Neutrino Oscillations and Dark Matter Searches with KM3NeT

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presentation by

Adriana Bariego Quintana Santiago Paz Castro

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Santiago Paz Castro

with the supervision of

Víctor Carretero

Neutrino Oscillation and Mass Hierarchy

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- We can’t see neutrinos.

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KM3NeT and Cherenkov Radiation

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- We can’t see neutrinos directly, but we are good at seeing light

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KM3NeT and Cherenkov Radiation

γ

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- We can’t see neutrinos, but we can see light coming from muons, electrons…

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Cherenkov Radiation

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- We can also distinguish neutrino flavors*

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- We can also distinguish neutrino flavors*

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KM3NeT and Cherenkov Radiation

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What do we search for?

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Neutrinos in a nutshell

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- Parameters for Neutrino Oscillation (θ’s, Δm², δ_CP)

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PMNS MATRIX (Pontecorvo, Maki, Nakagawa, Sakata)

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- Parameters for Neutrino Oscillation (θ’s, Δm², δ)

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1. Δm² ₃₁

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PMNS Matrix Parameters

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2. θ ₂₃

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2. θ ₂₃ = (49.26°, 41.21°, 51.3°)

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PMNS Matrix Parameters

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3. δ

_CP

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3. δ

_CP

effects? CP violation T violation CPT conservation

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- Mass Hierarchy, is Δm²₃₁ positive?

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- Mass Hierarchy, is Δm²₃₁ positive?

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Mass Hierarchy

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Mass Hierarchy

So far,

so good

but…

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Mass Hierarchy on track events

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Mass Hierarchy on track events 𝜈

_e

:𝜈

_μ ~ 1:2

In the atmosphere:

…

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~ 0.7

10^-38cm²/GeV

~ 0.35

10^-38cm²/GeV

And for Matter Effects…

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Normal Hierarchy

Inverted Hierarchy

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Mass Hierarchy on track events

NH - IH

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More to find…

- Mass hierarchy? θ₂₃ octant?

- Is CP conserved?

- Beyond SM theories? Sterile neutrinos? NSI?

- Neutrino Decay? Decoherence?

- Are neutrinos Dirac or Majorana?

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Summary

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More to find…

- Mass hierarchy? θ₂₃ octant?

- Is CP conserved?

- Beyond SM theories? Sterile neutrinos? NSI?

- Neutrino Decay? Decoherence?

- Are neutrinos Dirac or Majorana?

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Summary

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Adriana Bariego Quintana

with the supervision of

Sara Rebecca Gozzini Adrian Saina

Search for Dark Matter Signatures with KM3NeT

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- Observational evidences for a new component

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DARK MATTER? THE MISSING COMPONENT?

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DARK MATTER? THE MISSING COMPONENT?

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Galactic scales Galaxy cluster scales

Cosmological scales

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Galactic scales

[Vera Rubin et al, 1978]

- Prediction

- Observation

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DARK MATTER? THE MISSING COMPONENT?

Galactic scales

Dark Haloes

Dark Sub-Haloes

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Galaxy cluster scales

DM filaments peculiar motion

of clusters

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- Observational evidences for a new component - All evidence solely based on gravitational effects

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DARK MATTER? THE MISSING COMPONENT?

Proposed solutions:

1. Dark Matter

2. MOND (MOdified Newtonian Dynamics)

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- Observational evidences for a new component - All evidence solely based on gravitational effects - DM properties

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DARK MATTER? THE MISSING COMPONENT?

- Non-relativistic / cold - Non-baryonic

- Neutral

- Collisionless (weakly interacting)

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- DM candidates

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- DM candidates

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DARK MATTER? THE MISSING COMPONENT?

- DM candidates

WIMPs (Weakly Interacting Massive Particles)

- GeV-TeV - neutral - cold

- weakly coupled to SM

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- DM candidates

WIMPs (Weakly Interacting Massive Particles)

- GeV-TeV - neutral - cold

- weakly coupled to SM

WIMP

SM

SM SM

SM

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- DM interacts gravitationally space-time curvature

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DM IN KM3NeT

WIMP

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- DM interacts gravitationally — but KM3NeT:

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DM IN KM3NeT

WIMP

Measures the signal that neutrinos leave!!

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DM IN KM3NeT

WIMP

…

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DM IN KM3NeT

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DM IN KM3NeT

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TO FIND A DM SIGNAL

converts into muons

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TO FIND A DM SIGNAL

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TO FIND A DM SIGNAL

spectrum

flux flux effective

area

time between events

# events annihilation rate

total number of counts

shape of interaction

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TO FIND A DM SIGNAL

spectrum flux

annihilation rate

what about this?

1. Distribution on parameters 2. Event selection

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TO FIND A DM SIGNAL

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TO FIND A DM SIGNAL

spectrum flux

annihilation rate

what about this?

1. Distribution on parameters 2. Event selection

3. Use the distribution of parameters to create fake data

4. Likelihood maximisation: signal or background?

5. Flux computation

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TO FIND A DM SIGNAL

spectrum

flux flux effective

area

time between events

# events annihilation rate

shape of interaction

COMPARE

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LAST SLIDE, THANK YOU

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ADDITIONAL SLIDES.

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Cosmological scales

CMB

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DM IN KM3NeT

Z

neutral current

W

charged current Z

neutral current

the only we can measure

- Standard Model vertices:

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- Monte Carlo simulations of the events

- Reconstruction of these Monte Carlo events

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TO FIND A DM SIGNAL

True Events

Reconstructed Events

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TO FIND A DM SIGNAL

converts into muons

N

Monte Carlo Simulation events in KM3NeT

Flux of the interaction from some database (WIMPSim)

- Atmospheric spectrum

- Dark Matter Spectrum