for relic neutrino detection Rasa Muller PhD student at Nikhef, - PowerPoint PPT Presentation

November, 2018, The Netherlands KM3NeT hydrophones for relic neutrino detection Rasa Muller PhD student at Nikhef, Amsterdam Previous intern at TNO Delft Contributions Ernst-Jan Buis – Ivo van Vulpen

November, 2018, The Netherlands Km 3 KM3NeT hydrophones Ne utrino T elescope for relic neutrino detection

November, 2018, The Netherlands Microphones KM3NeT hydrophones underwater for relic neutrino detection Optical fiber Piezo

November, 2018, The Netherlands KM3NeT hydrophones for relic neutrino detection Cosmic Cosmological Neutrino neutrino Background (C 𝜉𝐶 )

I. Context/Theory II. Monte Carlo simulation III. Conclusion C 𝜉 B is closely related to CMB C 𝝃 B CMB • Cosmic microwave background • Cosmic neutrino background • Due to expansion of universe 1/3 4 • of the CMB temp: past 13.8 billion year history: 11 1.95 K 2.725 K Energy per particle 𝜈 eV - meV range R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 5

I. Context/Theory II. Monte Carlo simulation III. Conclusion Neutrino’s exist in a wide E-range U.F. Katz, Ch. Spiering 2011: High-Energy Neutrino Astrophysics: Status and Perspectives R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 6

I. Context/Theory II. Monte Carlo simulation III. Conclusion Large variety to detect neutrino’s E 𝜉 ~ 10 14 eV  nPa E 𝜉 ~ 10 21 eV  Pa Ice, Acoustics! Alternative techniques U.F. Katz, Ch. Spiering 2011: High-Energy Neutrino Astrophysics: Status and Perspectives R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 7

I. Context/Theory II. Monte Carlo simulation III. Conclusion Acoustic neutrino detection • Rapid expansion of medium after energy deposition and subsequent heating • Expansion leads to a pressure wave in water Acoustics! G.A. Askariyan, et al., 1979: Acoustic detection of high energy particle showers in warer R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 8

I. Context/Theory II. Monte Carlo simulation III. Conclusion Method to detect cosmic neutrino’s ? Acoustics! Alternative techniques U.F. Katz, Ch. Spiering 2011: High-Energy Neutrino Astrophysics: Status and Perspectives R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 9

I. Context/Theory II. Monte Carlo simulation III. Conclusion Relic neutrinos If relic 𝜉 ’s exist: Extremely high E 𝜉 ’s get absorbed at the Z-resonance by the C 𝜉 B 𝜉 𝐷𝜉𝐶 → 𝑎 0 → 𝑌 𝜉 + ҧ 2 𝑠𝑓𝑡 = 𝑛 𝑎 eV ≈ 4 ⋅ 10 21 𝐹 𝜉 2𝑛 𝜉 𝑛 𝜉 R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 10

KM3NeT hydrophone network to detect relic neutrinos How many acoustic detections EHEC 𝜉 in what E-range are required to prove the existence of relic neutrinos?

I. Context/Theory II. Monte Carlo simulation III. Conclusion Relic neutrinos 𝜉 𝐷𝜉𝐶 → 𝑎 0 → 𝑌 𝜉 + ҧ Monte Carlo simulation Redshift (z) R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 12

I. Context/Theory II. Monte Carlo simulation III. Conclusion High energy sources are required Bottom up Top down • Sources capable of extreme • High energy particles were “acceleration” “born” with these energies (galactic) (physics beyond the standard model) • z ∼ 20 • z ∼ 2 • super heavy dark matter decay • GRB / AGN R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 13

I. Context/Theory II. Monte Carlo simulation III. Conclusion Expected flux at Earth Primary Flux 1. Survival Probability P(E(1+z), z) Chance of a cosmic neutrino (injected at redshift z with energy E) to survive on its way to Earth 2. Source emissivity L(E(1+z), z) Number of neutrinos (per flavor and Energy) emitted per comoving volume R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 14

I. Context/Theory II. Monte Carlo simulation III. Conclusion Expected flux at Earth 𝑛 𝜉 𝐹 𝑠𝑓𝑡 1 + 𝑨 𝑛𝑏𝑦 Primary Flux 𝐹 𝑠𝑓𝑡 1. Survival Probability P(E(1+z), z) Source Chance of a cosmic neutrino (injected at evolution redshift z with energy E) to survive on its way to Earth 𝑜 − 𝛽 Energy spectrum 2. Source emissivity L(E(1+z), z) Number of neutrinos (per flavor and Energy) emitted per comoving volume R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 15

I. Context/Theory II. Monte Carlo simulation III. Conclusion Expected flux at Earth Primary Flux Secondary flux 1. Survival Probability P(E(1+z), z) Chance of a cosmic neutrino (injected at redshift z with energy E) to survive on its way to Earth 2. Source emissivity L(E(1+z), z) Number of neutrinos (per flavor and Energy) emitted per comoving volume R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 16

I. Context/Theory II. Monte Carlo simulation III. Conclusion Top down and Bottom up results Theoretical flux Results R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 17

I. Context/Theory II. Monte Carlo simulation III. Conclusion More optimal scenario Theoretical flux Results R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 18

I. Context/Theory II. Monte Carlo simulation III. Conclusion Observations and Conclusions • Type of source of major importance compared to Energy resolution of telescope • Significant detection of TD & BU require large sample of events • Optimal scenario factor 10 less detections required • Large source evolution enhances signal • Prove of CνB not straightforward, but once detected: wealth of information on particle, astrophysical & cosmological physics R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 19

I. Context/Theory II. Monte Carlo simulation III. Conclusion Remember: • It is a really new part of physics! • Unknown absolute flux of extremely high energetic neutrinos • So far no one dared to give exact characteristics about the possible sources • Top Down & Bottom up • All we need is time (and a nice hydrophone network) • Don’t forget the additional science … R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 20

I. Context/Theory II. Monte Carlo simulation III. Conclusion … other applications! Sea life communication Earthquake detection R.S. Muller ‘KM3NeT hydrophones for relic neutrino detection ’ November 2018 21

Thank you

Back-up Slides

Neutrino interactions

Acoustic signal

Pressure wave detection of neutrino • Bipolar pulse • 10 – 50 kHz • E 𝜉 ~ 10 14 eV  nPa • E 𝜉 ~ 10 21 eV  Pa

Assumptions • Spectral index • Quasi degenerate neutrino mass • α = 2 • 𝑛 𝜉 = 0.1 eV • Bottom up • Flat universe Density parameters ( Ω ) & hubble • z ∼ 2 constant (h) from Planck 2015 data • n = 4 ( n − α = 2 ) • Top down • 𝜉 ֞ ҧ 𝜉 • z ∼ 20 𝜉 𝑓 ֞ 𝜉 𝜈 ֞ 𝜉 𝜐 • n = 2 ( n − α = 0 )