Solar NeutrinosPerspectives and Objectives

Mark ChenQueenrsquos University and Canadian Institute for Advanced Research (CIFAR)

Outline

This is a short talk reviewing where we are with respect to two aspects of solar neutrinos

bull solar neutrino spectrum ndash astrophysicsbull neutrino oscillations survival probability versus neutrino

energy ndash particle physics

Solar Neutrino Energy Spectrum

Survival Probability ndash Pee(Eν)Borexino Nature 512 383 (2014)

SNO PRC 88 025501 (2013)

Pee

Eν

LMA day-night asymmetryNight ndash blue

Day ndash red

Have Been Detectedbull pp [Borexino radiochemical Ga experiments]

bull confirmed the Sun shines by pp fusion

bull 7Be [Borexino radiochemical Cl experiment]bull confirmed neutrino oscillations

bull pep [Borexino]bull has potential for probing vacuum-matter transition

bull 8B [SNO Super-Kamiokande Borexino KamLAND]bull observed neutrino flavour conversionbull measures θ12

Still to be Detectedbull CNObull hep SNO upper limit lt 23 times 104 cm1113113ndash2 sndash11131131

CNO Electron Capture Linesbull often forgotten

bull not all that significant

bull 13N line 2220 MeVbull 15O line 2754 MeVbull 17F line 2761 MeV

bull was an insignificant background for SNO NCbull line sources ndash opportunity for CNO detection

Stonehill Formaggio Robertson

pp solar neutrinosbull large liquid scintillators with low 14C can detect like

Borexino didbull liquid xenon has the potential to detect pp solar neutrinos

bull LZ XENON1T PANDAX XMASSbull ~1 pp event(day-tonne) with 50 keV threshold

LZ detector diagram

Borexino Nature 512 383 (2014)

bull analysis tags used to reject 11C by factor ~10 keeping 50 of the signal

bull 98 CL detection or 205σ

98CL

pep Borexino

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Outline

This is a short talk reviewing where we are with respect to two aspects of solar neutrinos

bull solar neutrino spectrum ndash astrophysicsbull neutrino oscillations survival probability versus neutrino

energy ndash particle physics

Solar Neutrino Energy Spectrum

Survival Probability ndash Pee(Eν)Borexino Nature 512 383 (2014)

SNO PRC 88 025501 (2013)

Pee

Eν

LMA day-night asymmetryNight ndash blue

Day ndash red

Have Been Detectedbull pp [Borexino radiochemical Ga experiments]

bull confirmed the Sun shines by pp fusion

bull 7Be [Borexino radiochemical Cl experiment]bull confirmed neutrino oscillations

bull pep [Borexino]bull has potential for probing vacuum-matter transition

bull 8B [SNO Super-Kamiokande Borexino KamLAND]bull observed neutrino flavour conversionbull measures θ12

Still to be Detectedbull CNObull hep SNO upper limit lt 23 times 104 cm1113113ndash2 sndash11131131

CNO Electron Capture Linesbull often forgotten

bull not all that significant

bull 13N line 2220 MeVbull 15O line 2754 MeVbull 17F line 2761 MeV

bull was an insignificant background for SNO NCbull line sources ndash opportunity for CNO detection

Stonehill Formaggio Robertson

pp solar neutrinosbull large liquid scintillators with low 14C can detect like

Borexino didbull liquid xenon has the potential to detect pp solar neutrinos

bull LZ XENON1T PANDAX XMASSbull ~1 pp event(day-tonne) with 50 keV threshold

LZ detector diagram

Borexino Nature 512 383 (2014)

bull analysis tags used to reject 11C by factor ~10 keeping 50 of the signal

bull 98 CL detection or 205σ

98CL

pep Borexino

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Solar Neutrino Energy Spectrum

Survival Probability ndash Pee(Eν)Borexino Nature 512 383 (2014)

SNO PRC 88 025501 (2013)

Pee

Eν

LMA day-night asymmetryNight ndash blue

Day ndash red

Have Been Detectedbull pp [Borexino radiochemical Ga experiments]

bull confirmed the Sun shines by pp fusion

bull 7Be [Borexino radiochemical Cl experiment]bull confirmed neutrino oscillations

bull pep [Borexino]bull has potential for probing vacuum-matter transition

bull 8B [SNO Super-Kamiokande Borexino KamLAND]bull observed neutrino flavour conversionbull measures θ12

Still to be Detectedbull CNObull hep SNO upper limit lt 23 times 104 cm1113113ndash2 sndash11131131

CNO Electron Capture Linesbull often forgotten

bull not all that significant

bull 13N line 2220 MeVbull 15O line 2754 MeVbull 17F line 2761 MeV

bull was an insignificant background for SNO NCbull line sources ndash opportunity for CNO detection

Stonehill Formaggio Robertson

pp solar neutrinosbull large liquid scintillators with low 14C can detect like

Borexino didbull liquid xenon has the potential to detect pp solar neutrinos

bull LZ XENON1T PANDAX XMASSbull ~1 pp event(day-tonne) with 50 keV threshold

LZ detector diagram

Borexino Nature 512 383 (2014)

bull analysis tags used to reject 11C by factor ~10 keeping 50 of the signal

bull 98 CL detection or 205σ

98CL

pep Borexino

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Survival Probability ndash Pee(Eν)Borexino Nature 512 383 (2014)

SNO PRC 88 025501 (2013)

Pee

Eν

LMA day-night asymmetryNight ndash blue

Day ndash red

Have Been Detectedbull pp [Borexino radiochemical Ga experiments]

bull confirmed the Sun shines by pp fusion

bull 7Be [Borexino radiochemical Cl experiment]bull confirmed neutrino oscillations

bull pep [Borexino]bull has potential for probing vacuum-matter transition

bull 8B [SNO Super-Kamiokande Borexino KamLAND]bull observed neutrino flavour conversionbull measures θ12

Still to be Detectedbull CNObull hep SNO upper limit lt 23 times 104 cm1113113ndash2 sndash11131131

CNO Electron Capture Linesbull often forgotten

bull not all that significant

bull 13N line 2220 MeVbull 15O line 2754 MeVbull 17F line 2761 MeV

bull was an insignificant background for SNO NCbull line sources ndash opportunity for CNO detection

Stonehill Formaggio Robertson

pp solar neutrinosbull large liquid scintillators with low 14C can detect like

Borexino didbull liquid xenon has the potential to detect pp solar neutrinos

bull LZ XENON1T PANDAX XMASSbull ~1 pp event(day-tonne) with 50 keV threshold

LZ detector diagram

Borexino Nature 512 383 (2014)

bull analysis tags used to reject 11C by factor ~10 keeping 50 of the signal

bull 98 CL detection or 205σ

98CL

pep Borexino

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Have Been Detectedbull pp [Borexino radiochemical Ga experiments]

bull confirmed the Sun shines by pp fusion

bull 7Be [Borexino radiochemical Cl experiment]bull confirmed neutrino oscillations

bull pep [Borexino]bull has potential for probing vacuum-matter transition

bull 8B [SNO Super-Kamiokande Borexino KamLAND]bull observed neutrino flavour conversionbull measures θ12

Still to be Detectedbull CNObull hep SNO upper limit lt 23 times 104 cm1113113ndash2 sndash11131131

CNO Electron Capture Linesbull often forgotten

bull not all that significant

bull 13N line 2220 MeVbull 15O line 2754 MeVbull 17F line 2761 MeV

bull was an insignificant background for SNO NCbull line sources ndash opportunity for CNO detection

Stonehill Formaggio Robertson

pp solar neutrinosbull large liquid scintillators with low 14C can detect like

Borexino didbull liquid xenon has the potential to detect pp solar neutrinos

bull LZ XENON1T PANDAX XMASSbull ~1 pp event(day-tonne) with 50 keV threshold

LZ detector diagram

Borexino Nature 512 383 (2014)

bull analysis tags used to reject 11C by factor ~10 keeping 50 of the signal

bull 98 CL detection or 205σ

98CL

pep Borexino

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

CNO Electron Capture Linesbull often forgotten

bull not all that significant

bull 13N line 2220 MeVbull 15O line 2754 MeVbull 17F line 2761 MeV

bull was an insignificant background for SNO NCbull line sources ndash opportunity for CNO detection

Stonehill Formaggio Robertson

pp solar neutrinosbull large liquid scintillators with low 14C can detect like

Borexino didbull liquid xenon has the potential to detect pp solar neutrinos

bull LZ XENON1T PANDAX XMASSbull ~1 pp event(day-tonne) with 50 keV threshold

LZ detector diagram

Borexino Nature 512 383 (2014)

bull analysis tags used to reject 11C by factor ~10 keeping 50 of the signal

bull 98 CL detection or 205σ

98CL

pep Borexino

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

pp solar neutrinosbull large liquid scintillators with low 14C can detect like

Borexino didbull liquid xenon has the potential to detect pp solar neutrinos

bull LZ XENON1T PANDAX XMASSbull ~1 pp event(day-tonne) with 50 keV threshold

LZ detector diagram

Borexino Nature 512 383 (2014)

bull analysis tags used to reject 11C by factor ~10 keeping 50 of the signal

bull 98 CL detection or 205σ

98CL

pep Borexino

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

bull analysis tags used to reject 11C by factor ~10 keeping 50 of the signal

bull 98 CL detection or 205σ

98CL

pep Borexino

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Borexino pep Δχ2 Details

LMA oscillated rate

SSM rate

A Wright

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Borexino CNO Upper Limitbull upper limit at 99CL is

bull 2 times High-Zbull 3 times Low-Z

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Deep Site Needed for CNO Solar Neutrino Detectionbull deep underground site (eg SNOLAB Jinping) reduces

cosmogenic 11C background

Borexino at Gran Sasso 3800 mwe SNO+ at SNOLAB 6000 mwe

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Pb-210Bi-210 Backgrounds

SNO+ signal extraction study

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

How to Improve pep and CNObull Borexino nice work to suppress 11C background though

some remains and the 210Bi-CNO separation remains difficultbull suppressing further by factors ~100 or more (depth) and also

tagging will open up the window for improved spectral fitting

bull 210Bi-CNO solar can be separated in principlebull lowest 210Bi backgrounds possible helps to facilitate

bull CNO and pep signals have covariances as shown thus improving CNO signal extraction improves pep (plus lower backgrounds help directly improve pep signal extraction)

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

SNO+ CNO and SNO 8Bbull use the SNO 8B measurement to constrain ldquoenvironmental

variablesrdquo in the solar core which also affects CNO νbull measure CNO flux (to plusmn10) and compare with solar models

to differentiate high-Z low-Z core metallicity

agrave la Haxton and Serenelli

where will theSNO+ CNOmeasurementpoint to

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

What Still to Learn from 8Bbull ldquomap outrdquo the solar neutrino survival probability Pee as a

function of Eν

bull can give us a handle on new physicsbull ideal to use pep or lower energy 8B for this

bull observation of the day-night effect by Super-K at 27σ is there a need to improve

figure from H Sekiyarsquos talk at LRT 2015

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Entire Slide for M Nakahatarsquos Talkat NeuTel 2015

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

New Physics at the Vacuum-Matter Transition

Friedland Lunardini Pentildea-GarayPee curve with non-standard interactions

de Holanda and Smirnov

Sterile Neutrinos

Mass-Varying Neutrinos

Gonzalez-Garcia Maltoni

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Entire Slide from H Sekiyarsquos Talk

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

Low Energy 8B Solar Neutrinos in SNO+

SNO+ 1 yr

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

CC Reactions on 13Cbull tagged interaction

bull 11 natural abundancebull log ft = 367 threshold 22 MeVbull followed by 13N β+ decay with 100 min half-lifebull use energy window time and spatial coincidence to reject

backgrounds

bull CC offers potentially better spectral shape determination (than ES from SNO+ lower energy 8B or Super-K)

from Ianni Montanino Villante

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν

13C Low Energy 8B Solar νbull rate of ~20 eventsktonyr including detection efficiency

(cuts)bull observe the reaction and then observe 13N decay at

the same position with energy between 10-22 MeV within ~30 min

bull potentially very little background (cosmogenic or radioactive)

bull need a 10 kton-sized detector (or larger like JUNO or LENA) to get an appreciable signal

• Slide 1
• Outline
• Solar Neutrino Energy Spectrum
• Survival Probability ndash Pee(Eν)
• Have Been Detected
• CNO Electron Capture Lines
• pp solar neutrinos
• pep Borexino
• Borexino pep Δχ2 Details
• Borexino CNO Upper Limit
• Deep Site Needed for CNO Solar Neutrino Detection
• Pb-210Bi-210 Backgrounds
• How to Improve pep and CNO
• SNO+ CNO and SNO 8B
• What Still to Learn from 8B
• Entire Slide for M Nakahatarsquos Talk at NeuTel 2015
• New Physics at the Vacuum-Matter Transition
• Entire Slide from H Sekiyarsquos Talk
• Low Energy 8B Solar Neutrinos in SNO+
• CC Reactions on 13C
• 13C Low Energy 8B Solar ν