Exploring the Invisible Universe: From Discovery to Precision Measurements

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1 Exploring the Invisible Universe: From Discovery to Precision Measurements Karsten M. Heeger Yale University March 27, 2015 Karsten Heeger, Yale University Münster, April 10,

2 Our Universe Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

3 Fig: Murayama neutrinos are the most abundant particles in the Universe besides photons Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

4 330 neutrinos/cm 3. One billion more neutrinos than protons. Fig: Murayama neutrinos are the most abundant particles in the Universe besides photons Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

5 Cluster Cosmology in 1930s Fritz Zwicky In 1933, Zwicky used the virial theorem to infer the existence of dark matter in the Coma cluster.

6 Gravitational Evidence for Dark Evidence Matter for Dark Matter gravitational lensing rotation curves of galaxies Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

7 Bullet Cluster Mass distribution inferred from gravitational lensing (dark matter) X-ray emitting gas (most of the baryons) In 2005, the Bullet Cluster proved the existence of dark matter.

8 Neutrinos and Matter Heavy Elements: 0.03% Ghostly Neutrinos: ~0.3% Matter in the Universe Stars: 0.5% Free Hydrogen and Helium: 4% Dark Energy: 70% Dark Matter: 25% neutrinos are highly abundant but with little mass dark matter accounts for 85% of all matter 8 Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

9 Neutrinos and the Early Universe c at T ~ 1 MeV (~ 1 sec) neutrinos decouple relic neutrino spectrum left over at T < 100 kev deuterium formation, followed by BBN n+p d+γ at T < 1 ev (380,000 yrs) photons decouple, cannot break up atoms no more free charges to scatter photons Universe becomes transparent p+e - H+γ 9

10 Neutrinos and the Early Universe c 380,000 yrs now 10

11 s Massive Neutrinos Play a Role in Large Scale Structure of the Universe Even small neutrino mass influences power spectrum of galaxy correlations Neutrinos that are more massive cause more clustering on large scales. 11 Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

12 Neutrinos and Supernovae SN 1987A without neutrinos dying stars would not explode 12 Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009 neutrinos helped cook the light elements in the Universe

13 Early Days of the Neutrino Pauli, 1930 Chadwick, 1914 N N + e - some nuclei emit electrons! Reines and Cowan, 1956 Observation of the Free Antineutrino inverse beta decay ν e + p e + + n 13

14 First Proposal For Direct Detection of Neutrino 14

3ν flavors upper limits on m ν from kinematic

15 Neutrinos in the Standard Model Discovery of ν µ and ν τ Accelerator studies of ν The Standard Model 3ν flavors upper limits on m ν from kinematic studies. massless ν (ad hoc assumption in Standard Model) 15

Neutrino Astrophysics 1938 Bethe & Critchfield p + p 2 H + e + + ν e 1947 Pontecorvo,1949 Alvarez propose neutrino detection through 37Cl + ν e 37 Ar + e - Light Element Fusion Reactions p + p 2 H +

16 Neutrino Astrophysics 1938 Bethe & Critchfield p + p 2 H + e + + ν e 1947 Pontecorvo,1949 Alvarez propose neutrino detection through 37Cl + ν e 37 Ar + e - Light Element Fusion Reactions p + p 2 H + e + + ν e p + e - + p 2 H + ν e 99.75% 0.25% 2H + p 3 He + γ 85% ~15% ~10-5 % 3He + 3 He 4 He + 2p 3He + p 4 He + e + +ν e 3He + 4 He 7 Be + γ 1960 s Ray Davis builds chlorine detector. John Bahcall, generates first solar model calculations and ν flux predictions Be % + e - 7 Li + γ +ν e 7Li + p α + α 0.02% 7Be + p 8 B + γ 8B 8 Be* + e + + ν e to see into the interior of a star and thus verify directly the hypothesis of nuclear energy generation in stars... (Bahcall, 1964) 16

17 Cl-Ar Solar Neutrino Experiment at Homestake ν e + 37 Cl 37 Ar + e SSM only sensitive to ν e 17

18 Solar Neutrino Measurements with SNO ν e ν e ν e ν e Solar Neutrino Problem: Too few ν e observed from the Sun. Even with all solar neutrino fluxes as free parameters, cannot reproduce the data. P MSM < 1.7% at 95% CL KMH, Robertson PRL 77:3270 (1996) Sudbury Neutrino Observatory (SNO) Neutral-Current Charged-Current Elastic Scattering ν e + ν µ +ν τ ν e ν e (ν µ +ν τ ) model-independent test of flavor change 18

19 Solar Neutrino Measurements with SNO 2.0 Neutral Current (NC) Elastic Scattering (ES) Charged Current (CC) CC Neutral-Current shape Elastic Scattering Results from Charged-Current SNO, 2002 constrained SNO results, 2002 Neutrino Signal (SSM/BP00) SSM 5.3 σ CC shape unconstrained ν e + ν µ +ν τ Total Neutrino flux ν e (ν µ +ν τ ) ν e Electron Neutrino flux solar neutrinos change flavor total flux of active solar neutrinos agrees with solar models 19

20 Reactor Antineutrinos with KamLAND Reactors in Japan KamLAND Kamioka 1kt liquid scintillator detector 55 reactors mean, flux-weighted reactor distance ~ 180km reactor ν flux at KamLAND ~ 6 x 10 6 /cm 2 /sec 20

Evidence for Reactor ν e Disappearance KamLAND 2003 Reactor Neutrino Physics 1956-2003 PRL 90:021802 (2003)

1 ton-yr solar predicted KamLAND 0 0 50 100 Thermal Power Flux (µw/cm 2 ) 6 5 4 3 2 1 mean, flux-weighted

21 Evidence for Reactor ν e Disappearance KamLAND 2003 Reactor Neutrino Physics PRL 90: (2003) Observed ν e 54 events No-Oscillation 86.8 ± 5.6 events Background 1 ± 1 events Livetime: ton-yr solar predicted KamLAND Thermal Power Flux (µw/cm 2 ) mean, flux-weighted reactor distance ~ 180km Many reactors, far away Distance (km) 21 Survival Evis >2.6 MeV

22 Direct Evidence for Neutrino Oscillation Solar νe SNO Reactor νe KamLAND Φνμτ Φνe L/E 22

23 Neutrino Oscillation Neutrino Oscillation Imply Neutrino Mass there are at least 3 states... Mass States Mass states Weak states First First Second Second First First Second Second ν 1 ν 2 ν e a = sinθ ν e cos 1 cosθsin ν e 2 b = θ sin 1 + θ cos ν 1 2 ν µ ν 2 Weak States ν µ " sinθ ( ν ν ν e )% =( ) cosθ µ 2sinθ cosθ )( sinθ 1 ν )," $ 2 # ν ' = +. ν % 1 µ & * 2sinθ cosθ $ ' -# & ν 2 Pure ν µ Pure ν µ Pure ν µ Pure ν µ Pure ν µ Pure ν µ ν 2 2 ν 1 Pontecorvo, Time, t % L ( P i i = sin 2 2θ sin 2 ' 1.27Δm 2 * & E ) energy and baseline dependent osc frequency depends on Δm 2 amplitude depends on θ 23

24 Neutrino Oscillation Neutrino Oscillation Imply Neutrino Mass there are at least 3 states... Mass States Mass states Weak states First First Second Second First First Second Second ν 1 ν 2 ν e a = sinθ ν e cos 1 cosθsin ν e 2 b = θ sin 1 + θ cos ν 1 2 ν µ ν 2 Weak States ν µ " sinθ ( ν ν ν e )% =( ) cosθ µ 2sinθ cosθ )( sinθ 1 ν )," $ 2 # ν ' = +. ν % 1 µ & * 2sinθ cosθ $ ' -# & ν 2 Pure ν µ Pure ν µ Pure ν µ Pure ν µ Pure ν µ Pure ν µ ν 2 2 ν 1 Pontecorvo, Time, t % L ( P i i = sin 2 2θ sin 2 ' 1.27Δm 2 * & E ) energy and baseline dependent osc frequency depends on Δm 2 amplitude depends on θ 24

25 Neutrino Energies Big-Bang neutrinos ~ ev Neutrinos from the Sun < 20 MeV Antineutrinos from nuclear reactors < 10.0 MeV Atmospheric neutrinos ~ GeV Neutrinos from accelerators up to GeV (10 9 ev) black holes, gamma ray bursters, supernova remnants, cosmic rays, WIMPs?? ev ev 25

Daya Bay Reactor Experiment Experimental

target mass: 20 ton per AD photosensors:

26 Daya Bay Reactor Experiment Experimental Halls Antineutrino Detector mineral oil Gd-doped liquid scintillator six 2.9 GWth reactors 6 detectors, Dec Jul days now running with 8 detectors liquid scintillator γ-catcher target mass: 20 ton per AD photosensors: PMTs energy resolution: (7.5 / E + 0.9)% 26

27 Karsten Heeger, Univ. of Wisconsin NUSS, July 13,

Antineutrino Candidates (Inverse Beta Decay) Prompt + Delayed Coincidence IBD candidates ν e + p e + + n prompt event: positron deposits energy and annihilates (~ns) delayed event: neutron

28 Antineutrino Candidates (Inverse Beta Decay) Prompt + Delayed Coincidence IBD candidates ν e + p e + + n prompt event: positron deposits energy and annihilates (~ns) delayed event: neutron thermalizes and captures on Gd Events/0.25 MeV Prompt Energy Signal Data, DYB-AD1 MC Events/0.05 MeV 3000 Delayed Energy Signal 2500 Data, DYB-AD MC Uncertainty in relative E d efficiency (0.12%) between detectors is largest systematic Prompt energy (MeV) Delayed energy (MeV) 28

29 Antineutrino Rate vs. Time IBD Rate (/day/ad) Daya Bay Near Hall Ling Ao Near Hall Far Hall Data No Oscillation Best Fit Dec Jan Feb Mar Apr May Jun Jul Run Time Detected rate strongly correlated with reactor flux expectations Predicted Rate assumes no oscillation Absolute normalization determined by fit to data Normalization within a few percent of expectations 29

30 Measurement of Neutrino Mixing at Daya Bay Observation of electron antineutrino disappearance over km-long baselines νe νe,x νe,x

31 Daya Bay Neutrino Oscillation Daya Bay demonstrates L/E oscillation Daya Bay Phys.Rev.Lett. 112 (2014) Neutrino oscillation is energy and baseline dependent % L ( P i i = sin 2 2θ sin 2 ' 1.27Δm 2 * & E ) Pi j 31

32 From Anomalies to Precision Oscillation Physics solar neutrino problem oscillation searches present precision measurements Ga Cl SK 32

Neutrino Mixing Mixing Angles # U e1 U e2 U e 3 & # 0.8 0.5 U e 3 & % ( U = U µ1 U µ2 U µ 3 % ( = % ( % 0.4 0.6 0.

7 ( ' U MNSP Matrix Maki, Nakagawa, Sakata, Pontecorvo # 1 0 0 & # cos) 13 0 e *i, CP % ( sin) & # 13 cos) 12 sin) 12 0& # 1 0 0 & =

33 Neutrino Mixing Mixing Angles # U e1 U e2 U e 3 & # U e 3 & % ( U = U µ1 U µ2 U µ 3 % ( = % ( % ( $ U "1 U " 2 U % " 3 ' $ ( ' U MNSP Matrix Maki, Nakagawa, Sakata, Pontecorvo # & # cos) 13 0 e *i, CP % ( sin) & # 13 cos) 12 sin) 12 0& # & = 0 cos) 23 sin) 23 % ( + % ( % ( % ( + *sin) 12 cos) 12 0 $ 0 *sin) 23 cos) % 23 ' *e i, CP $ sin) 13 0 cos) ( % ( + % 0 e i- / 2 ( 0 % i- / 2+i. ( 13 ' $ 0 0 1' $ 0 0 e ' atmospheric, K2K reactor and accelerator SNO, solar SK, KamLAND 0νββ 33

34 Open Questions in Neutrino Physics Neutrino mass and mixing Neutrino oscillation What is the absolute neutrino mass? Are neutrinos their own antiparticles? Are there more than 3 neutrinos? Is there CP violation? 34

35 Neutrino Mass and Particle Nature normal inverted quasi-degenerate Δm atm 2 m ν > ev What is the absolute mass scale? What is the mass hierarchy? Are neutrinos Majorana particles? Karsten Heeger, Univ. of Wisconsin Yale, March 27,

36 Project 8 - Neutrino Mass Measurement Electron energy spectrum near 18 kev endpoint should be distorted by the effective mass of ν e, squared. B = 1 T E = 18 kev f = 26 GHz P = 1 fw arxiv: D. M. Asner et al.,

37 Neutrinoless Double Beta Decay: 0νββ 2ν mode: conventional 2 nd order process in nuclear physics Γ 2ν = G 2ν M 2ν 2 G are phase space factors 0ν mode: hypothetical process only if M ν 0 AND ν = ν Γ 0ν = G 0ν M 0ν 2 m ββ 2 G 0ν ~ Q 5 0νββ would imply - lepton number non-conservation - Majorana nature of neutrinos Karsten Heeger, Univ. of Wisconsin Yale, March 27, νββ may allow us to determine - effective neutrino mass 37

38 Search for 0νββ in 130 Te cartoon of 2νββ and 0νββ spectra Experimental Signature of 0νββ - peak at the transition Q-value - enlarged by detector resolution - over unavoidable 2νββ background in 130 Te Cuoricino summed spectrum Q( 130 Te)=2527 kev energy = key event signature Karsten Heeger, Univ. of Wisconsin Yale, March 27,

1 mk) Single pulse example For E = 1 MeV: ΔT = E/C 0.1 mk Signal size: 1 mv voltage signal energy deposited Time constant: τ = C/G = 0.

39 TeO 2 Bolometers 5 cm 790g per crystal TeO 2 Bolometer: Source = Detector deposited energy Heat sink: Cu structure (8-10 mk) Thermal coupling: Teflon (G = 4 pw/mk) Thermometer: NTD Ge-thermistor (dr/dt 100 kω/µk) Absorber: TeO 2 crystal (C 2 nj/k 1 MeV / 0.1 mk) Single pulse example For E = 1 MeV: ΔT = E/C 0.1 mk Signal size: 1 mv voltage signal energy deposited Time constant: τ = C/G = 0.5 s Energy resolution: ~ 5 kev at 2.5 MeV Amplitude (a.u.) Karsten Heeger, Univ. of Wisconsin Yale, March 27, 2015 Time (ms) 39

40 CUORE at Gran Sasso, Italy 1.4-km avg. rock overburden = 3100 m.w.e. flat overburden factor 10 6 reduction in muon flux to ~ µ/(s cm 2 ) CUORE A Cuoricino 40

41 CUORE Detector and Cryostat Outermost shield DU Test Stand Ancient lead for shielding 988 detectors 206 kg of 130 Te The coldest cubic meter in the known Universe. 6mK stable base temperature. 41

42 CUORE Sensitivity CUORE sensitivity goal T1/2 0νββ > 9.5 x % C.L. Effective Majorana mass % C.L. Assumptions: 5 kev FWHM ROI resolution (δe), background rate (b) of 0.01 counts/(kev kg yr), 5 years of live time. [y] 1σ C.L. Sensitivity 0ν 1/2 T Cuoricino CUORE-0 - bkg: events/(kev kg y) CUORE - bkg: 0.01 events/(kev kg y) CUORE sensitivity goal T1/2 0νββ : 9.5 x yr (90% C.L.) [ev] m ββ Cuoricino exclusion 90% C.L. GERDA exclusion 90% C.L. KamLAND-Zen and EXO-200 exclusion 90% C.L. CUORE 90% C.L. sensitivity 2 m 23 <0 2 m 23 >0 76 Ge claim CUORICINO: y (90% C.L.) Live time [y] [ev] m lightest arxiv:

Neutrinos from Accelerators FNAL booster (8 GeV protons) target

dirt (~500 m) detector background Start with a beam of nearly

look for ν e appearance Short-baseline L/E ~ 1km/GeV search for

43 Neutrinos from Accelerators FNAL booster (8 GeV protons) target and horn (174 ka) K 0 K decay region (50 m) oscillations? dirt (~500 m) detector background Start with a beam of nearly pure muon neutrinos.look for ν e appearance Short-baseline L/E ~ 1km/GeV search for sterile neutrinos new physics? Long baseline L/E ~ 1000km/GeV mass hierarchy CP violation oscillation parameters 43

ν The particles produced tell you about the neutrino -> flavor -> energy

44 MicroBooNE Liquid Argon Time Projection Chamber Neutrino hits the argon and produces charged particles. ν The particles produced tell you about the neutrino -> flavor -> energy Electron neutrinos -> Electrons and others Muon neutrinos -> muons and others Other interactions that produce single photons 44

45 MicroBooNE Installation Once detector assembly was finished, Moved the detector to the detector hall summer

Deep Underground Neutrino Experiment (DUNE) Wide band beam 0.

5-10 GeV Baseline of 1300km from Fermilab to Homestake lots of matter to

46 Deep Underground Neutrino Experiment (DUNE) Wide band beam GeV new neutrino beam at Fermilab Observe oscillation spectrum GeV Baseline of 1300km from Fermilab to Homestake lots of matter to observe mass hierarchy effects! Determine mass hierarchy, measure CP violation at the same time starting in 2024? 46

47 What about dark matter? Neutrinos 0.3% Stars 0.5% Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

little with ordinary matter Stable and long-lived Leading Candidates: Axions - mass ~10-3 10-6 ev - Arises in the

48 What is Dark Matter? Observational evidence indicates: Non-baryonic Cold(ish) and massive (non-relativistic and exerts gravity) Interact little with ordinary matter Stable and long-lived Leading Candidates: Axions - mass ~ ev - Arises in the Peccei-Quinn solution to the strong- CP problem WIMPs: Weakly Interacting Massive Particles - mass of 1 GeV 10 TeV - weak scale cross sections results in observed abundance σ cm 2 <σ A v> cm 3 /s m χ 100 GeV 48

49 Detecting WIMPs annihilation χ χ production Indirect Detection Colliders Look for the missing energy Collect dark matter in Stars and Galaxies, then let them annihilate among themselves. q q Detect the decay particles Fermi/LAT scattering Direct Detection Let dark matter recoil off of nuclei Look for nuclear recoil X WIMP X nuclear recoil

50 Dark Matter Search in Ice (DM-Ice) 50m Modulation Search at South Pole DM-Ice-17 IceCube AMANDA (decommissioned) 1450m DeepCore DM-Ice17 17 kg of NaI(Tl) at 2450m depth in operation since 2011 Karsten Heeger, Yale University LNGS, April 15, bed 2450m 2820m

51 DM-Ice-17 Construction & Deployment Revive NAIAD xtals Detector assembly Shipment to Antarctica July 2010 Sep - Oct Dec. 1, 2010 Deployment Dec. 11, 2010 Detector in the hole 51

52 DM-Ice 17 Deployment - Hands-On 52 Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

ADMX-HF Experiment Axion Dark Matter experiment at High

standard model of electroweak interactions to explain the lack

ideal dark matter candidate due to its feeble interaction with

53 ADMX-HF Experiment Axion Dark Matter experiment at High Frequency (ADMX- HF) Axion is predicted in the context of the standard model of electroweak interactions to explain the lack of CP asymmetry in the strong force The axion (or axions) is an ideal dark matter candidate due to its feeble interaction with matter. Axions can be converted to photons by a strong magnetic field 53

Cosmological Simulations of Galaxy Cluster Formation N-body+Gasdynamics with Adaptive Refinement Tree (ART) code Box size ~ 80/h Mpc; Region shown ~ 2/h Mpc; Spatial resolution ~ a few kpc Modern

54 Cosmological Simulations of Galaxy Cluster Formation N-body+Gasdynamics with Adaptive Refinement Tree (ART) code Box size ~ 80/h Mpc; Region shown ~ 2/h Mpc; Spatial resolution ~ a few kpc Modern cosmological hydro simulations include the effects of baryons (i.e., gas cooling, star formation, heating by SNe/AGN, metal enrichment and transport). Simulations performed by the Yale BulldogM HPC cluster

Probing Dark Energy, Dark Matter and Neutrino with Galaxy Clusters X-ray Cluster Cosmology

1) sample of 49 clusters + 37 high-z clusters from the 400d X-ray selected cluster sample

Cluster Tension Planck 2015 Ω DE KEY: Robust Mass Proxy Yx (excluding cluster cores) σ 8 =0.

012 Possible Solutions: New Physics: sum of the neutrino masses is ~0.2eV!

55 Probing Dark Energy, Dark Matter and Neutrino with Galaxy Clusters X-ray Cluster Cosmology Vikhlinin et al Local (z<0.1) sample of 49 clusters + 37 high-z clusters from the 400d X-ray selected cluster sample Planck CMB vs. Cluster Tension Planck 2015 Ω DE KEY: Robust Mass Proxy Yx (excluding cluster cores) σ 8 =0.813(Ω M /0.25) ±0.013 w 0 =-0.991±0.045 Ω DE =0.740±0.012 Possible Solutions: New Physics: sum of the neutrino masses is ~0.2eV! Cluster mass calibration is biased by 45% Planck CMB results may be biased Galaxy Clusters provide powerful constraints on Dark Energy, Dark Matter, and Neutrino. But, exploiting the statistic power of future cluster surveys requires improved understanding of Cluster Astrophysics!!

56 Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

57 Every second there are billions of neutrinos going through this tiny spot! And we might be moving through a halo of dark matter particles. Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

58 The New Yale Wright Lab Experimental facilities for nuclear particle, and astrophysics Coming in 2016 Karsten Heeger May 27,

59 The New Yale Wright Lab Facilities for Research, Education and Teaching Research laboratories Instrument Design / Machine Shops Interaction Spaces / Communication / Education Karsten Heeger May 27,

60 95% of the Universe is unknown. Much opportunity for discovery! Explore it with us at Yale Physics! Thanks to Charlie Baltay, Daisuke Nagai, Bonnie Fleming, Reina Maruyama, Penny Slocum, Keith Baker, Steve Lamoreaux, Flavio Cavanna, Ornella Palamara Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009

Recent Discoveries in Neutrino Physics

Recent Discoveries in Neutrino Physics Experiments with Reactor Antineutrinos Karsten Heeger http://neutrino.physics.wisc.edu/ Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009 Standard Model and