxiv: T. Schwetz, MPIK, 24 Nov 2008 p. 1

2 Outline Introduction Review on DM direct detection phenomenology recent DAMA/LIBRA results DAMA vs XENON/CDMS for spin-independent elastic DM scattering Non-standard DM halos Beyond SI elastic DM scattering Summary T. Schwetz, MPIK, 24 Nov 2008 p. 2

3 Introduction R. Kolb, CERN academic training 2008 T. Schwetz, MPIK, 24 Nov 2008 p. 3

4 Introduction T. Schwetz, MPIK, 24 Nov 2008 p. 4

5 The CDM paradigm a popular candidate for DM is a Weakly Interacting Massive Particle T. Schwetz, MPIK, 24 Nov 2008 p. 5

6 The CDM paradigm a popular candidate for DM is a Weakly Interacting Massive Particle in the following I will try to be as model independent as possible: I just assume that there is an unknown particle around in our galaxy with some mass m χ and interaction cross section σ, and consider the phenomenology for direct detection experiments no constraints from collider searches will be considered T. Schwetz, MPIK, 24 Nov 2008 p. 5

7 DM direct detection T. Schwetz, MPIK, 24 Nov 2008 p. 6

8 DM direct detection Look for recoil of DM-nucleus scattering: χ + N χ + N cnts / kg-detector mass / kev recoil energy E R : dn de R (t) = ρ χ m χ σ(q) 2µ 2 χ d 3 v f ( v,t) v>v min v }{{} η(e R,t) ρ χ q = 2ME R DM energy density, default: 0.3 GeV cm 3 momentum transfer µ χ = m χ M/(m χ + M) reduced DM/nucleus mass η(e R, t) integral over DM velocity distribution in lab frame T. Schwetz, MPIK, 24 Nov 2008 p. 7

9 Cross section in general there is a spin-independent and spin-dependent contribution to the DM-nucleon scattering cross section: σ(q) = σ SI (q) + σ SD (q) T. Schwetz, MPIK, 24 Nov 2008 p. 8

10 Cross section spin-independent: σ SI (q) = σ 0 F(q) 2, F(q) : nuclear form factor, (norm.: F(0) = 1) σ 0 = 2µ2 χ π [Zf p + (A Z)f n ] 2 σ p µ 2 χ µ 2 p A 2 for f p f n spin-dependent: σ SD = 32µ2 χg 2 F 2J + 1 [ a 2 p S pp (q) + a p a n S pn (q) + a 2 ns nn (q) ] a p, a n : S pp (q), S pn (q), S nn (q): couplings to proton and neutron nuclear structure functions T. Schwetz, MPIK, 24 Nov 2008 p. 9

11 Cross section spin-independent: σ SI (q) = σ 0 F(q) 2, F(q) : nuclear form factor, (norm.: F(0) = 1) σ 0 = 2µ2 χ π [Zf p + (A Z)f n ] 2 σ p µ 2 χ µ 2 p A 2 for f p f n spin-dependent: σ SD = 32µ2 χg 2 F 2J + 1 [ a 2 p S pp (q) + a p a n S pn (q) + a 2 ns nn (q) ] a p, a n : S pp (q), S pn (q), S nn (q): couplings to proton and neutron nuclear structure functions A 2 -enhancement of SI cross section T. Schwetz, MPIK, 24 Nov 2008 p. 9

12 Cross section spin-independent: σ SI (q) = σ 0 F(q) 2, F(q) : nuclear form factor, (norm.: F(0) = 1) σ 0 = 2µ2 χ π [Zf p + (A Z)f n ] 2 σ p µ 2 χ µ 2 p A 2 for f p f n consider first only SI contribution: dn de R (t) = ρ χ m χ σ p F(q) 2 A 2 2µ 2 p η(e R,t) T. Schwetz, MPIK, 24 Nov 2008 p. 10

13 Velocity distribution η(e R,t) = v>v min (E R ) d 3 v f ( v,t) v v = v : DM velocity in detector rest frame v min : minimal DM velocity required to produce recoil energy E R ME R v min = = m χ + M ER 2µ 2 χ m χ 2M T. Schwetz, MPIK, 24 Nov 2008 p. 11

14 Velocity distribution η(e R,t) = v>v min (E R ) d 3 v f ( v,t) v v = v : DM velocity in detector rest frame v min : minimal DM velocity required to produce recoil energy E R ME R v min = = m χ + M ER 2µ 2 χ m χ 2M obtain velocity distribution in Earth rest frame f from distribution in galaxy rest frame f gal : f ( v,t) = f gal ( v + v + v (t)) T. Schwetz, MPIK, 24 Nov 2008 p. 11

15 Velocity distribution f ( v,t) = f gal ( v + v + v (t)) standard halo model : Maxwellian velocity distribution N [exp( v 2 / v 2 ) exp ( vesc/ v 2 2 )] v < v esc f gal ( v) = 0 v > v esc with v = 220 km/s and v esc = 650 km/s T. Schwetz, MPIK, 24 Nov 2008 p. 12

16 Velocity distribution f ( v,t) = f gal ( v + v + v (t)) sun velocity: earth velocity: v = (0, 220, 0) + (10, 13, 7) km/s v (t) with v 30 km/s T. Schwetz, MPIK, 24 Nov 2008 p. 12

17 Velocity distribution integral 1000 center of galaxy: x-axis 800 v min for M = 118 GeV( 127 I), m = 10 GeV v z [km/s] d 3 v f ( v,t) v>v min v kev 5 kev E R = 10 kev v min = ME R 2µ 2 χ v y [km/s] T. Schwetz, MPIK, 24 Nov 2008 p. 13

18 Velocity distribution integral center of galaxy: x-axis v min for M = 118 GeV( 127 I), m = 10 GeV, E rec = 3 kev v z [km/s] Dec 2 nd June 2 nd d 3 v f ( v,t) v>v min v v y [km/s] T. Schwetz, MPIK, 24 Nov 2008 p. 13

19 Velocity distribution integral 2 ] 2 e v+vobs (t) v [ e v vobs (t) v dv vmin(er) η(er,t) 1 vobs(t) 100 v min s ME R 2µ 2 χ vmin = vobs(t) = v + v (t) DM mass [GeV] 10 M = 67.5 GeV (Ge), E rec = 10 kev v [km/s] velocity distribution [arb. units] Dec. 2 nd June 2 nd M = 118 GeV (I), E rec = 3 kev M = 21.4 GeV (Na), E rec = 3 kev v mean T. Schwetz, MPIK, 24 Nov 2008 p. 14

20 DAMA/LIBRA results T. Schwetz, MPIK, 24 Nov 2008 p. 15

21 The DAMA experiment search for a scinitillation signal in NaI crystals DAMA/NaI 87.3 kg 7 yr 0.29 t yr DAMA/LIBRA kg 4 yr 0.53 t yr total exposure: 0.82 t yr DAMA/LIBRA consists of 25 detectors, 9.70 kg each cm 2 T. Schwetz, MPIK, 24 Nov 2008 p. 16

22 The DAMA experiment search for a scinitillation signal in NaI crystals DAMA/NaI 87.3 kg 7 yr 0.29 t yr DAMA/LIBRA kg 4 yr 0.53 t yr total exposure: 0.82 t yr total single-hit scintillation signal in DAMA/LIBRA: 10 Rate (cpd/kg/kev) Energy (kev) 1 cnts/d/kg/kev events/kev in DAMA/LIBRA T. Schwetz, MPIK, 24 Nov 2008 p. 16

23 The DAMA annual modulation signal evidence for an annual modulation of the count rate: Bernabei et al., kev Residuals (cpd/kg/kev) DAMA/NaI (0.29 ton yr) (target mass = 87.3 kg) DAMA/LIBRA (0.53 ton yr) (target mass = kg) Time (day) T. Schwetz, MPIK, 24 Nov 2008 p. 17

24 The DAMA annual modulation signal fitting count rate with S 0 + A cos ω(t t 0 ): expectation for DM: T = 1 yr, t 0 = 152 (2nd June) T. Schwetz, MPIK, 24 Nov 2008 p. 18

25 The DAMA annual modulation signal fitting count rate with S 0 + A cos ω(t t 0 ): expectation for DM: T = 1 yr, t 0 = 152 (2nd June) 8.2σ evidence for annual modulationt. Schwetz, MPIK, 24 Nov 2008 p. 18

26 Energy dependence of the modulation signal 0.03 S m (cpd/kg/kev) Energy (kev) Z m (cpd/kg/kev) σ contours 6-14 kev 2-6 kev modulation signal at 2 6 kev above 6 kev no modulation fitting: S 0 + S m cos ω(t t 0 ) + Z m sin ω(t t 0 ) S m (cpd/kg/kev) with t 0 = 152, T = 1 yr T. Schwetz, MPIK, 24 Nov 2008 p. 19

27 Can this be explained by DM? T. Schwetz, MPIK, 24 Nov 2008 p. 20

28 Can this be explained by DM? Yes, the DAMA signal can be explained, but it is difficult to reconcile it with constraints from other experiments. T. Schwetz, MPIK, 24 Nov 2008 p. 20

29 Nuclear recoil signals Rafael Moriond EW 2008 T. Schwetz, MPIK, 24 Nov 2008 p. 21

30 Quenching DAMA measures energy in electron equivalent (kevee) only a fraction q of nuclear recoil energy E R is observable as scintillation signal in DAMA: with q Na = 0.3, q I = 0.09 E obs = q E R the energy threshold of 2 kevee implies a threshold in E R of 6.7 kev for Na and 22 kev for I. T. Schwetz, MPIK, 24 Nov 2008 p. 22

31 Channeling Drobyshevski, ; Bernabei et al., with a certain probability a recoiling nucleus will not interact with the crystal but loose its energy only electro-magnetically for such channeled events q 1 T. Schwetz, MPIK, 24 Nov 2008 p. 23

32 Channeling fraction of nuclear recoil events with q fraction 10-2 Iodine recoils Sodium recoils E R (kev) Bernabei et al., channeling is important for low energy recoils T. Schwetz, MPIK, 24 Nov 2008 p. 24

33 Channeling and DAMA there are four types of events in the NaI of DAMA: R DAMA (E) = x=na,i M x M Na + M I { [1 fx (E/q x )]R x (E/q x ) }{{} quenched } +f x (E)R x (E) }{{} channeled T. Schwetz, MPIK, 24 Nov 2008 p. 25

34 Channeling and DAMA there are four types of events in the NaI of DAMA: %, 99.73% CL (2 dof) Na channel fitting DAMA requires σ p [cm 2 ] I channel Na quench I quench v min = m χ + M m χ 400 km/s ER 2M m χ [GeV] T. Schwetz, MPIK, 24 Nov 2008 p. 26

35 Fitting DAMA %, 99.73% CL (2 dof) best fit: m χ = 12 GeV χ 2 min = 36.8 / 34 dof σ p [cm 2 ] local minimum: m χ = 51 GeV χ 2 min = 47.9 / 34 dof ( χ 2 = 11.1) m χ [GeV] T. Schwetz, MPIK, 24 Nov 2008 p. 27

36 Fitting DAMA %, 99.73% CL (2 dof) σ p [cm 2 ] χ 2 min best fit: m χ = 12 GeV = 36.8 / 34 dof local minimum: m χ = 51 GeV χ 2 min = 47.9 / 34 dof ( χ 2 = 11.1) m χ [GeV] energy shape of the modulation is important Chang, Pierce, Weiner, Fairbairn, TS, not included e.g., in Gondolo, Gelmini, hep-ph/ Petriello, Zurek, (only two bins: 2-6 kev and 6-14 kev) T. Schwetz, MPIK, 24 Nov 2008 p. 27

37 Energy spectrum of the modulation 0.04 counts / kg / day / kevee GeV, 1.3e-41 cm 2 51 GeV, 7.8e-42 cm 2 6 GeV, 2.8e-41 cm E [kevee] T. Schwetz, MPIK, 24 Nov 2008 p. 28

38 Fitting DAMA %, 99.73% CL (2 dof) best fit: m χ = 12 GeV σ p [cm 2 ] χ 2 min = 36.8 / 34 dof prediction for total rate must not exceed the observed number of events Chang, Pierce, Weiner, Fairbairn, TS, local minimum: m χ = 51 GeV χ 2 min = 47.9 / 34 dof ( χ 2 = 11.1) m χ [GeV] T. Schwetz, MPIK, 24 Nov 2008 p. 29

39 Prediction for total rate GeV, 1.3e-41 cm 2 51 GeV, 7.8e-42 cm 2 counts / kg / day / kevee E [kevee] R(E R ) = B(E R ) + R DM (E R ;m χ,σ p ) + A(E R ;m χ,σ p ) cosω(t t 0 ) in a given model R DM and A are not independent T. Schwetz, MPIK, 24 Nov 2008 p. 30

40 Constraints from other experiments CDMS: exposure threshold M CDMS-Si (2005) 12 kg day 7 kev 26 GeV CDMS-Ge (2008) kg day 10 kev 67 GeV both CDMS-Si and CDMS-Ge observe zero events XENON10: 7 bins from 4.6 to 26.9 kev, 316 kg day exposure 10 candidate events: (1, 0, 0, 0, 3, 2, 4) T. Schwetz, MPIK, 24 Nov 2008 p. 31

41 DAMA vs CDMS/XENON σ p [cm 2 ] XENON CDMS-Ge 90%, 99.73% CL (2 dof) CoGeNT DAMA CDMS-Si DAMA 90% CL region excluded by 90% CL XENON, CDMS bounds DAMA and XENON regions touch each other at 3σ ( χ 2 = 11.2) χ 2 min,glob (P 2%) = 62.9/(45 2) m χ [GeV] P PG = T. Schwetz, MPIK, 24 Nov 2008 p. 32

42 DAMA vs CDMS/XENON σ p [cm 2 ] XENON CDMS-Ge CoGeNT 90%, 99.73% CL (2 dof) DAMA no channeling DAMA CDMS-Si DAMA 90% CL region excluded by 90% CL XENON, CDMS bounds DAMA and XENON regions touch each other at 3σ ( χ 2 = 11.2) χ 2 min,glob (P 2%) = 62.9/(45 2) m χ [GeV] P PG = T. Schwetz, MPIK, 24 Nov 2008 p. 32

43 Non-standard DM halos? T. Schwetz, MPIK, 24 Nov 2008 p. 33

44 Via Lactea N-body DM halo simulation (234 million particles) Diemand, Kuhlen, Madau, astro-ph/ T. Schwetz, MPIK, 24 Nov 2008 p. 34

45 Via Lactea N-body DM halo simulation (234 million particles) Diemand, Kuhlen, Madau, astro-ph/ α 1 α R f 0.6 f R f T α T r [ kpc ] r [ kpc ] fitting radial and transvers distribution of Via Lactea data: [ (ṽ2 ) αr ] [ (ṽ2 ) αt ] 1 exp R 2πv T, exp T N R fr 2 N T ft 2 T. Schwetz, MPIK, 24 Nov 2008 p. 34

46 Via Lactea (a) 90%, 99.73% CL (2 dof) σ p [cm 2 ] CDMS-Ge DAMA Via Lactea χ 2 min,glob (P 2%) = 62.3/(45 2) XENON CDMS-Si P PG = m χ [GeV] T. Schwetz, MPIK, 24 Nov 2008 p. 34

47 CDMS-Ge CDMS-Ge Non-standard Maxwellian halos (b) 90%, 99.73% CL (2 dof) (c) 90%, 99.73% CL (2 dof) (d) CDMS-Ge 90%, 99.73% CL (2 dof) Maxwellian v = 110 km/s v R = 142 km/s v T = 63 km/s v esc = 450 km/s σ p [cm 2 ] global DAMA CDMS-Si σ p [cm 2 ] global CDMS-Si DAMA σ p [cm 2 ] DAMA CDMS-Si XENON XENON m χ [GeV] XENON m χ [GeV] m χ [GeV] T. Schwetz, MPIK, 24 Nov 2008 p. 35

48 CDMS-Ge CDMS-Ge Non-standard Maxwellian halos (b) 90%, 99.73% CL (2 dof) (c) 90%, 99.73% CL (2 dof) (d) CDMS-Ge 90%, 99.73% CL (2 dof) Maxwellian v = 110 km/s v R = 142 km/s v T = 63 km/s v esc = 450 km/s σ p [cm 2 ] global DAMA CDMS-Si σ p [cm 2 ] global CDMS-Si DAMA σ p [cm 2 ] DAMA CDMS-Si XENON XENON m χ [GeV] XENON m χ [GeV] m χ [GeV] asymmetric halo with small vel. dispersion gives reasonable fit rather extreme assumptions on halo poperties T. Schwetz, MPIK, 24 Nov 2008 p. 35

49 DM streams Gondolo, Gelmini, hep-ph/ ; Chang, Pierce, Weiner, v str = 900 km/s σ str = 20 km/s aligned with sun s motion 3% of halo DM density marginal solutions appear at m χ 2 and 4 GeV T. Schwetz, MPIK, 24 Nov 2008 p. 36

50 Beyond spin-independent elastic DM scattering spin-dependent scattering inelastic scattering DM scattering only on electrons T. Schwetz, MPIK, 24 Nov 2008 p. 37

51 Spin-dependent scattering in general there is a spin-independent and spin-dependent contribution to the DM nucleon scattering cross section: σ = σ SI + σ SD with σ SD = 32µ2 χg 2 F 2J + 1 [ a 2 p S pp (q) + a p a n S pn (q) + a 2 n S nn(q) ] a p, a n : S pp (q), S pn (q), S nn (q): couplings to proton and neutron nuclear structure functions remember: σ SI σ p (µ χ /µ p ) 2 A 2 F(q) 2 A 2 -enhancement T. Schwetz, MPIK, 24 Nov 2008 p. 38

52 Spin-dependent scattering coupling mainly to an un-paired nucleon: neutron proton 23 11Na even odd I even odd Xe, Xe odd even 73 32Ge odd even coupling with proton looks promising for DAMA T. Schwetz, MPIK, 24 Nov 2008 p. 39

53 Spin-dependent scattering coupling mainly to an un-paired nucleon: neutron proton 23 11Na even odd I even odd Xe, Xe odd even 73 32Ge odd even coupling with proton looks promising for DAMA BUT: strong constraint from Super-Kamiokande bound on neutrinos from DM annihilations in the sun Savage, Gelmini, Gondolo, Freese, Hooper, Petriello, Zurek, Kamionkowski, T. Schwetz, MPIK, 24 Nov 2008 p. 39

54 SD scattering: neutron-only coupling ΣΧn pb spin dependent a p 0, neutron only Savage, Gelmini, Gondolo, Freese, M WIMP GeV DAMA 7Σ 5Σ DAMA 3Σ 90 DAMA 7Σ 5Σ with channeling DAMA 3Σ 90 with channeling CRESST I TEXONO CoGeNT XENON 10 CDMS I Si CDMS II Ge T. Schwetz, MPIK, 24 Nov 2008 p. 40

55 SD scattering: proton-only coupling ΣΧp pb Savage, Gelmini, Gondolo, Freese, DAMA 7Σ 5Σ DAMA 3Σ 90 DAMA 7Σ 5Σ with channeling DAMA 3Σ 90 with channeling CRESST I TEXONO CoGeNT spin dependent a n 0, proton only M WIMP GeV Super K XENON 10 CDMS I Si CDMS II Ge constraint from COUPP: σ p SD 1 m χ 10 GeV T. Schwetz, MPIK, 24 Nov 2008 p. 41

56 Inelastic DM scattering Tucker-Smith, Weiner, hep-ph/ , hep-ph/ ; Chang, Kribs, Tucker-Smith, Weiner, in addition to the DM χ there exists an excited state χ, with a mass splitting m χ m χ = δ 100 kev 10 6 m χ elastic scattering χ + N χ + N is suppressed with respect to inelastic scattering χ + N χ + N T. Schwetz, MPIK, 24 Nov 2008 p. 42

57 Inelastic DM scattering v min [km/s] inelastic elastic Ge I, Xe m χ = 120 GeV, δ = 100 kev E R [kev] v inel min = ( ) 1 MER + δ 2MER µ χ v el min = MER 2 1 µ χ sampling only high-velocity tail of velocity distribution no events at low recoil energies targets with high mass are favoured T. Schwetz, MPIK, 24 Nov 2008 p. 43

58 Inelastic DM scattering Chang, Kribs, Tucker-Smith, Weiner, leads to very different event spectrum as in case of elastic scattering (exponentially falling) T. Schwetz, MPIK, 24 Nov 2008 p. 44

59 Inelastic DM scattering T. Schwetz, MPIK, 24 Nov 2008 p. 45

60 Inelastic DM scattering Chang, Kribs, Tucker-Smith, Weiner, XENON, ZEPLIN, and CRESST have seen already DM! T. Schwetz, MPIK, 24 Nov 2008 p. 46

61 DM scattering off electrons DAMA observes just scitillation light, XENON and CDMS require the coincidence of two signals If DM interacted only with electrons, it would not show up in XENON/CDMS but could provide the DAMA annual modulation. T. Schwetz, MPIK, 24 Nov 2008 p. 47

62 DM scattering off electrons To deposit 2 kev by χ + e χ + e the electron cannot be at rest explore scattering on electrons bound to the nucleus. E + (kev) 10 1 p = 5 MeV/c p = 1 MeV/c in NaI the e have p 0.5 MeV with a probability p = 0.1 MeV/c max. released energy for v χ = ( )c and θ = π m χo (GeV) Bernabei et al., T. Schwetz, MPIK, 24 Nov 2008 p. 48

63 DM scattering off electrons To deposit 2 kev by χ + e χ + e the electron cannot be at rest explore scattering on electrons bound to the nucleus ξσ e 0 (pb) in NaI the e have p 0.5 MeV with a probability m χo (GeV) Bernabei et al., T. Schwetz, MPIK, 24 Nov 2008 p. 48

64 Summary T. Schwetz, MPIK, 24 Nov 2008 p. 49

65 Summary DAMA observes an annual modulation of their count rate at a significance of 8.2σ. The phase is in agreement with DM scattering. T. Schwetz, MPIK, 24 Nov 2008 p. 50

66 Summary DAMA observes an annual modulation of their count rate at a significance of 8.2σ. The phase is in agreement with DM scattering. An interpretation of this signal in terms of SI elastic DM scattering is in conflict with bounds from XENON and CDMS at the level of 3σ. T. Schwetz, MPIK, 24 Nov 2008 p. 50

67 Summary DAMA observes an annual modulation of their count rate at a significance of 8.2σ. The phase is in agreement with DM scattering. An interpretation of this signal in terms of SI elastic DM scattering is in conflict with bounds from XENON and CDMS at the level of 3σ. Reconciling the data seems to require very extreme assumptions on DM halo properties. T. Schwetz, MPIK, 24 Nov 2008 p. 50

68 Summary Beyond spin-independent scattering: Spin-dependent scattering on protons can evade the bounds from XENON and CDMS, but then strong constraints from Super-Kamiokande indirect DM searches apply. T. Schwetz, MPIK, 24 Nov 2008 p. 51

69 Summary Beyond spin-independent scattering: Spin-dependent scattering on protons can evade the bounds from XENON and CDMS, but then strong constraints from Super-Kamiokande indirect DM searches apply. Inelastic DM scattering allows an explanation of the DAMA signal which is going to be tested soon by the CRESST experiment. T. Schwetz, MPIK, 24 Nov 2008 p. 51

70 Summary Beyond spin-independent scattering: Spin-dependent scattering on protons can evade the bounds from XENON and CDMS, but then strong constraints from Super-Kamiokande indirect DM searches apply. Inelastic DM scattering allows an explanation of the DAMA signal which is going to be tested soon by the CRESST experiment. DM scattering off electrons seems to be a phenomenologically valid explanation. T. Schwetz, MPIK, 24 Nov 2008 p. 51

71 Thank you for your attention! T. Schwetz, MPIK, 24 Nov 2008 p. 52

72 Additional slides T. Schwetz, MPIK, 24 Nov 2008 p. 53

73 Dropping the first energy bin %, 99.73% CL (2 dof) counts / kg / day / kevee GeV, 1.3e-41 cm 2 51 GeV, 7.8e-42 cm 2 6 GeV, 2.8e-41 cm 2 σ p [cm 2 ] global CDMS-Ge XENON without 1 st bin DAMA CDMS-Si E [kevee] m χ [GeV] χ 2 DAMA,min m DAMA χ,best χ 2 glob,min GOF χ 2 PG PG m glob χ,best default w/o 1 st bin T. Schwetz, MPIK, 24 Nov 2008 p. 54

74 Exclusion curves depend on energy threshold ex.: new evaluation of L eff in XENON: scintillation yield of Xe for nuclear recoils, relative to the zero-field scintillation yield for electron recoils at 122 kevee. E R = S1 L y L eff S e S n L eff 0.15 instead of 0.19 at low energies moves the threshold of 4.6 kev to about 6 kev Sorensen et al., T. Schwetz, MPIK, 24 Nov 2008 p. 55

75 Exclusion curves depend on energy threshold ex.: new evaluation of L eff in XENON: scintillation yield of Xe for nuclear recoils, relative to the zero-field scintillation yield for electron recoils at 122 kevee. E R = S1 L y L eff S e S n L eff 0.15 instead of 0.19 at low energies moves the threshold of 4.6 kev to about 6 kev E. idm2008, Stockholm T. Schwetz, MPIK, 24 Nov 2008 p. 55

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