Poster Prize Competition: Wednesday Finals 2’40” Each Presentations Ordered Along the Poster Wall No

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Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Prospects for Exploring New Physics in Coherent Elastic Neutrino-Nucleus Scattering Joseph JOHNSTON (MIT) 23 Experiments Study for g-mode oscillations in the Sun using solar neutrino with Super- Yuuki NAKANO (Kamioka Observatory, ICRR, 35 Kamiokande University of Tokyo) Search for heavy neutrinos with the near detector ND280 of the T2K experiment Mathieu LAMOUREUX (DPhP, IRFU, CEA) 43

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

XMASS project

 A multi-purpose experiment using liquid xenon at the Kamioka Observatory in Japan  Direct detection of dark matter  Observation of low energy solar neutrinos (pp/7Be)  Search for neutrino-less double beta decay 80cm

 XMASS-I detector

 832 kg of liquid xenon 11m  Low energy threshold, low background, large mass  Sensitive to e/g events as well as nuclear recoil events  Stably taking data for more than 4 years 10m XMASS has challenged a variety of topics in neutrino physics Poster Wall #1 Neutrino physics with the XMASS liquid xenon detector K. Hiraide (ICRR, the University of Tokyo) for the XMASS Collaboration

Two-neutrino double electron capture (ECEC) Supernova (SN) neutrinos and GW follow-up n  Analogue to double beta decay X-ray  Coherent elastic n-nucleus scattering (CEvNS)  2n mode: allowed but observed  Neutral current  sensitive to all n flavors 78 130 only for Kr and Ba Xe  Large cross section  0n mode: Majorana if observed …  Recoil energy ~O(10 keV) n  A n  A

 Signature of 124Xe 2n ECEC n X-ray  New way to detect galactic SN neutrinos 124 - 124 4  Xe+2e  Te+2ne  Expect 3~21 evts (10 kpc), O(10 ) evts (196pc)  A peak at 63.6 keV by X-rays/Auger electrons  Gravitational-wave (GW) follow-up  Results  Searched for Preliminary  Improved analysis event bursts w/ particle ID associated with This work  No significant GW events Super-K n anti-n signal observed.  Upper limits on m,t m,t 22 Super-K n  T1/2>2.1x10 yrs n fluence e (90% CL) from GW170817 n (NS-NS merger) Super-K anti- e Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

CEvNS is a Standard Model process: Current and planned CEvNS Projects: Neutrino Magnetic Moment: • MINER: 10 kg Si+Ge at a 1 MW, Adds a term to CEvNS 푑휎 퐺 퐹 2 2 200 eV threshold 푚푎푔. 2 2 2 = 푄푊 퐸 (1 + 푐표푠휃) 푑휎휐−푁 휋훼 휇휈푍 1 1 퐸푅 2 푑(푐표푠휃) 8휋 = 2 − + 2 퐹 (퐸푅) • NUCLEUS: Several grams CaWO4 + 푑(퐸푅) 푚푒 퐸푅 퐸휈 4퐸휈 Al2O3, 10 eV energy threshold 2 푄푊 = 푍 4 푠푖푛 휃푊 − 1 + N • Ricochet: Several kg of Zn, Ge, Si, or Os, 50 eV threshold

• Bolometers at a reactor probe lower energies • Consider a bolometer at the 8.5 GW Chooz reactor complex, placed at the 400m near site or 80 m very near site Neutrino Coupling to Quarks Massive Scalar Mediator: Massive Vector Mediator: General Non-Standard Interactions:

Adds a term to CEvNS Interferes with CEvNS 2 1 푢푉 푑푉 1 2 푢푉 푑푉 푄푊 = ቎4푁 − + 휖푒푒 + 2휖푒푒 +푍 − 2푠푖푛 휃푊 + 2휖푒푒 + 휖푒푒 ቉ . 2 2 2 2 2 푑휎휙 푔휈 푄휙 퐸 푚 2 푄 = 푅 푁 퐹2(퐸 ) 푄 → 푄 = 푄 − 푍′ 2 2 2 2 푅 푊 푆푀+푁푃 푊 2 2 2 푑(퐸푅) 4휋 퐸휈 (푞 +푚휙) 퐺퐹 푞 + 푚푍′ 푢푉 푑푉 푢푉 푑푉 +4 푁 휖푒휏 + 2휖푒휏 + 푍 2휖푒휏 + 휖푒휏 푄휙 = (15.1 푍 + 14 푁)푔푞

푢푉 푑푉 • Breaking the 휖훼훽 푎푛푑 휖훼훽degeneracy is important for determining the mass hierarchy with DUNE (P. Coloma and T. Schwetz, Phys. Rev. D 95, 079903 (2017)) • Probing low energies places strong bounds at light mediator masses below ~ 10 MeV • Combining multiple targets places strong NSI bounds Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

Search for neutrinos from dark matter annihilation in the Earth core with the Super- Katarzyna FRANKIEWICZ 134 Kamiokande detector (National Center for Research) Predictions for Right-Handed Neutrinos From the Littlest Seesaw and Leptogenesis Susana MOLINA SEDGWICK 149 (University of Southampton) Blazars as neutrinos factories Chiara RIGHI 201 (Università degli studi dell'Insubria) p. 1 Study for g-mode oscillations in the Sun using solar neutrino with Super-Kamiokande @Neutrino 2018, 6th June 2018. Yuuki Nakano (Kamioka observatory, ICRR, Univ. of Tokyo) for the Super-Kamiokande collaboration ■Introduction and motivation - There are several periodic variations in the Sun. (1) 11-years periodic change of sunspot at the surface. (2) Solar oscillations around its equilibrium due to restoring force.

Oscillation Restoring force Region Frequency p-mode Pressure Surface convection A few mHz (~ 5 minutes) g-mode Gravity Core 100-300 μHz (Never detected) (Buoyancy) (a few hours) - These variations may affect the solar neutrino production. → Search for periodic variation using solar neutrino in Super-Kamiokande. p. 2 ■8B neutrino production and g-mode oscillation - Production rate of 8B ν is depends on temperature. Astrophys. J. 765, 14 (2013) Produced → T24-25 (Tcore~106-7 K) at the core of the Sun. at the core - Due to g-mode, temperature (electron density) may fluctuate at the core of the Sun. → Flux of 8B ν may be amplified by a factor of 170. Astrophys. J. Lett. 792, L53 (2014) ■Method to search for g-mode oscillation - Super-Kamiokande has accumulated ~100k neutrino events so far. - There are two methods to search for g-mode oscillations in Super-K.

- For more detail: come to my poster. I’m happy to discuss this study with you. Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

Search for neutrinos from dark matter annihilation in the Earth core with the Super- Katarzyna FRANKIEWICZ 134 Kamiokande detector (National Center for Research) Predictions for Right-Handed Neutrinos From the Littlest Seesaw and Leptogenesis Susana MOLINA SEDGWICK 149 (University of Southampton) Blazars as neutrinos factories Chiara RIGHI 201 (Università degli studi dell'Insubria) Search for heavy neutrinos with the T2K experiment Poster # 43, Wednesday session Presenter: M. Lamoureux How to detect heavy neutrinos? How to explain neutrino masses • NI couple to W and Z with a strength (and consequently oscillations)? 2 2 mν UαI ≡ |ΘαI | ∼ O A natural extension is one with 3 new MN right-handed neutrinos (sterile): H NI 0 mD ! c 1 c ν W − ν ν L θαI L R T ν να 2 mD mR R | {z } M ℓα light neutrinos • Can be produced e.g. in colliders or in 2 mD meson decays (arXiv:1502.00477). heavy neutrinos mν ∼ 0.1 eV mR . 2 MN ∼ mR • For 0.1 < MN < 100 GeV/c , we have 3× 2 −10 −8 Uα ∼ 10 − 10 . 3×

0.100 90% limits from

0.001 current experiments 2 eI U 10-5 IHEP-JINR CHARM ATLAS NA3 on the mixing of Pion decay L3 Three new heavy neutrinos at an -7 Kaon decay DELPHI 10 PS191 unknown scale (eV → GUT)! heavy neutrinos to 0.01 0.10 1 10 100 electron and muon. MI [GeV] Search for heavy neutrinos with the T2K experiment Poster # 43, Wednesday session Presenter: M. Lamoureux Analysis and results: Detection in T2K: • Remaining background after selection: Heavy neutrinos are produced alongside less than 2 evts (from active ν int.) standard neutrino beam. They propagate and can decay in T2K near • Bayesian approach, marginalization detector ND280 → detection of 2 particles with a Markov Chain Monte Carlo.

−6 T2K preliminary with opposite charges. 2 e 10 U 2 T2K U PS191 (2•body) + + ± ∓ ± ∓ − e K → ` N N → ` π , ` ` ν 10 7 PS191 (3•body)

beam 280m ! dump detectors −8 p off-axisoff-axis "! 10 target 2.5 o 90% C.L. station decay muon − pipe monitors Super-Kamiokande 10 9

0m0m 110m140m 120m 280m 280m 295km − 10 10 150 200 250 300 350 400 450 500 2 T2K put the MN [MeV/c ] simulation −6 T2K preliminary

2 µ 10

U most stringent 2 T2K pion Uµ PS191 (2•body) limits in the 10−7 PS191 (3•body) heavy neutrino muon E949 high mass region. 10−8

10−9

10−10 150 200 250 300 350 2 MN [MeV/c ] Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

T2K Oscillation Analysis How to evaluate ?

T2K oscillation analysis aims to extract oscillation Cross-section mismodelling could introduce probability from a rate of event in the Super-K biases on the final values of oscillation detector. parameters. ➤ Need to evaluate this Need to modelize neutrino flux and interaction. Cross-section Osc. Probability 1) Build simulated data at ND280 and Flux Det. Efficiency SK with alternative models. External data Build some flux and cross-section models with external 2) Fit at ND280 with data sets (NA61/SHINE, MINERνA, MiniBooNE…) nominal model.

ND280 data 3) Propagate at SK Constrain those models with un-oscillated neutrino data and fit SK simulated at the near detector data.

Super-K data 4) Compare the Fit those models to the Super-K data to extract the result with a fit to the oscillation parameters of interest : θ Δm2 θ δ 23 32 13 CP nominal MC.

Simon Bienstock 1 Studying the impact of neutrino cross-section mismodelling on the T2K oscillation analysis Poster #48

What’s the impact on the analysis ? An additional uncertainty

We can quantify this effect by comparing 1D The biases being too large, defined a procedure oscillation parameters likelihood curves. based on the results of the study to have an additional uncertainty.

➤ Additional parameter being able to absorb shape effects.

➤ Smearing of the oscillation parameters likelihood.

We get bias for all the alternative models and oscillation parameters. This additional uncertainty impacts mainly 2 the disappearance parameters θ23 Δm 32 We can define if biases are acceptable.

Simon Bienstock 2 Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

Ashley Back (ISU), Liudmila Kolupaeva (JINR)

on behalf of the NOvA Collaboration

Poster №82

June 2018 NEUTRINO 2018

A.Back, L. Kolupaeva NOvA results June 2018 1 / 3 The NuMI Oﬀ-Axis νe Appearance Experiment. 2018 analysis results

Neutrino oscillation physics goals: With 8.85 ×1020 POT in ν mode 0 ν Mass Hierarchy and 6.91 ×1020 POT in ν¯ mode we found:

0 δCP 0 58 νe event with background expectation 15.1 2 0 octant of θ23 and ∆m32 0 18 ν¯ events with background expectation 5.3

Neutrino beam NOvA Preliminary Antineutrino beam NOvA Preliminary Low PID High PID Low PID High PID 12 20 FD data FD data 2018 Best Fit 10 2018 Best Fit Wrong Sign Bkg. Wrong Sign Bkg. POT-equiv POT-equiv

15 Total Beam Bkg. Core 8 Total Beam Bkg. Core 20 20

Cosmic Bkg. Peripheral Cosmic Bkg. Peripheral 10 10 × × 6 10

5 2 Events / 6.91 Events / 8.85 0 0 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 Reconstructed Neutrino Energy (GeV) Reconstructed Neutrino Energy (GeV)

Fitting the νe and νµ spectra we get the following results.

A.Back, L. Kolupaeva NOvA results June 2018 2 / 3 Joint νe + νµ ﬁt 2018 analysis results

NOvA Preliminary NOvA Preliminary 0.7 0.7

0.6 0.6 23 23 θ θ

2 0.5 2 0.5 sin sin 0.4 0.4

1σ 2σ 3σ Best Fit 1σ 2σ 3σ Best Fit 0.3 NH 0.3 IH 0 π π 3π 2π 0 π π 3π 2π 2 δ 2 2 δ 2 CP CP NOvA FD 8.85×1020 POT equiv ν + 6.9×1020 POT ν

5 NOvA Preliminary Joint ﬁt results: NH Lower octant

) NH Upper octant 0 Best ﬁt: 4 σ IH Lower octant NH, δCP = 0.17π, IH Upper octant 2 3 sin θ23 = 0.58 ± 0.03 (UO), 2 +0.12 −3 2 ∆m32 = 2.51−0.08 × 10 eV 2 0 Reject the IH, δCP = π/2 at >3σ, reject IH, all values of δCP at 1.8σ.

Significance ( 1

00 π π 3π 2π See the poster №82 for details 2 δ 2 CP A.Back, L. Kolupaeva NOvA results June 2018 3 / 3 Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

In order for MicroBooNE to weigh in on the origin of the LEE, we need concrete models to test.

For this we need to move from the observed excess in MiniBooNE data to a predicted true underlying excess.

E.g. Electron-like Model

First step, construct a response matrix from MiniBooNE Reconstructed Energy Spectrum Monte Carlo Simulations which, for a given hypothesis, contains all the detector, reconstruction and selection 1 effects. Unfold!

Removes Detector Smearing, Reconstruction Effects, Analysis Selections, ..etc..

Reconstructed Energy Spectrum True Neutrino Energy Spectrum

Given an underlying hypothesis, the constructed response matrix is

used to “unfold” and remove all analysis specific and detector effects, recovering the true underlying excess For an example& more, #114 photon-like modelPoster In this electron-like example we assume the excess is solely due to an Come see my energy dependent increase in the intrinsic e CC event rate 2 Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

WIMP

20 years of atmospheric neutrino data collected ν with the Super-K is used ~50 000 events In the Earth’s core, the spin- independent (SI) interactions dominate in the capture For each tested WIMP mass and annihilation channel, process. we find the configuration of ATM BKG + DM SIGNAL that would match DATA the best.

19 samples, binned in lepton momentum &

cosθZ → 595 bins

If the WIMP mass matches the mass of a heavy element in the Earth, the capture rate will increase considerably. No excess of dark matter induced neutrinos has been observed as 90% CL limits on WIMP-nucleon SI scattering x-section compared to atmospheric ν bkg

The peaks correspond to resonant capture on the most abundant elements: 16O, 24Mg, 28Si and 56Fe, and their isotopes.

The strongest limits among all neutrino experiments up to date. wide range of tested WIMP masses Majority of the WIMP parameter space favored three dark matter annihilation channels by the DAMA/LIBRA results is ruled out. considered unique sensitivity for low energies → poster #134 Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

Littlest Seesaw: SM extension with 2 new RHν singlets Renormalisation Group Evolution: Evolve observables to low scales using RG running (REAP) Leptogenesis: 0 Lepton asymmetry generated through decay of lightest RHν 12 ! = % & !)* ! = ( ! "# # # '( " 37 )* *,-,/,0 Susana Molina Sedgwick NEUTRINO 2018

Method: Fit high scale parameters to low scale neutrino data and BAU from Leptogenesis (χ2 analysis)

Scan over neutrino masses: -2 & )+ 1.0 × 10 ≤ () ≤ 5.0 × 10 [GeV] b/10 #+ 5"# ≤ "% ≤ 1.0 × 10 [GeV] and a, b : free parameters in Yukawa matrices

4-dimensional gridding

LS highly predictive: 7 observables Case A Case D from 4 parameters 10 13 Matm / GeV 5.051 x 10 1.357 x 10 Excellent ﬁt; suggests δ ≃ −90°; allows 13 10 Msol / GeV 5.067 x 10 1.056 x 10 indirect prediction of RHν masses a 0.00805868 0.13484 b 0.082948 0.00115694 Learn about Testable at high energies low energies χ2 / d.o.f. 3.17 / 3 4.65 / 3 Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114

✓• ✓• The rich radiative They are environment abundant in boost the �� the nearby reation. Universe. • ✗• But they are too ✗Their photon rare in the density is not Universe to enough to �� produce the trigger entire neutrino reation. (low flux observed by accretion rate) IceCube. (No BUT multiplets ✓ detection) • structured jet could potentially boost the BL Lac emission up to the level required by the � detected by IceCube! ✓• Righi C. Tavecchio F. TXS0506+056 is a BL Lac object!! BL Lac as neutrino emitters

TXS0506+056 is a BL Lac of 2FHL catalogue (Fermi detection above 50GeV).

Assuming BL Lacs objects of 2FHL as the only emitters of IceCube neutrino flux:

• We assume a simple linear relation between �-ray and neutrino fluxes, �and � to obtain a neutrino flux for each source and the expected count rate observed by IceCube and Km3NeT.[Righi et al. 2017] • We started an observational campaign to a better characterization of 7 others BL Lacs of 2FHL in spatial correlation with a neutrino event.[Righi et al. submitted]

A NEW PROBLEM:

Mkn421 is the brightest BL Lac object in the sky. Why we we do not have clear detection of neutrino events from this source?[Righi et al. in prep.]

For more details have a look to my poster

2 Righi C. Tavecchio F. Poster Prize Competition: Wednesday Finals 2’40” each presentations ordered along the poster wall no. Title Presenter Poster wall Neutrino physics with the XMASS liquid xenon detector Katsuki HIRAIDE (ICRR, University of Tokyo) 1

Studying the impact of neutrino cross-section mismodelling on the T2K oscillation Simon BIENSTOCK (LPNHE) 48 analysis

NOvA joint ve + vµ oscillation results in neutrino and antineutrino modes Liudmila KOLUPAEVA (JINR) 82

MicroBooNE tests of the MiniBooNE Low Energy Excess Mark ROSS-LONERGAN (Columbia University) 114