Overview Motivation Link between Cosmic Ray and Neutrino Physics - - PowerPoint PPT Presentation

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Overview Motivation Link between Cosmic Ray and Neutrino Physics - - PowerPoint PPT Presentation

Sep 04, 2023 313 likes •977 views

30 Years of High-Energy Neutrino Astronomy: What have we achieved? A brief Review of the Past and some Thoughts for the Future. Peter K. F. Grieder University of Bern Switzerland Vulcano Workshop 2010 May 24-29

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Peter K. F. Grieder

University of Bern Switzerland

Vulcano Workshop 2010 May 24-29 Frontier Objects in Astrophysics and Particle Physics

30 Years of High-Energy Neutrino Astronomy:

What have we achieved?

A brief Review of the Past and some Thoughts for the Future.

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Overview

  • Motivation
  • Link between Cosmic Ray and Neutrino Physics
  • Summary of Historic Events, Relevant Years
  • Neutrino Detection: Methods and Telescopes
  • Present Results: Predictions and Measurements
  • Experimental Aspects, Sites, Problems of Past

and Present in View of KM3

  • Comments on Supplementary Auxiliary Detector

Systems, Fall-back Projects

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Why Neutrino Astronomy

Find the Sources of UHE Cosmic Rays Astrophysical, Cosmological, Particle Physics Aspects Today’s astronomy is based on EM radiation: Optical Radio Infrared X-Rays Gamma Rays

It yields a rich but single-sided picture of the Universe

Much remains obscure, invisible. New alternative approaches, techniques are required. Neutrino astronomy is such an approach. It opens a new non-EM window into the Universe.

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A Specific Problem Presents the UHE Primary Cosmic Radiation

(Spectral uncertainties at UHE, GZK cutoff?)

Compressed Double-Logarithmic Spectrum

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Primary Cosmic Ray Spectrum

(Akeno, AGASA, EAS-TOP and Yakutsk data excluded)

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Questions concerning UHE CR

  • Where ends the primary spectrum *
  • Nature and composition of primaries *
  • Is there a GZK cutoff *
  • Where are the sources
  • What is the nature of the sources, mechanisms
  • Classical accelerators, cutoffs
  • Top-down hypothesis, mechanisms

* Answers are in sight

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How to Locate UHE CR Sources: Methods and Techniques

  • Anisotropy studies of arrival direction of

UHE CR air showers

Hadron astronomy (magnetic fields, GZK cutoff)

Gamma-ray astronomy (CMBR)

  • Search for, locate Cosmic Powerhouses

Gamma-ray astronomy

Neutrino astronomy

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Likely / Suspected Sources of UHE-CR, Neutrinos

  • Point Sources:
  • Supernova Remnants (E ≤ 10**16 eV)
  • AGNs
  • Blazars
  • Gamma Ray Bursters
  • Diffuse Sources:
  • GZK Neutrinos
  • Topological Defects, Supermassive Particles
  • Z-Bursts
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Important Developments, Landmarks

(Back to the Roots: How it all Began)

  • The energy crisis of the late 1920s (energy conservation in beta

decay) prompted Pauli’s neutrino hypothesis as solution (1930).

  • Reines & Cowan’s experiment verified existence of neutrino (1956),

(Reines, Nobel Price 1995).

  • Discovery of >10**18 eV showers by Clark et al. (1957) raises

questions concerning nature and origin of primaries (extragalactic?).

  • Frank, Tamm and Cherenkov (1937/1938) get Nobel Price (1958),

triggers development of Cherenkov detectors (Ginzburg, 1941/2003)

  • Cocconi (ICRC Moscow, 1959) proposed search for UHE gamma

ray showers to locate CR sources (CMBR was not yet established).

  • Markov (Rochester Conf., 1960). proposed UHE neutrino detection

in ocean, using Cherenkov light to locate CR sources.

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Developments, Landmarks (cont.)

  • Askaryan developed acoustic shock (1957) and Cherenkov radio

theory (1961).

  • Lederman et al. (1962) prove existence of electron and muon

neutrino (Nobel Price 1988).

  • Penzias and Wilson (1964) discover CMBR (Nobel Prive 1978).
  • Greisen, Zatsepin and Kuzmin (1966) predict GZK Cutoff.
  • Perl et al. (1975) discover tau lepton (Nobel Price 1995), tau

neutrino awaits discovery.

  • Neutrino oscillations (Theory: Pontecorvo et al., 1957, 1967;
  • bservations ~1993, ratio of ratios) (Koshiba, Nobel Price 2002).
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Comment

The evolution of Neutrino Physics has strongly affected neutrino astronomy in general, and in particular the scientific goals, but also the experimental concepts and techniques (electron-, muon- and tau neutrinos, and neutrino oscillations).

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Neutrino Detection

Via Neutrino Reactions only

Characteristics of neutrino reactions and reaction products are neutrino flavor specific.

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Effects of Neutrino Reactions in Target

Acoustic Shock, Optical and Radio Cherenkov Emission

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Detector Requirements

Small neutrino cross sections require large target mass / volume, large detector surface / volume Suitable target / detector media are large bodies of water, ice, salt, air or rock, the Moon

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Astrophysical Neutrino Telescopes

Concepts, Detection Principles

(Site and Energy Range Specific) Type Medium Detection

Deep-water water optical Cherenkov, acoustic shock Deep-ice ice optical, radio Cherenkov, acoustic

Surface air, rock EAS particles, fluorescence, radio Balloon ice radio Cherenkov emission Satellite air, ice, fluorescence, radio Cherenkov, rock reflected optical Cherenkov light

Typical Design Concepts

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3-D DUMAND Type Water / Ice Optical Cherenkov and Acoustic Detector Arrays

AMANDA, ANTARES, Baikal, IceCube, NEMO, NESTOR, KM3

Hawaii

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Surface based Particle, Fluorescence and Radio Detectors: Auger, GLUE, LOFAR (Tokyo INS)

Young, Inclined (Horizontal) Air Shower

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Balloon based Radio Detectors

ANITA (Antarctic Impulsive Transient Antenna)

Antarctica

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Satellite based Cherenkov Radio Detectors

LORD Project (Lunar Orbiting Detector)

Horn Antennas

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Satellite based Fluorescence Detectors

JEM-EUSO Project

Observes CR and Neutrino Induced Showers

Sakaki et al., 2008

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Site, Medium and Concept Specific Problems, Advantages

Ocean: instrumentation, long-range deployment from ship, platform, (ice), remote operations, background. Detector is serviceable.

ANTARES, (Baikal), NEMO, NESTOR, KM3

Ice sheet: access, drilling (melting) of holes to site, detector is irreparable, homogeneity, background. Comparatively easy deployment.

AMANDA, IceCube

Surface: background, event identification. Easy instrumentation, access.

Auger, GLUE, LOFAR (Tokyo INS)

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Site, Medium and Concept Specific Problems, Advantages

(cont.)

Balloon: launch, radio background, short run time, difficult analysis and interpretation. Large target area, volume; high threshold energy.

ANITA

Satellite: launch, optical, radio background. Very high threshold energy, huge target volume, area.

FORTE, JEM-EUSO, LORD

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Relevant Target / Detector Medium Specific Properties, Parameters

Composition (water, ice, air, salt, rock) Density, Homogeneity (Temperature) Optical properties, parameters (scattering, attenuation, refraction) Acoustic properties (sound propagation) Electromagnetic properties, parameters (radio propagation) (dielectric constant, conductivity)

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Neutrino Fluxes: Model Predictions

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Sensitivities of different Detectors:

Anticipated and Determined Sensitivities of Different Experiments

Saltzberg (2005)

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Measured Neutrino Flux Limits:

Results from Different Experiments

Gorham et al. 2004 Barwick et al., 2006

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Deep-Water Cherenkov Arrays:

Site Relevant Properties

Geographic location Depth Sky exposure Water properties Environment Background

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Muons Neutrinos

Detector Site

Relevant Parameters, Properties Geographic Location

Sky Visibility, Background

DUMAND

Near Equator

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Depth (Altitude):

Sky Visibility, Background: an Example

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Skymap of Detected Neutrinos by AMANDA II at South Pole

(can only observe northern hemisphere)

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Sea / Ocean Parameters

NESTOR Site DUMAND Site

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Sea / Ocean Parameters (cont.)

NESTOR Site DUMAND Site

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Background, Environmental Considerations:

(Site Specific)

  • ptical

cosmic rays bioluminescence, chemo-luminescence natural radioactivity, 40K acoustic noise (radio noise) bio-fowling (stops at > 800 m b.s.l.) sedimentation (e.g., Sahara sand, Rivers) sea, ocean currents lightning storms

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Muon Depth-Intensity Relation

In Standard Rock In Water

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Muon Depth-Intensity Relation (cont.)

Sea water NESTOR site

4108 m 3697 m Depth 3338 m ANTARES NESTOR NEMO, KM3

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Bioluminescence, Hawaii Site

Depth 3000 m (tethered)

Calibration Pulses

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Bioluminescence (cont.)

Ocean currents and turbulence can cause stimulated bioluminescence

  • f bacteria.

Effect is geographic location and depth dependent. Fish, animals are irrelevant sources

  • f bioluminescence.

Nearby rivers, cities increase effect.

C dark noise, 3°C F bottom tethered (100 m a.g.) 1500 m 2500 m 3500 m 4500 m

Channel Number 1 M 100 cps 100

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Bioluminescence, Hawaii Site (cont.)

4300 m 3000 m

4300 m at start ascent

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DUMAND Site

Optical Background v/s Depth in Pacific near Hawaii

Descent, Ascent ~40 – 80 cm/s (facing down)

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Deep-Water Cherenkov Arrays:

Important Elements, Topics

  • Optical (Acoustic) Sensor Modules, Clusters.
  • Array Design, Structure, Layout (mechanical).
  • Data Acquisition, Transmission and Processing Strategy, associated

Electronics.

  • Event Reconstruction and Analysis.
  • System and Event Simulation.
  • Array and Environmental Monitoring System, Housekeeping.
  • Deployment and Installation.
  • Support and Maintenance.
  • Auxiliary Systems, (Shallow Muon Array etc.)
  • Fall-Back Projects.
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Optical Sensor Modules

Benthos glass pressure housing (17”) for optical detector module.

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DUMAND Optical Detector Module

DUMAND optical detector module showing 17 “ Benthos glass pressure housing, 15” Hamamatsu PMT with magnetic shield (grid) and electronics (HVPS, control, monitoring, data and command handling system, 3-way communication).

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Optical Module Options for KM3

Pressure housing holds many small PMT’s (left) or two mid-size (right). OM Cluster below.

Module orientation is relevant

Module Cluster Twins

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Proposed Array Structures

! Must be Deployed !

KM3NeT NESTOR

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120 m 4000 m

NESTOR Tower

Folded

Tower Separation Tower Height 500 m

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Ocean Deployment Techniques

From Standard Ship (De Steiger) in Pacific, no Fun

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SSP Kaimalino (USN) at Sea Semi-Submersible Platform with DPS

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SPS Deployment from Kaimalino

Optical, Calibration Modules String Controller

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Work on Deck of the Kaimalino

  • P. Grieder and G. Wilkins (1987)
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String Deployment/Recovery from SSP Kaimalino (Diver’s View, ~30 m, Video)

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SSP Kaimalino (Front View)

at Snug Harbor, Honolulu, Hawaii

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SSP Kaimalino

in Drydock at Kaneohe, Hawaii

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SSC Kaio (Japan)

Semi-Submersible Catamaran

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Oceanographic Research Vessel

Thomas G. Thompson (D.P.S.)

Helicopter picture by P. Grieder during string deployment

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Future Deployment Platform

Stable, Floating, Semi-Submersible (D.P.S.)

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Submarines and Robots

Sea Cliff (Pilot, Navigator, Observer, >5000m b.s.l. )

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Submarines and Robots (cont.)

Remotely Operated Vehicle (ROV)

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Detector Modules and Deployment Schemes

Old Ideas from the History Book Revisited Simple configurations simplify deployment

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Phase Shifting Light Collector-OM Combinations (from History Book)

Phase Shifting Light Collector Fan Sea Urchin Design Pressure Envelope 3 m Spines WS Sensor Tube

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Deployment Schemes, String Packing

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On-Shore Fly’s Eye

Partial Fly’s Eye

  • n Puu Hualalai,

Big Island ,Hawaii 2700 m a.s.l.

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Shallow, Anchored Muon Array

10 GeV Muon Array

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Thank you for your attention

Article on junction box, 400 m string & 30 km cable deployment on WEB: http://www.itp.unibe.ch/astrocosmo