Short-Baseline may hide lots of New Physics! ⌫ H ⌫ 4 Non-Unitarity � � U τ 1 U ∗ ∆ m 2 τ 2 � � U µ 1 U ∗ � � � � U e 1 U ∗ µ 2 43 e 2 � � U µ 1 U ∗ � � µ 2 arxiv:1503.08879 ⌫ 3 Near Detec- tor Physics ∆ m 2 32 ⌫ 2 ∆ m 2 21 ⌫ 1 Light Sterile arxiv:1507.08204 Neutrino 5 / 24
Short-Baseline may hide lots of New Physics! ⌫ H ⌫ 4 Non-Unitarity 1.0 � � U τ 1 U ∗ ∆ m 2 τ 2 � � U µ 1 U ∗ � � � � 0.8 U e 1 U ∗ µ 2 43 e 2 � � Survival Probability U µ 1 U ∗ � � µ 2 0.6 arxiv:1503.08879 ⌫ 3 Near Detec- 0.4 tor Physics ∆ m 2 32 0.2 ⌫ 2 ∆ m 2 0.0 21 ⌫ 1 0.001 0.010 0.100 1 10 100 Light Sterile L / E [ A.U. ] arxiv:1507.08204 Neutrino 5 / 24
Short-Baseline may hide lots of New Physics! 31 ∆ m 2 ⌫ H ⌫ 4 Non-Unitarity 1.0 � � U τ 1 U ∗ ∆ m 2 τ 2 � � U µ 1 U ∗ � � � � 0.8 U e 1 U ∗ µ 2 43 e 2 � � Survival Probability U µ 1 U ∗ � � µ 2 0.6 arxiv:1503.08879 ⌫ 3 Near Detec- 0.4 tor Physics ∆ m 2 32 0.2 ⌫ 2 ∆ m 2 0.0 21 ⌫ 1 0.001 0.010 0.100 1 10 100 Light Sterile L / E [ A.U. ] arxiv:1507.08204 Neutrino 5 / 24
Short-Baseline may hide lots of New Physics! 31 21 ∆ m 2 ∆ m 2 ⌫ H ⌫ 4 Non-Unitarity 1.0 � � U τ 1 U ∗ ∆ m 2 τ 2 � � U µ 1 U ∗ � � � � 0.8 U e 1 U ∗ µ 2 43 e 2 � � Survival Probability U µ 1 U ∗ � � µ 2 0.6 arxiv:1503.08879 ⌫ 3 Near Detec- 0.4 tor Physics ∆ m 2 32 0.2 ⌫ 2 ∆ m 2 0.0 21 ⌫ 1 0.001 0.010 0.100 1 10 100 Light Sterile L / E [ A.U. ] arxiv:1507.08204 Neutrino 5 / 24
Short-Baseline may hide lots of New Physics! 31 21 4 i ∆ m 2 ∆ m 2 ∆ m 2 ⌫ H ⌫ 4 Non-Unitarity 1.0 � � U τ 1 U ∗ ∆ m 2 τ 2 � � U µ 1 U ∗ � � � � 0.8 U e 1 U ∗ µ 2 43 e 2 � � Survival Probability U µ 1 U ∗ � � µ 2 0.6 arxiv:1503.08879 ⌫ 3 Near Detec- 0.4 tor Physics ∆ m 2 32 0.2 ⌫ 2 ∆ m 2 0.0 21 ⌫ 1 0.001 0.010 0.100 1 10 100 Light Sterile L / E [ A.U. ] arxiv:1507.08204 Neutrino 5 / 24
Short-Baseline may hide lots of New Physics! ⌫ H ⌫ 4 Non-Unitarity � � U τ 1 U ∗ ∆ m 2 τ 2 � � U µ 1 U ∗ � � � � U e 1 U ∗ µ 2 43 e 2 � � U µ 1 U ∗ � � µ 2 arxiv:1503.08879 ⌫ 3 Near Detec- tor Physics ∆ m 2 32 ⌫ 2 ∆ m 2 21 ⌫ 1 Light Sterile arxiv:1507.08204 Neutrino ∆ m 2 4 i ⇡ 1 eV 2 5 / 24
Short-Baseline may hide lots of New Physics! ⌫ H Non-Unitarity � � U τ 1 U ∗ τ 2 � � U µ 1 U ∗ � � � � U e 1 U ∗ µ 2 e 2 � � U µ 1 U ∗ � � µ 2 arxiv:1503.08879 Non- Near Detec- Standard tor Physics Interaction ⌫ 4 ∆ m 2 43 ⌫ 3 Light Sterile ∆ m 2 32 Neutrino ⌫ 2 ∆ m 2 21 ⌫ 1 arxiv:1507.08204 6 / 24
Short-Baseline may hide lots of New Physics! ⌫ H Non-Unitarity � � U τ 1 U ∗ τ 2 ⌫ i � � U µ 1 U ∗ � � � � U e 1 U ∗ µ 2 e 2 � � U µ 1 U ∗ � � µ 2 arxiv:1503.08879 Non- Near Detec- � , Z 0 .. Standard tor Physics Detector Interaction ⌫ j ⌫ 4 ∆ m 2 43 ⌫ 3 Light Sterile ∆ m 2 32 Neutrino ⌫ 2 ∆ m 2 21 ⌫ 1 arxiv:1507.08204 6 / 24
Short-Baseline may hide lots of New Physics! ⌫ H Non-Unitarity � � U τ 1 U ∗ τ 2 ⌫ i � � U µ 1 U ∗ � � � � U e 1 U ∗ µ 2 e 2 � � U µ 1 U ∗ � � µ 2 arxiv:1503.08879 Non- Near Detec- � , Z 0 .. Standard tor Physics Detector Interaction ⌫ j ⌫ 4 ∆ m 2 43 arxiv:1710.09360 ⌫ 3 Light Sterile ∆ m 2 32 Neutrino ⌫ 2 ∆ m 2 21 ⌫ 1 arxiv:1507.08204 6 / 24
Short-Baseline may hide lots of New Physics! production: Decay Propagation: Matter Detection: Charge Current l α ⌫ α Standard ⌫ α W l α W W P ⌫ α Non-Standard ⌫ α � , W 0 l α � , W 0 P ⌫ β 7 / 24
Short-Baseline may hide lots of New Physics! production: Decay Propagation: Matter Detection: Charge Current l α ⌫ α Standard ⌫ α W l α W W P ⌫ α Non-Standard ⌫ α � , W 0 l α � , W 0 P ⌫ β 7 / 24
Short-Baseline may hide lots of New Physics! production: Decay Propagation: Matter Detection: Charge Current l α ⌫ α Standard ⌫ α W l α W W P ⌫ α Non-Standard ⌫ α � , W 0 l α � , W 0 P ⌫ β 7 / 24
Short-Baseline may hide lots of New Physics! production: Decay Propagation: Matter Detection: Charge Current l α ⌫ α Standard ⌫ α W l α W W P ⌫ α Non-Standard ⌫ α � , W 0 l α � , W 0 P ⌫ β 7 / 24
Short-Baseline may hide lots of New Physics! production: Decay Propagation: Matter Detection: Charge Current l α ⌫ α Standard ⌫ α W l α W W P ⌫ α Non-Standard ⌫ α � , W 0 l α � , W 0 P ⌫ β 7 / 24
Short-Baseline may hide lots of New Physics! production: Decay Propagation: Matter Detection: Charge Current l α ⌫ α Standard ⌫ α W l α W W P ⌫ α Non-Standard ⌫ α � , W 0 l α � , W 0 P ⌫ β 7 / 24
Short-Baseline may hide lots of New Physics! production: Decay Propagation: Matter Detection: Charge Current l α ⌫ α Standard ⌫ α W l α W W P ⌫ α l β Non-Standard � , W 0 ⌫ α ⌫ α � , W 0 l α � , W 0 P ⌫ β 7 / 24
Short-Baseline may hide lots of New Physics! ⌫ H Non-Unitarity � � U τ 1 U ∗ τ 2 ⌫ i � � U µ 1 U ∗ � � � � U e 1 U ∗ µ 2 e 2 � � U µ 1 U ∗ � � µ 2 arxiv:1503.08879 Non- Near Detec- � , Z 0 .. Standard tor Physics Detector Interaction ⌫ j ⌫ 4 arxiv:1710.09360 ∆ m 2 43 ⌫ 3 Light Sterile ∆ m 2 32 Neutrino ⌫ 2 ∆ m 2 21 ⌫ 1 arxiv:1507.08204 8 / 24
Short-Baseline may hide lots of New Physics! ⌫ H Non-Unitarity � � U τ 1 U ∗ τ 2 ⌫ i � � U µ 1 U ∗ � � � � U e 1 U ∗ µ 2 e 2 � � U µ 1 U ∗ � � µ 2 arxiv:1503.08879 Non- Near Detec- � , Z 0 .. Standard tor Physics Detector Interaction ⌫ j ⌫ 4 arxiv:1710.09360 ∆ m 2 43 Source/Detec. NSI only ⌫ 3 Light Sterile ∆ m 2 32 Neutrino ⌫ 2 ∆ m 2 21 ⌫ 1 arxiv:1507.08204 8 / 24
We can put better constraints to new physics! Why are those (short-baseline) experiments interesting? 9 / 24
We can put better constraints to new physics! Why are those (short-baseline) experiments interesting? These new physics contain a short-distance (non-Standard) ⌫ µ ! ⌫ µ 9 / 24
We can put better constraints to new physics! Why are those (short-baseline) experiments interesting? These new physics contain a short-distance (non-Standard) ⌫ µ ! ⌫ µ Non-Unitarity NSI Sterile Neutrino ⇠ sin 2 2 ✓ µe P NU ⇠ | ↵ 21 | 2 P NSI ⇠ | ✏ d eµ + ✏ s eµ | 2 P 3+1 µe µe µe 9 / 24
We can put better constraints to new physics! Why are those (short-baseline) experiments interesting? These new physics contain a short-distance (non-Standard) ⌫ µ ! ⌫ µ Non-Unitarity NSI Sterile Neutrino ⇠ sin 2 2 ✓ µe P NU ⇠ | ↵ 21 | 2 P NSI ⇠ | ✏ d eµ + ✏ s eµ | 2 P 3+1 µe µe µe Thus, N e ⇠ � e + P NEW � µ µe 9 / 24
We can put better constraints to new physics! Why are those (short-baseline) experiments interesting? 0.07 LBNF � � 0.06 These new physics contain a short-distance (non-Standard) ⌫ µ ! ⌫ µ LBNF � e Normalized Flux 0.05 BNB � � 0.04 BNB � e 0.03 Non-Unitarity NSI Sterile Neutrino 0.02 0.01 ⇠ sin 2 2 ✓ µe P NU ⇠ | ↵ 21 | 2 P NSI ⇠ | ✏ d eµ + ✏ s eµ | 2 P 3+1 µe 0.00 µe µe 250 200 ��� / �� e 150 100 Thus, N e ⇠ � e + P NEW � µ 50 µe 0 0 1 2 3 4 5 Energy [ GeV ] 9 / 24
We can put better constraints to new physics! Why are those (short-baseline) experiments interesting? 0.07 LBNF � � 0.06 These new physics contain a short-distance (non-Standard) ⌫ µ ! ⌫ µ LBNF � e Normalized Flux 0.05 BNB � � 0.04 BNB � e 0.03 Non-Unitarity NSI Sterile Neutrino 0.02 0.01 ⇠ sin 2 2 ✓ µe P NU ⇠ | ↵ 21 | 2 P NSI ⇠ | ✏ d eµ + ✏ s eµ | 2 P 3+1 µe 0.00 µe µe 250 200 ��� / �� e 150 O (10 2 ) 100 Thus, N e ⇠ � e + P NEW � µ 50 µe 0 0 1 2 3 4 5 Energy [ GeV ] 9 / 24
We can put better constrain to new physics! We simulated: 10 / 24
We can put better constrain to new physics! We simulated: SBNE = SBND + µ BooNE + ICARUS 10 / 24
We can put better constrain to new physics! We simulated: SBNE = SBND + µ BooNE + ICARUS LBNF beam with: protoDUNE and ICARUS as ND 10 / 24
We can put better constrain to new physics! 10 - 6 10 - 5 10 - 4 10 - 3 15 SBNE ICARUS at LBNF 10 �� 2 protoDUNE - SP 5 0 10 - 6 10 - 5 10 - 4 10 - 3 2 or | � e � 2 d + � e � s | � 21 10 / 24
We can put better constrain to new physics! 10 - 6 10 - 5 10 - 4 10 - 3 15 SBNE ICARUS at LBNF 10 �� 2 protoDUNE - SP SBNE: | ↵ 21 | 2 < 2 ⇥ 10 � 4 5 0 10 - 6 10 - 5 10 - 4 10 - 3 2 or | � e � 2 d + � e � s | � 21 10 / 24
We can put better constrain to new physics! 10 - 6 10 - 5 10 - 4 10 - 3 15 SBNE ICARUS at LBNF 10 �� 2 protoDUNE - SP LBNF: SBNE: | ↵ 21 | 2 < 2 . 5 ⇥ 10 � 5 | ↵ 21 | 2 < 2 ⇥ 10 � 4 5 0 10 - 6 10 - 5 10 - 4 10 - 3 2 or | � e � 2 d + � e � s | � 21 10 / 24
We can put better constrain to new physics! 10 - 6 10 - 5 10 - 4 10 - 3 15 Current: SBNE | ↵ 21 | 2 < 7 ⇥ 10 � 4 ICARUS at LBNF 10 �� 2 protoDUNE - SP LBNF: SBNE: | ↵ 21 | 2 < 2 . 5 ⇥ 10 � 5 | ↵ 21 | 2 < 2 ⇥ 10 � 4 5 0 10 - 6 10 - 5 10 - 4 10 - 3 2 or | � e � 2 d + � e � s | � 21 10 / 24
We can put better constrain to new physics! 10 - 6 10 - 5 10 - 4 10 - 3 15 SBNE ICARUS at LBNF 10 �� 2 protoDUNE - SP LBNF: | ↵ 21 | 2 < 2 . 5 ⇥ 10 � 5 5 0 10 - 6 10 - 5 10 - 4 10 - 3 2 or | � e � 2 d + � e � s | � 21 Can we really reach this level? 10 / 24
We need to know the expected flux precisely! This New Physics changes ⌫ spectrum, N ν e / � ν e + | ↵ 21 | 2 � ν µ and P ( ⌫ µ ! ⌫ e ) = 1 � sin 2 2 ✓ µe sin ∆ m 41 L 4 E 11 / 24
We need to know the expected flux precisely! This New Physics changes ⌫ spectrum, N ν e / � ν e + | ↵ 21 | 2 � ν µ and P ( ⌫ µ ! ⌫ e ) = 1 � sin 2 2 ✓ µe sin ∆ m 41 L 4 E Traditionally, neutrino oscillation experiments uses (at least) two detectors: 11 / 24
We need to know the expected flux precisely! This New Physics changes ⌫ spectrum, N ν e / � ν e + | ↵ 21 | 2 � ν µ and P ( ⌫ µ ! ⌫ e ) = 1 � sin 2 2 ✓ µe sin ∆ m 41 L 4 E Traditionally, neutrino oscillation experiments uses (at least) two detectors: Source ⌫ 11 / 24
We need to know the expected flux precisely! This New Physics changes ⌫ spectrum, N ν e / � ν e + | ↵ 21 | 2 � ν µ and P ( ⌫ µ ! ⌫ e ) = 1 � sin 2 2 ✓ µe sin ∆ m 41 L 4 E Traditionally, neutrino oscillation experiments uses (at least) two detectors: Source ⌫ Near Detector 11 / 24
We need to know the expected flux precisely! This New Physics changes ⌫ spectrum, N ν e / � ν e + | ↵ 21 | 2 � ν µ and P ( ⌫ µ ! ⌫ e ) = 1 � sin 2 2 ✓ µe sin ∆ m 41 L 4 E Traditionally, neutrino oscillation experiments uses (at least) two detectors: Source ⌫ Near Detector Far Detector 11 / 24
We need to know the expected flux precisely! This New Physics changes ⌫ spectrum, N ν e / � ν e + | ↵ 21 | 2 � ν µ and P ( ⌫ µ ! ⌫ e ) = 1 � sin 2 2 ✓ µe sin ∆ m 41 L 4 E Traditionally, neutrino oscillation experiments uses (at least) two detectors: Source ⌫ Near Detector Far Detector 11 / 24
We need to know the expected flux precisely! This New Physics changes ⌫ spectrum, N ν e / � ν e + | ↵ 21 | 2 � ν µ and P ( ⌫ µ ! ⌫ e ) = 1 � sin 2 2 ✓ µe sin ∆ m 41 L 4 E Traditionally, neutrino oscillation experiments uses (at least) two detectors: Source ⌫ Near Detector Far Detector Extrapolation 11 / 24
Knowing the flux will be challanging! But we want to measure zero distance e ff ects! 12 / 24
Knowing the flux will be challanging! But we want to measure zero distance e ff ects! We need to rely on other types of measurements (see hep-ex/arxiv:1201.3025) 12 / 24
Knowing the flux will be challanging! But we want to measure zero distance e ff ects! We need to rely on other types of measurements (see hep-ex/arxiv:1201.3025) (1) Modeling the distribution of ⇡ and K produced by the proton beam 12 / 24
Knowing the flux will be challanging! But we want to measure zero distance e ff ects! We need to rely on other types of measurements (see hep-ex/arxiv:1201.3025) (1) Modeling the distribution of ⇡ and K produced by the proton beam (2) Measuring the muon flux in the decay pipeline and relate it to the ⌫ flux 12 / 24
Knowing the flux will be challanging! But we want to measure zero distance e ff ects! We need to rely on other types of measurements (see hep-ex/arxiv:1201.3025) (1) Modeling the distribution of ⇡ and K produced by the proton beam (2) Measuring the muon flux in the decay pipeline and relate it to the ⌫ flux (3) Measuring the low energy transfer events (low- ⌫ ) 12 / 24
Knowing the flux will be challanging! But we want to measure zero distance e ff ects! We need to rely on other types of measurements (see hep-ex/arxiv:1201.3025) (1) Modeling the distribution of ⇡ and K produced by the proton beam (2) Measuring the muon flux in the decay pipeline and relate it to the ⌫ flux May be a ff ected (3) Measuring the low energy transfer events (low- ⌫ ) by new physics 12 / 24
Knowing the flux will be challanging! But we want to measure zero distance e ff ects! We need to rely on other types of measurements (see hep-ex/arxiv:1201.3025) (1) Modeling the distribution of ⇡ and K produced by the proton beam (2) Measuring the muon flux in the decay pipeline and relate it to the ⌫ flux May be a ff ected (3) Measuring the low energy transfer events (low- ⌫ ) by new physics Need to know production di ff erential cross section and the horn magnetic field 12 / 24
Knowing the flux will be challanging! But we want to measure zero distance e ff ects! We need to rely on other types of measurements (see hep-ex/arxiv:1201.3025) (1) Modeling the distribution of ⇡ and K produced by the proton beam (2) Measuring the muon flux in the decay pipeline and relate it to the ⌫ flux May be a ff ected (3) Measuring the low energy transfer events (low- ⌫ ) by new physics Need to understand detector very well and is hard to measure E dependency Need to know production di ff erential cross section and the horn magnetic field 12 / 24
We parametrized our lack of knowledge Let’s parametrize our lack of knowledge to see its impact: # of Events [a.u.] E ν [a.u.] 13 / 24
We parametrized our lack of knowledge Let’s parametrize our lack of knowledge to see its impact: Normalization: N 0 (1 + a ) # of Events [a.u.] E ν [a.u.] 13 / 24
We parametrized our lack of knowledge Let’s parametrize our lack of knowledge to see its impact: Normalization: N 0 (1 + a ) a = 0 # of Events [a.u.] E ν [a.u.] 13 / 24
We parametrized our lack of knowledge Let’s parametrize our lack of knowledge to see its impact: Normalization: N 0 (1 + a ) a = 0 a = � 5% # of Events [a.u.] E ν [a.u.] 13 / 24
We parametrized our lack of knowledge Let’s parametrize our lack of knowledge to see its impact: Normalization: N 0 (1 + a ) a = 0 a = � 5% # of Events [a.u.] a = 5% E ν [a.u.] 13 / 24
Shape uncertanty can spoil the sensitivity! Let’s parametrize our lack of knowledge to see its impact: # of Events [a.u.] E ν [a.u.] 14 / 24
Shape uncertanty can spoil the sensitivity! Let’s parametrize our lack of knowledge to see its impact: Shape: N 0 i (1 + a i ) , bin i = 1 , 2 , ... # of Events [a.u.] E ν [a.u.] 14 / 24
Shape uncertanty can spoil the sensitivity! Let’s parametrize our lack of knowledge to see its impact: Shape: N 0 i (1 + a i ) , bin i = 1 , 2 , ... a i = 0 # of Events [a.u.] E ν [a.u.] 14 / 24
Shape uncertanty can spoil the sensitivity! Let’s parametrize our lack of knowledge to see its impact: Shape: N 0 i (1 + a i ) , bin i = 1 , 2 , ... a i = 0 a i 6 = 0 # of Events [a.u.] E ν [a.u.] 14 / 24
Shape uncertanty can spoil the sensitivity! Let’s parametrize our lack of knowledge to see its impact: Shape: N 0 i (1 + a i ) , bin i = 1 , 2 , ... ! ! a i = 0 n r e t a i 6 = 0 t a # of Events [a.u.] p n o i t a l l i c s o y n a e s o l y a m e W E ν [a.u.] 14 / 24
σ s the real parameter here A bit of math.... 15 / 24
σ s the real parameter here A bit of math.... ! 2 N bin N exp � (1 � b � b i ) N bg � (1 � a � a i ) N th � 2 = X i i i + � 2 SYS , N exp p i i =1 15 / 24
σ s the real parameter here A bit of math.... ! 2 N bin N exp � (1 � b � b i ) N bg � (1 � a � a i ) N th � 2 = X i i i + � 2 SYS , N exp p i i =1 15 / 24
σ s the real parameter here A bit of math.... ! 2 N bin N exp � (1 � b � b i ) N bg � (1 � a � a i ) N th � 2 = X i i i + � 2 SYS , N exp p i i =1 15 / 24
σ s the real parameter here A bit of math.... ! 2 N bin N exp � (1 � b � b i ) N bg � (1 � a � a i ) N th � 2 = X i i i + � 2 SYS , N exp p i i =1 ✓ a ✓ b ✓ a i ✓ b i N bin ◆ 2 ◆ 2 ◆ 2 ◆ 2 � 2 X SYS = + + + , � a � b � sa � sb i =1 15 / 24
σ s the real parameter here A bit of math.... ! 2 N bin N exp � (1 � b � b i ) N bg � (1 � a � a i ) N th � 2 = X i i i + � 2 SYS , N exp p i i =1 ✓ a ✓ b ✓ a i ✓ b i N bin ◆ 2 ◆ 2 ◆ 2 ◆ 2 � 2 X SYS = + + + , � a � b � sa � sb i =1 We minimize over a, b, a i , b i 15 / 24
σ s the real parameter here A bit of math.... ! 2 N bin N exp � (1 � b � b i ) N bg � (1 � a � a i ) N th � 2 = X i i i + � 2 SYS , N exp p i i =1 ✓ a ✓ b ✓ a i ✓ b i N bin ◆ 2 ◆ 2 ◆ 2 ◆ 2 � 2 X SYS = + + + , � a � b � sa � sb i =1 We minimize over a, b, a i , b i � sa = � sb = � s Spectrum error 15 / 24
σ s changes only the usual uncertanty Usual histogram comparisson (Pearson’s � 2 ) gives 16 / 24
σ s changes only the usual uncertanty Usual histogram comparisson (Pearson’s � 2 ) gives 2 0 1 @ N data � N theo � 2 = X i i A q N data i i 16 / 24
σ s changes only the usual uncertanty Usual histogram comparisson (Pearson’s � 2 ) gives 2 0 1 @ N data � N theo � 2 = X i i A q N data Statistical Uncertainty i i 16 / 24
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