New Physics Probes in Future Neutrino Experiments

Abstract

Neutrino physics is a broad and diverse ﬁeld, both experimentally and theoretically. As the standard oscillation picture begins to settle we are moving into an era where precise tests of the neutrino picture can be made. In this talk I will discuss the present and future status of many theoretical probes and a broad range of experiments spanning twenty orders of magnitude in neutrino energy. In particular, I will highlight the strongly interconnected nature of new physics studies in the neutrino sector.

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 0/47 New Physics Probes in Future Neutrino Experiments

Peter B. Denton

Brookhaven Colloquium

October 29, 2019 1907.08311 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 2/47 Why Neutrinos Are Awesome

1. 7+ new parameters I Oscillations 6 → I Mass scale 1+ → 2. Mass generation mechanism 3. Nature of neutrinos 4. Poorly measured great place to look for new physics ⇒ 5. Resolve anomalies 6. Role of neutrinos in the early universe 7. Extreme particle physics production 8. High degree of interconnectivity

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 3/47 Experiments Physics ↔ Mass Scale

Reactor

Astrophysical

Atmospheric

Collider

Denton Accelerator

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 4/47 Experiments Physics ↔ Mass Scale 0νββ End Point LEGEND KATRIN SuperNEMO Project-8 NEXT HOLMES nEXO ECHo Darwin CUORE CUPID Cosmology SNO+ KamLAND-Zen Reactor PLANCK PandaX SBL LBL GERDA CνB CMBS4 LSS PROSPECT KamLand PTOLEMY STEREO SDSS JUNO Astrophysical NEOS DESI DANSS Euclid Neutrino-4 LSST Radio WFIR H20 MBL ANITA ARCA Daya Bay GRAND Baikal Reno POEMMA KM3NeT Double Chooz RNO CONUS IceCube MINER DeepCore SuperK CONNIE CEvNS ORCA Atmospheric HyperK INO

DUNE Collider COHERENT LBL LHC+ FASERnu SBL SHiP MATHUSLA MiniBooNE MicroBooNE NOvA SBN T2K T2HK(K) ESSnuSB

Denton Accelerator

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 4/47 Experiments Physics ↔ Mass Scale Extreme 0νββ End Environments Point LEGEND KATRIN SuperNEMO Project-8 NEXT HOLMES nEXO ECHo Darwin CUORE CUPID Cosmology SNO+ KamLAND-Zen NSI Reactor PLANCK PandaX SBL LBL GERDA CνB CMBS4 LSS PROSPECT KamLand PTOLEMY STEREO SDSS JUNO Astrophysical NEOS DESI DANSS Euclid Neutrino-4 LSST Radio WFIR H20 MBL Sterile ANITA ARCA Daya Bay GRAND Baikal Reno POEMMA KM3NeT Double Chooz RNO CONUS IceCube MINER DeepCore SuperK CONNIE CEvNS ORCA Atmospheric HyperK INO

DUNE Collider COHERENT LBL Mixing LHC+ FASERnu SBL Mass SHiP νBSM MATHUSLA MiniBooNE MicroBooNE NOvA SBN T2K T2HK(K) ESSnuSB

Denton Accelerator

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 4/47 Experiments Physics ↔ Mass Scale Extreme 0νββ End Environments Point LEGEND High Low KATRIN SuperNEMO Energy Project-8 NEXT Energy HOLMES nEXO Galactic SN Cosmogenic ECHo Darwin DSNB Blazar CUORE CνB AGN CUPID GRB Cosmology SNO+ TDE KamLAND-Zen SNR NSI NC Reactor PLANCK PandaX Pulsar CC SBL LBL GERDA CνB CMBS4 LSS PROSPECT μ->eγ SPVAT KamLand PTOLEMY STEREO SDSS μ->eee JUNO Astrophysical NEOS DESI ν scattering DANSS Euclid Mediator Neutrino-4 LSST Radio WFIR H20

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 4/47 Mass Generation Dirac

`¯ Y HE `¯ Y HN˜ + h.c. L ⊃ − L ` R − L ν R −6 Impose B L yν /ye 10 − ∼ Seesaw

1 v2 T v2 1 v2 T Mν: Yν Y λ∆Y∆ YΣ Y − 2 MR ν M∆ − 2 MΣ Σ

H. Fritzsch, M. Gell-Mann, P. Minkowski PLB 1975 Inverse P. Minkowski PLB 1977 1 1 M M µ M T W. Konetschny, W. Kummer PLB 1977 ν : D T D MS MS D. Wyler, L. Wolfenstein NPB 1983 R. Foot, H. Lew, X. He, G. Joshi ZPC 1989 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 5/47 Discovery of Oscillations

Super-KamiokaNDE SNO 2 3 2 2 5 2 P (νµ νµ) ∆m 10− eV P (ν ν ) ∆m 10 eV → ∼ e → e ∼ −

SK hep-ex/9807003 SNO nucl-ex/0204008

Oscillations v < c ⇒ ν Three distinct masses

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 6/47 Oscillation Physics

To get oscillations, need to produce neutrinos in a diﬀerent basis than how they propagate       νe Ue1 Ue2 Ue3 ν1 νµ = Uµ1 Uµ2 Uµ3 ν2 ντ Uτ1 Uτ2 Uτ3 ν3

Lots of parameters 18 Unitarity 9 Charged lepton rephasing 6 Neutral lepton rephasing 4

θ12, θ13, θ23, δ

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 7/47 Oscillations Pedagogy

Standard parameterization of lepton mixing matrix:

   iδ   1 c13 s13e− c12 s12 U =  c23 s23  1   s12 c12  − s c s eiδ c 1 − 23 23 − 13 13 Many other unitary matrices, all valid H. Fritzsch, Z-z. Xing hep-ph/0103242

CP violation governed by the Jarlskog

2 J = s12c12s13c13s23c23 sin δ

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 8/47 Neutrino Masses Oscillations →

1. Neutrinos propagate in mass eigenstates 2. Each mass state accumulates a phase

2 mi φi = 2E x 3. Interference cares about phase diﬀerences, sensitive to m2 m2 ∆m2 i − j ≡ ij

4. Oscillations insensitive to absolute mass scale

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 9/47 Experiment to Oscillation Parameters

2 2 Six oscillation parameters: θ12, θ13, θ23, δ, ∆m21, ∆m31

2 I Atmospheric νµ disappearance sin 2θ23, ∆m → | 31| SuperK, IMB, IceCube 2 I Solar νe disappearance cos 2θ12, ∆m → ± ± 21 SNO, Borexino, SuperK

I Reactor νe disappearance: 2 I LBL sin 2θ12 and ∆m → | 21| KamLand I Future LBL ∆m2 → ± 31 JUNO 2 I MBL θ13, ∆m → | 31| Daya Bay, RENO, Double Chooz 2 I Accelerator LBL νe appearance: ∆m , cos 2θ23, θ13, δ ± 31 ± T2K, NOvA, T2HK, DUNE

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 10/47 0.04 Denton 2 0 s13 0.8 2 0.2 s23 0.45 2 0.15 s12 10 2 5 2 ∆m21/10− 4 2 3 ∆m /10− 1 | 31| 2 1σ 1 bf 2σ 0 δ/π 3σ 1998 2000 2005 2010 2015 2018 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 11/47 Are Neutrinos Normal or Not? Normal Ordering Inverted Ordering

νe νµ ντ νe νµ ντ

ν3 ν2

ν1

ν2

ν1 ν3

2 m3? sin θ23?

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 12/47 Most Generic Three Flavor Consistency Check

Normalisations 9 3σ Rows α =e 9 α =µ U U U α =τ | e1| | e2| | e3| w/o Unitarity (All data) 6 Columns 6 with Unitarity i =1 2 (All data) 2 i =2 χ χ i =3 ∆ ∆ 2σ 3 w/o Unitarity (No normalisation 3 or sterile data) µ e 0 9 1σ Uµ1 Uµ2 Uµ3 0 | | | | | | -1 10-2 10 0.5 6 2 2 2 2 2 2 1 ( U 1 + U 2 + U 3 ) or 1 ( U + U + U ) 2 − | α | | α | | α | − | ei| | µi| | τi| χ Rows Columns ∆ 3 Unitarity Triangle Closures 9 3σ Rows α,β =e,µ 0 α,β =e,τ 9 α,β =µ,τ Uτ1 Uτ2 Uτ3 | | | | | | 6 Columns i,j =1,2 6

2 i,j =1,3 2 χ =2 3

χ i,j , ∆ 2σ ∆

3 3 eµ

0 0 0.2 0.4 0.6 0.8 1 0 0.2 0.4 0.6 0.8 1 0 0.2 0.4 0.6 0.8 1 1σ

Uα1 Uα2 Uα3 0 -1 | | | | | | 10-2 10 0.5

U U ∗ +U U ∗ +U U ∗ or U U ∗ +U U ∗ +U U ∗ | α1 β1 α2 β2 α3 β3 | | ei ej µi µj τi τj | Rows Columns S. Parke, M. Ross-Lonergan 1508.05095

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 13/47 Long Baseline Oscillations: Present

295 km 810 km

G. Feldman 1901.09431 NOvA FNAL Users Meeting ’19

Mass ordering separation N Ls2 ∝ e 23 Matter eﬀect mass ordering ⇒ L. Wolfenstein PRD 1978

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 14/47 Long Baseline Oscillations: Future DUNE T2HK

MO 3 σ ∼ ∆θ 1 23 ∼ ◦ T2HK 1412.4673

Second maximum ESSnuSB 1611.06118 T2HKK 1309.7022 ∆θ 1 DUNE 1807.10334 Peter B. Denton (BNL)23 ∼ ◦ Brookhaven Colloquium: October 29, 2019 15/47 Long Baseline Oscillations: Cross Sections

M. Betancourt, et al. 1805.07378

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 16/47 JUNO: Mass Ordering

1. 53 km baseline p 2. Targeting 3%/ E/MeV resolution 3. Expected to open in 2021

JUNO 1507.05613 ND is necessary F. Capozzi, E. Lisi, A. Marrone 1508.01392 H. Wang, et al. 1602.04442 D. Forero, R. Hawkins, P. Huber 1710.07378 ND isn’t necessary D. Danielson, A. Hayes, G. Garvey 1808.03276

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 17/47 DUNE: Beyond LBL Oscillations

Solar

F. Capozzi, et al. 1808.08232 May be possible to measure: ∆m2 , θ , δ, θ , ∆m2 , and θ ! ± 31 23 13 21 12 Atmospheric K. Kelly, et al. 1904.02751 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 18/47 Supernova Neutrinos

Galactic SN Mass Ordering → K. Scholberg 1707.06384 Diﬀuse Supernova Neutrino Background can constraint RSN and fBH NO IO 0.6 HK (Gd) 0.5 HK (Gd)+JUNO HK (Gd)+JUNO+DUNE 0.4 SN − 0.3 BH ¯ f ∆ 0.2

0.1

0.0 0.0 0.1 0.2 0.3 0.4 0.5 0.0 0.1 0.2 0.3 0.4 0.5 f¯BH SN f¯BH SN − − K. Møller, A. Suliga, I. Tamborra, PBD 1804.03157

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 19/47 Neutrino Mass Scale

p 2 Endpoint: me < 1.1 eV 0νββ: mββ . 0.65 eV

KATRIN 1909.06048 2 P 2 2 m = Uei m e | | i

P APPEC 1910.04688 Cosmology: mi < 0.12 eV P 2 mββ = U mi Planck 1807.06209 | ei | Considerable nuclear uncertainties

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 20/47 Neutrinoless Double Beta Decay: Prospects

M. Agostini, G. Benato, J. Detwiler 1705.02996

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 21/47 Sterile Neutrinos: Where are they Hiding? 1 HL LHC − s y a c

2 e 10− D VLHC n o s e

NA62 M

V LHeC N 10 4 L − KATRIN ILC FASER CLIC CMB 2 | 6 AL3X N 10− e V | L TRISTAN H C 8 b 10− ATLAS M A T H U CMS 10 S 10− L DUNE SHiP A ATHENA FCC ee CMB +BAO +H0 − 12 BBN Seesaw 10− 9 6 3 3 10− 10− 10− 1 10

mN [GeV] F. Deppisch CERN Neutrino Platform ’19 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 22/47 Sterile Neutrinos: the eV puzzle Experimental evidence for m 1 eV: 4 ∼ I LSND + MiniBooNE: 3.8 σ + 4.7 σ LSND hep-ex/0104049 MiniBooNE 1805.12028 I Reactor Antineutrino Anomaly: 3 σ G. Mention, et al. 1101.2755 Daya Bay 1704.01082 A. Hayes, E. McCutchan, A. Sonzogni, et al. 1707.07728 I Gallium anomaly: 3 σ C. Giunti, M. Laveder 1006.3244 2.3 σ: J. Kostensalo, J. Suhonen, C. Giunti, P. Srivastava 1906.10980 I NEOS, DANSS, Neutrino-4: 3 σ, 2.8 σ, 2.8 σ ∼ NEOS Neutrino, ’18 DANSS Neutrino, ’18 Neutrino-4 1809.10561

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 23/47 Sterile Neutrinos: eV Constraints Experimental constraints from: I IceCube 1605.01990 I MINOS/MINOS+ 1710.06488 I Super-K 1410.2008 I KARMEN hep-ex/0203021 I CDHS PLB 134, 281 (1984) I Daya Bay, MINOS, Bugey-3 1607.01177 I OPERA 1303.3953 I ICARUS 1209.0122 I NOvA 1706.04592 I PROSPECT 1806.02784 . . 3 + N doesn’t help J. Kopp, et al. 1303.3011 Cosmology needs to be accommodated Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 24/47 LSND, MiniBooNE Alternatives CPT violation H. Murayama, T. Yanagida hep-ph/0010178 G. Barenboim, L. Borissov, J. Lykken hep-ph/0212116 Dark Energy D. Kaplan, A. Nelson, N. Weiner hep-ph/0401099 Extra dimensions H. Pas, S. Pakvasa, T. Weiler hep-ph/0504096 Many non-sterile BSM explanations ruled out J. Jordan, et al. 1810.07185 Upscatter to unstable νs which promptly decays

C. Arg¨uelles,M. Hostert, Y. Tsai 1812.08768 E. Bertuzzo, et al. 1807.09877

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 25/47 Short Baseline Neutrino Program

1. Leverage LAr to discriminate photons from electrons µB 1910.02166 2. L is easier to measure than E

P. Machado, O. Palamara, D. Schmitz 1903.04608 3. Test bed for LAr technology

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 26/47 Sterile Neutrinos: keV range

I m4 1 keV DM & ⇒ S. Dodelson, L. Widrow, hep-ph/9303287 I 7 keV sterile from X-ray line E. Bulbul, et al. 1402.2301

102 Ω Diﬀuse X-ray Background h 2 Ω = 0 h 2 Ω = 0 .005 h 2 = 0 .025 ν Fermi GBM µ , ν .11 τ → ν s supernovaNuSTAR bound (this work)

L 10 = 0 M31 Unresolved CXB

. Milky Way 1 Bulbul et al. L = 0

. 003 [keV] s m

1 L 100-300 pc Fornax Core = 0 Preferred Region

Tremaine-Gunn Bound 1 10− 13 11 9 7 10− 10− 10− 10− sin2(2θ)

C. Arg¨uelles,V. Brdar, J. Kopp 1605.00654 A. Suliga, I. Tamborra, M. Wu 1908.11382 C. Dessert, N. Rodd, B. Safdi 1812.06976

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 27/47 Heavy Neutral Lepton Searches

Above mZ , new neutrino states could be νR or νL HNL not “sterile” ⇒

Physics Beyond Colliders group 1901.09966

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 28/47 Neutrinos at the LHC with FASER

1 1 1 energy ranges of

0.9 0.9 accelerator data 0.9 oscillated ντ measurements /GeV) /GeV) 2 0.8 2 0.8 0.8 IceCube ντ, ντ

cm ν cm µ SK ντ, ντ •38 0.7 •38 0.7 0.7

10 OPERA ντ 10 × E53 ν

e × ( ν

0.6 ( 0.6 IceCube ( 0.6 ν /E

ν DONUT ν , ν /E

e e /GeV) ν σ

0.5 0.5 2 0.5 σ νµ DONUT ν , ν ν cm τ τ 0.4 E53 ν 0.4 µ 0.4 e , •38 FASERν ν FASERν µ mixed) 10 0.3 νe spectrum (a.u.) 0.3 FASERν × 0.3 ν spectrum (a.u.) ( τ νµ spectrum (a.u.) ν 0.2 0.2 /E 0.2 ν σ 0.1 0.1 0.1

0 0 3 5 6 0 102 103 104 102 10 104 10 10 102 103 104

Eν (GeV) Eν (GeV) Eν (GeV)

FASER, PBD 1908.02310

I Cross sections Eν 1 TeV I Prompt neutrino production ∼ I ντ measurements I CC NSI 2 3 2 2 I Sterile ∆m 10 eV I sin θW ∼ Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 29/47 Neutrino Non-Standard Interactions

Generalized framework connects oscillations to scattering X = 2√2G f,P (¯ν γµP ν )(fγ¯ P f) LNC,NSI − F αβ α L β µ f,P,α,β

P PL,PR , f e, u, d , NC & CC, SPVAT ∈ { } ∈ { } L. Wolfenstein PRD 1978 M. Lindner, W. Rodejohann, X-J. Xu 1612.04150

135 parameters!     0 1 + ee eµ eτ 1 2 H = U  ∆m21  U †+√2GF Ne  eµ∗ µµ µτ  2E 2 ∆m31 eτ∗ µτ ττ B. Dev, PBD, et al. 1907.00991

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 30/47 NSIs: Oscillation - Scattering Synergy Oscillations Scattering p 2 Mediator mass Nearly any MZ0 & Q LMA-Dark Degeneracies Direct probe Diagonal ντ sector Can probe Need ντ ’s

CHARM

u d ǫee ǫee COHERENT

u d NuTeV ǫµµ ǫµµ

u d ǫττ ǫττ

Oscillation LMA-Dark: P. Coloma, T. Schwetz 1604.05772 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 31/47 Neutrino Non-Standard Interactions: Scattering

T. Han, et al. 1910.03272

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 32/47 NSI Global Fit: Oscillations

ee µµ ee µµ − − Solar

ττ µµ Atmospheric −

eµ LBL

Oscillations eτ LBL 90% CL u θ >45 d 12 < ◦ µτ Atmospheric 1.0 0.5 0.0 0.5 − − q,V αβ Oscillations are independent of mZ0 . P. Coloma, PBD, et al. 1701.04828

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 33/47 Heavy NSI Global Fit: CHARM & NuTeV ee ee

µµ

ττ

eµ

Osc + CHARM + NuTeV eτ 90% CL u θ >45 d 12 < ◦ µτ

1.0 0.5 0.0 0.5 − − q,V αβ Heavy m 0 1 GeV. P. Coloma, PBD, et al. 1701.04828 ⇒ Z & Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 34/47 NSI Constraints: COHERENT

ee ee

µµ µµ

ττ ττ (w/osc)

eµ

COHERENT eτ 90% CL u d > = θ12 45◦ < µτ

1.0 0.5 0.0 0.5 − − q,V αβ Valid down to mZ0 & 10 MeV PBD, Y. Farzan, I. Shoemaker, 1804.03660 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 35/47 Looking to the COHERENT Future Interference of diﬀerent materials is powerful

0.15

0.10 2 q,V 1 Yn (1 4 sin θW ) 0.05 ee,deg = − − 3 Yn + 1 Y [1, 1.43] n ∈ q,V eτ 0.00 q,V [0.15, 0.18] ee,deg ∈

0.05 Y = N /N − n n p

0.10 100 kg yrs Xe with Etr = 10 keV − · 100 kg yrs Ne with Etr = 10 keV · Denton 10% systematic Solar upturn? 0.15 − 0.05 0.00 0.05 0.10 0.15 0.20 − q,V ee Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 36/47 Ultra-light Neutrino Non-Standard Interactions

E.g. L L or L L symmetries e − µ e − τ

M. Bustamante, S. Agarwalla 1808.02042

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 37/47 Neutrino Non-Standard Self Interactions

NSI NSSI CMB Inﬂation H0 IceCube ν4 K-decay →100 → → 105 → → → → Z width NO m1 CMB 4 10 m2 m m φ = 5 MeV 3 interacting mode 1 3 CMB 10− self − 10 IceCube

eﬀ TCνB N

[TeV] 2 g 10 res CMB ΛCDM mode ν,

2 E 1 10− 10 m φ = 0 .2 MeV 100

3 1 10− 1 0 1 10− 4 3 2 1 0 10− 10 10 10− 10− 10− 10− 10 mφ [MeV] mlightest [eV]

G. Barenboim, PBD, I. Oldengott 1903.02036 C. Kreisch, F-Y. Cyr-Racine, O. Dor´e 1902.00534 N. Blinov, et al. 1905.02727 Supernova:

A. Das, A. Dighe, M. Sen 1705.00468

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 38/47 A Neutrino Decay Example We want to explain IceCube anomaly in ﬂavor and energy

νe νµ ντ

ν3

Model recipe: 1. ν-decay depletes ν’s at low energy

2. Want fewer νµ at low energy Mr. Stark, 3. Let ν and ν decay I don’t feelsogood... 2 3 4. Keep ν1 stable

Preferred over SM > 3 σ ν2

ν1 PBD, I. Tamborra 1805.05950

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 39/47 Invisible ν Decay Constraints and Evidence

IceCube (ν2, ν3) Tracks & Cascades Atm + LBL (ν3) Solar (ν2) IceCube (νi) SN1987A (¯νe) CMB (νi)

12 8 4 0 4 8 12 10− 10− 10− 10 10 10 10 τ/m [s/eV]

The νµ spectrum is diﬀerent than PBD, I. Tamborra, 1805.05950 the νe, ντ at IceCube S. Hannestad, G. Raﬀelt, hep-ph/0509278 IC 1607.08006 Kamiokande-II, PRL 58 1490 (1987) IC PoS ICRC2015 (2016) 1109 G. Pagliaroli, et al., 1506.02624 J. Berryman, A. de Gouvea, D. Hernandez, 1411.0308 M. Gonzalez-Garcia and M. Maltoni, 0802.3699 ν2, ν3-decay explains this, > 3 σ

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 40/47 The Tau Neutrino: Status

The tau neutrino is the poorest measured particle

Lepton universality? Γ(B D(∗)τν¯) (g 2) , → − µ Γ(B D(∗)`ν¯) → Some indirect detections: Analysis , NC+CC BestFit 68%, 90%

Analysis , NC+CC BestFit 68%, 90%

Analysis , CC BestFit 68%, 90%

16 direct detections Analysis , CC ∼ BestFit 68%, 90% SuperK 2017, CC 68% DONuT 0711.0728 arXiv:1711.09436 OPERA 2018, CC 68% arXiv:1804.04912 OPERA 1804.04912 0.0 0.5 1.0 1.5 2.0 Normalization

IC 1901.05366 SK 1711.09436

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 41/47 The Tau Neutrino: Terrestrial Prospects DUNE FASERν

ντ +ν τ

0.8 FASERν / GeV ]

2 0.6 cm - 38 M. Masud, M. Bishai, P. Mehta 1704.08650 0.4 [ 10 / E ν σ 0.2 DONUT

102 103 104 E[GeV]

FASER, PBD, et al. 1908.02310

A. de Gouvˆea,et al. 1904.07265

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 42/47 The Tau Neutrino: Astrophysical Prospects

IceCube double bang/pulse signature: Two candidates IC 1909.05162

ANITA, GRAND, POEMMA, RNO,

] νe : νµ : ντ = 1:1:1 GRAND, PBD, et al. 1810.09994 1 −

sr 7 IceCube (2015)

1 10− −

POEMMA 1708.07599 s GRAND10k (3 yr) 2 POEMMA (3 yr) − IceCube (2018) ARIANNA (3 yr) 8 10− ARA-37 (3 yr) [GeV cm ) ν ∨ ∨ E

( Cosmogenic ν ν 9 ∨

Φ Pessimistic 10− GRAND200k (3 yr) 2 ν Standard E ) ¯ ν GRAND200k integrated (3 yr) + ν ( 10 10− GRAND200k integrated (10 yr) All-ﬂavor 11 10− 105 106 107 108 109 1010 1011 Neutrino energy Eν [GeV] Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 43/47 The ANITA Anomaly Two upcoming showers E 1 EeV, θ 30 sh ∼ ∼ ◦ ANITA 1603.05218 ANITA 1803.05088 Problems: 1. Absorption > 106 more Earth-skimming events ⇒ 2. IceCube and Auger have comparable larger sensitivity → A. Romero-Wolf, et al. 1811.07261 BSM solutions: I Sterile neutrinos J. Cherry, I. Shoemaker 1802.01611 I DM in Earth L. Anchordoqui, et al. 1803.11554 I Axions I. Esteban, et al. 1905.10372 I Long-lived state E. Dudas, et al. 1805.07342 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 44/47 Didn’t Discuss CνB Radioactive sources Unitarity violation LIV, CPT violation Large extra dimensions ν - DM connections DM searches at neutrino experiments Neutrino searches at DM experiments

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 45/47 Key Points

I Oscillation parameters becoming measured

I Strong BSM constraints will follow

I Mass scale probable

I Experiments in dark hallways

I Investigate experimental/theoretical combinations

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 46/47 Thanks and happy Halloween!

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 47/47 Backups

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 48/47 References

SK hep-ex/9807003 M. Gonzalez-Garcia, et al. hep-ph/0009350 0.04 Denton 2 M. Maltoni, et al. hep-ph/0207227 0 s13 0.8 2 SK hep-ex/0501064 0.2 s23 0.45 SK hep-ex/0604011 2 0.15 s12 10 T. Schwetz, M. Tortola, J. Valle 0808.2016 2 5 2 ∆m21/10− 4 M. Gonzalez-Garcia, M. Maltoni, J. Salvado 1001.4524 2 3 ∆m /10− 1 | 31| 2 1σ T2K 1106.2822 1 bf 2σ 0 δ/π 3σ D. Forero, M. Tortola, J. Valle 1205.4018 1998 2000 2005 2010 2015 2018 D. Forero, M. Tortola, J. Valle 1405.7540 P. de Salas, et al. 1708.01186

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 49/47 Sterile Neutrinos: Where are they Hiding? 1 PROSPECT SK +IC +DC NA3 144 144 64 Ce Pr I 187 Cu H CMS Re − E s P 2 45 Rovno y Ca a Belle

10 c − −

3 e H J I D NEOS N 20 n R 35 F o EWPD S s e L3 4 63 Ni Bugey M 10− V DELPHI

P N

S L 1 9 ATLAS Borexino 1 BESIII CMB 2 | 6 N 10− e V

| PIENU CHARM

8 NA62 10−

Supernovae T2K 10 BBN 10−

X ray CMB +BAO +H0 Seesaw 12 − 10− 9 6 3 3 10− 10− 10− 1 10

mN [GeV] F. Deppisch CERN Neutrino Platform ’19 Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 50/47 Supernova Neutrinos

0.5 ] 1

− 0.4 yr 3 − 0.3 Mpc 4 − 0.2 (0) [10

SN HK (Gd) ¯ R 0.1

∆ HK (Gd)+JUNO HK (Gd)+JUNO+DUNE 0.0 0.8 1.0 1.2 1.4 1.6 0.8 1.0 1.2 1.4 1.6 4 3 1 4 3 1 R¯SN(0) [10− Mpc− yr− ] R¯SN(0) [10− Mpc− yr− ]

K. Møller, A. Suliga, I. Tamborra, PBD 1804.03157

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 51/47 NSI Global Fit

Solar Chlorine, Gallex/GNO, SAGE, Super-K, Borexino, and SNO. Atmospheric Super-K, MINOS, and T2K. Reactor CHOOZ, Palo Verde, Double CHOOZ, Daya Bay, and RENO. Short baseline Bugey, ROVNO, Krasnoyarsk, ILL, G¨osgen,and SRP. Global ﬁt to oscillation data P. Coloma, PBD, et al. 1701.04828

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 52/47 Solar Parameters with DUNE and JUNO

F. Capozzi, et al. 1808.08232

Peter B. Denton (BNL) Brookhaven Colloquium: October 29, 2019 53/47 GRAND Cosmic Ray Parameter Estimation

GRAND can constrain the redshift evolution of the UHECR sources m, and the the nuclear composition of the UHECRs αS 1

0.8

0.6

0.4

0.2

0 -3 -2 -1 0 1 2 3 4

K. Møller, PBD, I. Tamborra 1809.04866

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