June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of...

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June 17, 2002 Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy [email protected] Katsushi Arisaka Trends, Needs and Dreams in Astro- Physics

Transcript of June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of...

Page 1: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 1June 17, 2002

University of California, Los Angeles

Department of Physics and Astronomy

[email protected]

Katsushi Arisaka

Trends, Needs and Dreams in Astro-

Physics

Page 2: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 2June 17, 2002

Talk Outline

Astro-Physics Cosmology High-energy Particle Astro-physics

Experiments Ongoing Future

Photo-detectors Demands New Detectors on Horizon Dream Detectors

Page 3: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 3June 17, 2002

Talk Outline

Astro-Physics Cosmology High-energy Particle Astro-physics

Experiments Ongoing Future

Photo-detectors Demands New Detectors on Horizon Dream Detectors

Page 4: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 4June 17, 2002

Hubble Deep Field

~100 Billion GalaxiesRed shift up to 10

Page 5: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 5June 17, 2002

Evolution of the Early Universe

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Radius of Universe (cm)

Golf Ball

People

Mountain

Earth

1 A.U.

1 Light Year

Galaxy

1

105

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1015

1020

1025

1028

10-33 Big Bang!

Now

Page 6: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 6June 17, 2002

Tools to explore the Early Universe

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Energy (GeV)

10-3eV

Accelerator

Telescope

Page 7: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 7June 17, 2002

Unification of Fundamental Forces

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Planck

EW

Now

GUT

Gra

vit

atio

n

Str

on

g

We

ak

Ele

ctr

om

agn

eti

c

FundamentalInteraction

Ele

ctr

o-W

ea

k

GU

T

Page 8: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 8June 17, 2002

Hubble Deep FieldPhysicists’ View of Early Universe

Page 9: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 9June 17, 2002

Symmetry Breaking

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Energy (GeV)

10-3eV

Simple

SymmetryBreak Down

Complex

Page 10: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 10June 17, 2002

Relics from the Earliest Universe

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Energy (GeV)

10-3eV

Gravitational Wave

CMB

Neutralino(Cold Dark Matter)

Relic Neutrino(Hot Dark Matter)

GUT Particle

Planck

EW

Now

GUT

Big Bang

Page 11: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 11June 17, 2002

CMB : Matter-Radiation Decoupling

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Planck

EW

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GUT

Matter-RadiationDecoupling CMB

Time = 300,000 years

Temperature = 3,000 oK

Energy = 0.3 eV

Z = 1,100

Page 12: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 12June 17, 2002

CMB Anisotropy by COBE DMR

Page 13: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 13June 17, 2002

CMB Anisotropy by Boomerang

Page 14: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 14June 17, 2002

Recent Results of CMB Anisotropy

Page 15: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 15June 17, 2002

The Accelerating Universe

Page 16: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 16June 17, 2002

Density of Our Universe

Matter

Universe is Flat. Inflation

70% is Dark Energy. Accelerating

Page 17: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 17June 17, 2002

Talk Outline

Astro-Physics Cosmology High-energy Particle Astro-physics

Experiments Ongoing Future

Photo-detectors Demands New Detectors on Horizon Dream Detectors

Page 18: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 18June 17, 2002

Relics from the Earliest Universe

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1eV

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10-3eV

Gravitational Wave

Neutralino(Cold Dark Matter)

Relic Neutrino(Hot Dark Matter)

GUT Particle

CMB

Dark Energy

Planck

EW

Now

GUT

Big Bang

Page 19: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 19June 17, 2002

The Extreme Universe

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Planck

EW

Now

GUT

Big Bang

Active Galactic Nuclei

Gamma Ray Burst

Supernova Neutron Star Black Holes

Page 20: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 20June 17, 2002

Messengers from the Universe

Photons• Visible, Infrared, UV • X-rays, Gamma-rays• Micro-wave, Radio

Charged Particles• Ultra High Energy Cosmic Rays• Anti-particles

Neutrinos• Solar-neutrino, Supernova• Relic Neutrino

Dark Matter Gravitons not covered

in this talk

Page 21: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 21June 17, 2002

Messengers from the Universe

Photons• Visible, Infrared, UV • X-rays, Gamma-rays• Micro-wave, Radio

Charged Particles• Ultra High Energy Cosmic Rays• Anti-particles

Neutrinos• Solar-neutrino, Supernova• Relic Neutrino

Dark Matter Gravitons

Page 22: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 22June 17, 2002

SDSS (Sloan Digital Sky Survey)

• 2.5m Diameter• 3o x 3o FOV• f/2.25• 30 x 4Mega-pixel CCD

Focal Plane

Page 23: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 23June 17, 2002

SDSS Early Data Release

Distance record-holderGoal:

500 sq. degree of the sky.

14 million objects.

Spectra for 50,000 galaxies5,000 quasars.

Page 24: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 24June 17, 2002

LSST (Large-aperture Synoptic Survey Telescope)

• 8m Diameter• 3o x 3o FOV• f/1.2, 50cm Focal plane• 1.4Giga-pixel CCD

Page 25: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 25June 17, 2002

NGST (Next Generation Space Telescope)

GSFC Design

• Mirror Diameter: ~6.5 m• FOV: 4’ x 4’• Wavelength: 0.6-28 m• Orbit: L2 point • Payload mass: ~3000 kg • Mission duration: 5-10 years

Page 26: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 26June 17, 2002

SNAP (SuperNova Acceleration Probe)

• Mirror Diameter: 2 m• FOV: 1o x 1o

• Wavelength: 0.35-1 m• IR Photometry: 10’x10’,

HgCdTd • IR Spectroscopy: 2”x2”

Page 27: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 27June 17, 2002

SNAP – Dark Energy Sensitivity

Page 28: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 28June 17, 2002

Deep Sky Survey by Telescopes

HSTKeck

SDSS

SNAP

NGST

LSST

Larger MirrorLarger FOV

Space

Ground

Page 29: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 29June 17, 2002

The Extreme Universe

Pulsar

GRB

AGN

SNR

Radio Galaxy

Page 30: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 30June 17, 2002

GLAST - Gamma Ray Sky Survey

CsI + Photo Diode

Si Strip

Page 31: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 31June 17, 2002

Gamma ray Telescopes

80 m

VERITAS HESS

• 10m Diameter• ~500PMT/Camera• 4-7 Telescopes

Page 32: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 32June 17, 2002

MAGIC under Construction

• 17m mirror• 3.6o FOV• 600 PMTs• Upgrade to GaAsP HAPD

Page 33: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 33June 17, 2002

-ray Wide-FOV Telescope

• >3m diameter• >30o FOV• Mega pixel

Page 34: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 34June 17, 2002

Messengers from the Universe

Photons• Visible, Infrared, UV • X-rays, Gamma-rays• Micro-wave, Radio

Charged Particles• Ultra High Energy Cosmic Rays• Anti-particles

Neutrinos• Solar-neutrino, Supernova• Relic Neutrino

Dark Matter Gravitons

Page 35: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 35June 17, 2002

Energy Spectrum of Cosmic Rays

• Energy Spectrum ~ E-3

• The spectrum extends beyond 1020eV

• Beyond 1020eV, Flux is only one particle per km2-century

1TeV

Page 36: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 36June 17, 2002

Tools to explore the Early Universe

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Energy (GeV)

10-3eV

Accelerator

Telescope

UHE Cosmic Rays

Page 37: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 37June 17, 2002

Nearly impossible to accelerate beyond 1020eV by nature.

Top-down Mechanism?

Protons can travel straight at E>1020eV. Charged-Particle Astronomy

Protons can not travel beyond ~50Mpc at E> 5 x 1019eV due to interaction with CMB.

ZGK Cut-off

Why is 1020eV so special?

Page 38: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 38June 17, 2002

#S

#S

S

Pierre-Auger Observatory

Southern Augerin Argentina

N

Northern Augerin Utah

50km

Page 39: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 39June 17, 2002

Surface Detector and the Andes

1,600 Water Tanks x 3 PMTs = 4,800 of 9” PMTs

Page 40: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 40June 17, 2002

EUSO on International Space Station

EUSO

Page 41: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 41June 17, 2002

Night Sky

Page 42: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 42June 17, 2002

EUSO vs. Pierre-Auger

EUSO

Pierre-Auger

~400km

Page 43: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 43June 17, 2002

EUSO Detector16:16:09

f/1.25, 7mm pixel, 2.8m EPD, Dmax < 3.75

Scale:

0.03

DJL 06-Jan-00

735.29 MM

• 2.5m Diameter• 60o FOV• f/1.25

Hamamatsu R7600-M16/64250k Pixel

Page 44: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 44June 17, 2002

OWL Stereo View from Space

~1,000km

~1,000km

Page 45: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 45June 17, 2002

AMS - Anti-Matter Search

• RICH uses Multi-anode PMT• Hamamatsu R7600-M16• 14k Pixel

Page 46: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 46June 17, 2002

AMS on International Space Station

Page 47: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 47June 17, 2002

Messengers from the Universe

Photons• Visible, Infrared, UV • X-rays, Gamma-rays• Micro-wave, Radio

Charged Particles• High Energy Cosmic Rays• Anti-particles

Neutrinos• Solar-neutrino, Supernova• Relic Neutrino

Dark Matter Gravitons

Page 48: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 48June 17, 2002

Super-Kamiokande

• 11,200 of 20” PMTs• Expected to resume end of this year with 50% PMTs

Page 49: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 49June 17, 2002

Future: Hyper-K/UNO

~200k of 20” PMTs

Page 50: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 50June 17, 2002

NESTOR and ANTARES

NESTOR

ANTARES

Page 51: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 51June 17, 2002

AMANDA

Page 52: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 52June 17, 2002

ICECUBE

1 km

AM

AN

DA

-II

10 TeV Muon Event

60 PMTs/string x 80 strings= 4,800PMTs

Page 53: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 53June 17, 2002

Detection of Cosmic Radiation

CDMS

Super-K

AMANDA

Pierre-Auger

Hyper-K

ICECUBE

EUSOOWL

Zeplin

Larger VolumeLower Threshold

Dark Matter

Neutrino

Cosmic Ray

Page 54: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 54June 17, 2002

Talk Outline

Astro-Physics Cosmology High-energy Particle Astro-physics

Experiments Ongoing Future

Photo-detectors Demands New Detectors on Horizon Dream Detectors

Page 55: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 55June 17, 2002

Photon Detector

SDSS

EUSO

VERITAS

Super-K

LSST

OWL

Wide FOV

Hyper-K

More PixelsBetter Sensitivity

CCD

PMT

Auger-FD

Auger-SD

AMS

Page 56: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 56June 17, 2002

Demands on Photon Detectors

Giga-Pixel CCD Sky Survey

Mega-Pixel (1-5mm), Photon Counting EUSO/OWL, Wide-FOV -ray Telescope

Large Area (>50cm), Photon Counting Neutrino, Proton decay

Time-resolving Imaging Transient Phenomena

Low Costs!

Page 57: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 57June 17, 2002

Demands on Photon Detectors

Giga-Pixel CCD Sky Survey

Mega-Pixel (1-5mm), Photon Counting EUSO/OWL, Wide-FOV -ray Telescope

Large Area (>50cm), Photon Counting Neutrino, Proton decay

Time-resolving Imaging Transient Phenomena

Low Costs!

Page 58: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 58June 17, 2002

New Detectors on Horizon

Vacuum Multi-Pixel HPD DEP Flat Panel PMT Hamamatsu, Burle Silicon MCP Nano-science New Photo Cathode

Solid State Silicon PMT Russia STJ ESTEC TES Stanford

Page 59: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 59June 17, 2002

DEP Hybrid Photodiode (HPD)

• Baseline design for LHC-b RICH• 8cm diameter• 61 Pixel, (5mm view)

Page 60: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 60June 17, 2002

Energy Resolution

QE as high as possible. ( > 30% ) Col as close as 100% ( > 0.9 )

ENF as close as 1.0 ( < 1.2 ) G >> ENC (~1000e-) ( >> 104 ) NBG << N ( << 1 )

Page 61: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 61June 17, 2002

Energy Resolution

No.of Photons

100 101 102 103 104 105 106 107

En

erg

y R

eso

lutio

n

0.001

0.01

0.1

1

10

Poisson Limit

Photo Diode

APDHPD

PMT

Page 62: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 62June 17, 2002

Hamamatsu Flat Panel PMT

64 Pixels

Page 63: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 63June 17, 2002

Burle Flat PMT

• 2 inch Square • Ceramic Case• Dual MCP-PMT• 4 anodes, uniformity < 2:1• Maximum Gain ~ 1 x 106

85001 Single Electron Spectrum

Charge (e)

0 5e+5 1e+6 2e+6 2e+6

Cou

nts

0

2000

4000

6000

8000

10000

2270V 2400V

by Paul Hink

Page 64: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 64June 17, 2002

Silicon MCP

By O. Siegmund, U.C. Berkeley

• ~7µm pores• >75% open area• Diamond coated

Gain

1.00E+00

1.00E+01

1.00E+02

1.00E+03

1.00E+04

1.00E+05

0 500 1000 1500 2000

Voltage (V)

Ga

in

Si 208

CVD 105-1

CVD107-5

CVD106-1

CVD120-2

CVD114-1-c

CVD122-2

CVD122-4

CVD122-4-BEO

CVD134-1

CVD134-4

CVD139-2

CVD139-4

ITT Glass MCP

CVD169-3

Glass MCP

Si MCP

Gain > 1,000

Page 65: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 65June 17, 2002

Semiconductor Photo-cathodeby HamamatsuInGaN

Page 66: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 66June 17, 2002

Silicon Photomultiplier

Gain~106 DQE~10%ENF=1.0

by P. Buzhan, B. Dolgoshein et. al.

Page 67: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 67June 17, 2002

Superconducting Tunneling Junctions (STJ)

Energy resolution

Developed by ESTEC, ESA Detect Photon by Photon:

Energy < 0.1 eV Time < 1 nsec Position < 10 m

Page 68: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 68June 17, 2002

Transition Edge Sensor (TES)

The Astrophysical Journal, 563: 221È228, 2001 December 10R. Romani ,et al.

20 x 20 m2

Page 69: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 69June 17, 2002

Crab Pulsar observed by TES

Page 70: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 70June 17, 2002

Mega-Pixel TES/STJ

Detect Photon by Photon:

Energy < 0.1 eVTime < 1 nsecPosition < 10 m

Ultimate Photon Detector!

Page 71: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 71June 17, 2002

Dream Team for Astro-Physics

CCD: ~10m � 1G pixelsSTJ: ~20m � 1M pixelsHAPD: ~1mm � 1K pixels

Page 72: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 72June 17, 2002

Multi-pixel Hybrid APD

Glass Window (1mmt)

50.5mm �

InGaN Photo Cathode

APD Array

Readout Electronics

47.6mm �

Ceramic Case

(32 x 32 = 1024 Pixel)

HV LV Optical Fiber forSignal Readout

• 1.4mm � Pixel Size, 1.5mm Pitch• 32 x 32 = 1,024 Pixels• QE ~ 50% at 350 ~ 400nm • Gain ~105

Page 73: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 73June 17, 2002

Katsushi’s Dream Telescope

Ground & Space-based 2 observatory:

•20m diameter mirror•30o FOV, f/0.8•0.1arcsec pixel size•1Tera pixels•Photon counting•1nsec time resolution•0.01eV energy resolution

Page 74: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 74June 17, 2002

Concluding Remarks

Where did we come from? Where are we going?

The answer is still hidden in the dark side of the Universe which only more advanced photo-detectors can see.

Time is now to develop dream detectors!

Page 75: June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Katsushi.

Beaune 2002, Katsushi Arisaka 75June 17, 2002

Can “your photo-detector” see the dark side of this picture?