Long-baseline searches for sterile neutrinos using neutral current - - PowerPoint PPT Presentation

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Jun 09, 2023 114 likes •303 views

Long-baseline searches for sterile neutrinos using neutral current interactions in NOvA Jeremy Hewes New Perspectives 2018 19th June 2018 Introduction Previous NOvA talks considered neutral currents as a background to charged current

SLIDE 1

Long-baseline searches for sterile neutrinos using neutral current interactions in NOvA

Jeremy Hewes New Perspectives 2018 19th June 2018

SLIDE 2

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Introduction

Previous NOvA talks considered neutral currents as a background to

charged current processes. This talk discusses NOvA’s 2018 searches for neutral current disappearance, in which NCs are the signal!

Overview:
Motivation and experimental overview.
Search for NC disappearance in neutrino data, and upcoming

plans with new covariance method.

Search for NC disappearance in antineutrino data, using standard

extrapolation technique.

Future plans for NOvA sterile neutrino searches.

SLIDE 3

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

3+1 sterile neutrino oscillations

Search for evidence of mixing

between active neutrino states (νe, νμ, ντ) and fourth sterile state (νs).

Look for disappearance among

neutral current (NC) events, which are insensitive to standard three-flavour

scillations.
Approximate near detector

(SBL) and far detector (LBL)

scillation probabilities on right.
Note that in analysis, use

exact treatment of 3+1

scillation probabilities.

    νe νµ ντ νs     =     Ue1 Ue2 Ue3 Ue4 Uµ1 Uµ2 Uµ3 Uµ4 Uτ1 Uτ2 Uτ3 Uτ4 Us1 Us2 Us3 Us4         ν1 ν2 ν3 ν4    

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1 − P LBL,3+1

νµ→νs

≈ 1 − 1 2 cos4 θ14 cos2 θ34 sin2 θ24

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+A sin2 ∆31 − B sin 2∆31

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sha1_base64="H6/BLEy6C31bGCxUH6+LHUzyD4=">ACFHicbZDLSsNAFIYnXmu9RV26GSyCUCxJFXRZqwuXFewFmhgm0k7dDIJMxOhD6EG1/FjQtF3Lpw59s4abOorT8M/HznHM6c348Zlcqyfoyl5ZXVtfXCRnFza3tn19zb8koEZg0cQi0fGRJIxy0lRUMdKJBUGhz0jbH15n9fYjEZJG/F6NYuKGqM9pQDFSGnlmuXzlSMof0urYuSFMIS89s8fwFNYzDKtwhnpmyapYE8FY+emBHI1Pb6U4CQlXmCEpu7YVKzdFQlHMyLjoJLECA9Rn3S15Sgk0k0nR43hsSY9GERCP67ghM5OpCiUchT6ujNEaiDnaxn8r9ZNVHDpTHiSIcTxcFCYMqglCsEcFwYqNtEFYUP1XiAdIKx0jkUdgj1/8qJpVSu2VbHvzku1eh5HARyCI3ACbHABauAWNEATYPAEXsAbeDejVfjw/icti4Z+cwB+CPj6xfBdJy8</latexit>

P SBL,3+1

νµ→νµ

= 1 − 4|Uµ4|2(1 − |Uµ4|2) sin2 ∆41

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= 1 − cos2 θ14 sin2 θ24 sin2 ∆41

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∆ab = ∆m2

abL

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A = sin2 θ34 sin2 2θ23

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B = 1 2 sin δ24 sin θ24 sin 2θ34 sin 2θ23

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SLIDE 4

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018 4

L/E (km/GeV)

10 1 10

10 )

ν →

ν 1 - P( 0.2 0.4 0.6 0.8 1 1.2 0.2 0.4 0.6 0.8 1 1.2 3-Flavor Prob.

= 0.05 eV

41 2

m Δ

= 0.5 eV

41 2

m Δ

= 5 eV

41 2

m Δ

ND FD

Neutrino Energy (GeV) 1 10

10 Neutrino Energy (GeV) 1 10

3+1 sterile neutrino oscillations

Δm32 Δm21 Δm41 ν4 ν3 ν2 ν1

Signal is always a deficit, never an

excess — “smoking gun”.

Sensitive to mixing parameters

θ24, θ34, Δm412 and δ24.

SLIDE 5

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

NOvA (NuMI Off-axis νe Appearance) is a long-baseline

accelerator experiment based at Fermilab.

Measures neutrinos from Fermilab’s NuMI beam.
Functionally identical plastic scintillator near and far

detectors.

ND: 1km baseline, FNAL, 300 tons.
FD: 810km baseline, Ash River, 14 kt, 14 mrad off-

axis.

The NOvA experiment

SLIDE 6

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Previous NOvA NC analyses

Previous NOvA analyses searched for NC disappearance in neutrino data using

standard extrapolation technique.

Allowed regions in θ24 vs θ34 parameter space produced at fixed values of Δm412.
Extrapolation technique limited to parameter space where no sterile oscillations occur in

near detector, Δm412 < 5 eV2.

(deg.)

θ

10 20 30 40

(deg.)

θ

10 20 30 40

NOvA 2016: 68% C.L. NOvA 2016: 90% C.L. NOvA 2017: 68% C.L. NOvA 2017: 90% C.L.

NOvA Preliminary

Energy Deposited in Scintillator (GeV)

1 2 3 4 5 6 7 8 9 10

POT

Events / 0.5 GeV / 8.85x10

20 40 60 80

FD Data

Syst. Uncertainty

3 Flavor NC Prediction Cosmic Background CC Background

ν CC Background

= 2.44x10

32 2

m Δ ° = 45

θ , ° = 8.5

θ = 1.097 NDF

NOvA Preliminary

2017 analysis

SLIDE 7

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

New NOvA NC analyses

Two new analyses for 2018:
Re-analyse neutrino beam dataset with new event selection and joint

two-detector method.

Analyse new antineutrino beam dataset with previously used

extrapolation technique.

Both analyses utilise NOvA’s machine learning-based CVN (see previous

talk by M. Groh) for event selection — arXiv:1604.01444

Cosmic rejection and event selection retrained since previous analysis.
Sample purity improved without sacrificing signal selection efficiency.

SLIDE 8

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Neutrino beam data event selection

Cosmic rejection:

EM showers travelling

away from beam.

Transverse momentum

cut.

Activity close in time to

candidate event.

NC-specific boosted

decision tree (BDT) trained to reject cosmics.

Event selection:

Use Convolutional Visual Network (CVN) event

selection technique to identify NC events.

Dominant backgrounds are charged current (CC)

and cosmic interactions.

Events

NC Selection Cosmic Rejection Containment Event Quality Data Quality

Cosmic Background CC Background NC 3 Flavor Simulation Neutrino Beam

NOvA Preliminary

0.2 0.4 0.6 0.8 1

CVNnc Identifier

POT-equiv

10 × Events / 8.85

Neutrino Beam FD Data: NC Simulation CC Background Cosmic Background

NOvA Preliminary

0.2 0.4 0.6 0.8 1

Cosmic Rejection BDT Response

20 40 60 80

POT-equiv

10 × Events / 8.85

Neutrino Beam FD Data: NC Simulation CC Background Cosmic Background

NOvA Preliminary

SLIDE 9

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Neutral current candidate event

SLIDE 10

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Covariance method

At high sterile mass splitting Δm412,

extrapolation method breaks down due to disappearance in near detector.

Use covariance matrix to treat both

detectors on an equal footing, while still cancelling systematic uncertainties.

10 20 30 40

Deposited energy bins

10 20 30 40

Deposited energy bins

0.1 0.2

Fractional covariance

NOvA Preliminary

Neutrino Beam ND FD ND FD

χ2 =

X

i=1 N

X

j=1

(xi − µi)[V −1]ij(xj − µj)

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Vij,syst = PU

n=1(Sn,i − µi)(Sn,j − µj)

U − 1

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L/E (km/GeV)

10 1 10

10 )

ν →

ν 1 - P( 0.2 0.4 0.6 0.8 1 1.2 0.2 0.4 0.6 0.8 1 1.2 3-Flavor Prob.

= 0.05 eV

41 2

m Δ

= 0.5 eV

41 2

m Δ

= 5 eV

41 2

m Δ

ND FD

Neutrino Energy (GeV) 1 10

10 Neutrino Energy (GeV) 1 10

SLIDE 11

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Neutrino beam data results

Observed 201 events, compared to 188

± 13 (syst.) predicted from MC simulation.

Consistent with three-flavour oscillations.

Far detector spectrum

Signal uncertainty (%)

20 − 20 Statistical error Total syst. error Beam Calibration Kaon Uncertainty Light Levels Neutrino Interaction Neutron Uncertainty Normalisation Oscillation Param PPFX Tau Uncertainty

NOvA Preliminary

5 10 15 20

Deposited Energy (GeV)

5 10 15 20 25

POT-equiv / 0.25 GeV

10 × Events / 8.85

Neutrino Beam FD Data:

syst. range

σ 1 Total Simulation Beam-induced Backgrounds Cosmic-induced Background

NOvA Preliminary

Far detector signal systematic uncertainties dominated by cross-sections. Large uncertainty on kaon flux in neutrino beam. Significant contributions from flux uncertainties.

SLIDE 12

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Antineutrino beam data event selection

Events

NC Selection Cosmic Rejection Containment Event Quality Data Quality

Cosmic Background CC Background NC 3 Flavor Prediction Antineutrino Beam

NOvA Preliminary

0.2 0.4 0.6 0.8 1

CVNnc Identifier

1 10

POT

10 × Events / 6.91

Antineutrino Beam FD Data: NC Prediction CC Background Cosmic Background

NOvA Preliminary

0.2 0.4 0.6 0.8 1

Cosmic Rejection BDT Response

20 40 60 80 100 120 140

POT

10 × Events / 6.91

Antineutrino Beam FD Data: NC Prediction CC Background Cosmic Background

NOvA Preliminary

Event selection:

Use Convolutional Visual Network (CVN) event

selection technique to identify NC events.

Dominant background are charged current (CC)

and cosmic interactions. Cosmic rejection:

EM showers travelling

away from beam.

Transverse momentum

cut.

Activity close in time to

candidate event.

NC-specific boosted

decision tree (BDT) trained to reject cosmics.

SLIDE 13

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

20 − 10 − 10 20

Signal uncertainty (%)

Statistical error Total syst. error X-section tune Neutron Kaon Beam Light Level GENIE Calibration

Antineutrino beam data results

Observed 61 compared to 69 ± 8 (syst.) from MC

prediction.

Use extrapolation method to create 68% CL allowed

region (non-FC corrected).

1D 68% CL limits: 25.5° for θ24, 31. 5° for θ34.
Anticipate limit will improve as NOvA adds more statistics.

5 10 15 20

Deposited Energy (GeV)

5 10 15 20

POT

10 × Events / 1 GeV / 6.91

Antineutrino Beam FD Data:

syst. range

σ 1 Total Prediction Beam-induced Backgrounds Cosmic-induced Background

NOvA Preliminary

10 20 30 40 50

(degrees)

10 20 30 40

(degrees)

NOvA 2018 68% C.L.

Antineutrino Beam POT

10 × 6.91

10 × = 2.44

32 2

m Δ = 0.558

sin , ° = 8.3

= 0.5 eV

41 2

m Δ

NOvA Preliminary

SLIDE 14

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

4 −

3 −

2 −

1 −

10 1

sin

1 −

10 1 10

)

(eV

41 2

m Δ

Super-Kamiokande 90% CL

Future plans

Development of covariance method

allows for limits to be set over a broader range of parameter space.

First, analysis of neutrino beam data

using covariance method allows limits to be set in Δm412.

Once this method is used for neutrino

beam data, it can be extended to antineutrino beam data also.

More long-term goal: set limit using

neutrino and antineutrino data simultaneously.

4 −

3 −

2 −

1 −

10 1

sin

2 −

1 −

10 1 10

)

(eV

41 2

m Δ

CDHS 90% CL CCFR 90% CL SciBooNE+MiniBooNE 90% CL Super-Kamiokande 90% CL IceCube 90% CL MINOS 90% CL

SLIDE 15

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Summary

Search for active neutrino disappearance into a sterile flavour state in NOvA.
Both neutrino and antineutrino data are consistent with three-flavor
scillations.
Produced 68% CL allowed region in θ24 vs θ34 for antineutrino data using

extrapolation method.

Will use covariance method to perform a joint ND-FD fit to produce contours

in θ24, θ34 and Δm412 for neutrino data.

In the longer term, intend to perform similar analyses for antineutrino data,

and ultimately fit neutrino and antineutrino data (and CC and NC data) simultaneously.

http://novaexperiment.fnal.gov

SLIDE 16

Backup slides

SLIDE 17

Searches for sterile neutrinos in NOvA | J. Hewes | New Perspectives 2018

Neutrino beam data systematic uncertainties

Signal uncertainty (%)

20 − 20 Statistical error Total syst. error Beam Calibration Kaon Uncertainty Light Levels Neutrino Interaction Neutron Uncertainty Normalisation Oscillation Param PPFX Tau Uncertainty

NOvA Preliminary

Background uncertainty (%)

40 − 20 − 20 40 Statistical error Total syst. error Beam Calibration Kaon Uncertainty Light Levels Neutrino Interaction Neutron Uncertainty Normalisation Oscillation Param PPFX Tau Uncertainty

NOvA Preliminary

Signal uncertainty (%)

30 − 20 − 10 − 10 20 30 Statistical error Total syst. error Beam Calibration Kaon Uncertainty Light Levels Neutrino Interaction Neutron Uncertainty Normalisation Oscillation Param PPFX

NOvA Preliminary

Background uncertainty (%)

30 − 20 − 10 − 10 20 30 Statistical error Total syst. error Beam Calibration Kaon Uncertainty Light Levels Neutrino Interaction Neutron Uncertainty Normalisation Oscillation Param PPFX

NOvA Preliminary