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Transcript of June 17, 2002Beaune 2002, Katsushi Arisaka 1 University of California, Los Angeles Department of...
Beaune 2002, Katsushi Arisaka 1June 17, 2002
University of California, Los Angeles
Department of Physics and Astronomy
Katsushi Arisaka
Trends, Needs and Dreams in Astro-
Physics
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
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
Beaune 2002, Katsushi Arisaka 4June 17, 2002
Hubble Deep Field
~100 Billion GalaxiesRed shift up to 10
Beaune 2002, Katsushi Arisaka 5June 17, 2002
Evolution of the Early Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Radius of Universe (cm)
Golf Ball
People
Mountain
Earth
1 A.U.
1 Light Year
Galaxy
1
105
1010
1015
1020
1025
1028
10-33 Big Bang!
Now
Beaune 2002, Katsushi Arisaka 6June 17, 2002
Tools to explore the Early Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Accelerator
Telescope
Beaune 2002, Katsushi Arisaka 7June 17, 2002
Unification of Fundamental Forces
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
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
Beaune 2002, Katsushi Arisaka 8June 17, 2002
Hubble Deep FieldPhysicists’ View of Early Universe
Beaune 2002, Katsushi Arisaka 9June 17, 2002
Symmetry Breaking
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Simple
SymmetryBreak Down
Complex
Beaune 2002, Katsushi Arisaka 10June 17, 2002
Relics from the Earliest Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Gravitational Wave
CMB
Neutralino(Cold Dark Matter)
Relic Neutrino(Hot Dark Matter)
GUT Particle
Planck
EW
Now
GUT
Big Bang
Beaune 2002, Katsushi Arisaka 11June 17, 2002
CMB : Matter-Radiation Decoupling
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Planck
EW
Now
GUT
Matter-RadiationDecoupling CMB
Time = 300,000 years
Temperature = 3,000 oK
Energy = 0.3 eV
Z = 1,100
Beaune 2002, Katsushi Arisaka 12June 17, 2002
CMB Anisotropy by COBE DMR
Beaune 2002, Katsushi Arisaka 13June 17, 2002
CMB Anisotropy by Boomerang
Beaune 2002, Katsushi Arisaka 14June 17, 2002
Recent Results of CMB Anisotropy
Beaune 2002, Katsushi Arisaka 15June 17, 2002
The Accelerating Universe
Beaune 2002, Katsushi Arisaka 16June 17, 2002
Density of Our Universe
Matter
Universe is Flat. Inflation
70% is Dark Energy. Accelerating
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
Beaune 2002, Katsushi Arisaka 18June 17, 2002
Relics from the Earliest Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Gravitational Wave
Neutralino(Cold Dark Matter)
Relic Neutrino(Hot Dark Matter)
GUT Particle
CMB
Dark Energy
Planck
EW
Now
GUT
Big Bang
Beaune 2002, Katsushi Arisaka 19June 17, 2002
The Extreme Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Planck
EW
Now
GUT
Big Bang
Active Galactic Nuclei
Gamma Ray Burst
Supernova Neutron Star Black Holes
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
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
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
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.
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
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
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”
Beaune 2002, Katsushi Arisaka 27June 17, 2002
SNAP – Dark Energy Sensitivity
Beaune 2002, Katsushi Arisaka 28June 17, 2002
Deep Sky Survey by Telescopes
HSTKeck
SDSS
SNAP
NGST
LSST
Larger MirrorLarger FOV
Space
Ground
Beaune 2002, Katsushi Arisaka 29June 17, 2002
The Extreme Universe
Pulsar
GRB
AGN
SNR
Radio Galaxy
Beaune 2002, Katsushi Arisaka 30June 17, 2002
GLAST - Gamma Ray Sky Survey
CsI + Photo Diode
Si Strip
Beaune 2002, Katsushi Arisaka 31June 17, 2002
Gamma ray Telescopes
80 m
VERITAS HESS
• 10m Diameter• ~500PMT/Camera• 4-7 Telescopes
Beaune 2002, Katsushi Arisaka 32June 17, 2002
MAGIC under Construction
• 17m mirror• 3.6o FOV• 600 PMTs• Upgrade to GaAsP HAPD
Beaune 2002, Katsushi Arisaka 33June 17, 2002
-ray Wide-FOV Telescope
• >3m diameter• >30o FOV• Mega pixel
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
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
Beaune 2002, Katsushi Arisaka 36June 17, 2002
Tools to explore the Early Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Accelerator
Telescope
UHE Cosmic Rays
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?
Beaune 2002, Katsushi Arisaka 38June 17, 2002
#S
#S
S
Pierre-Auger Observatory
Southern Augerin Argentina
N
Northern Augerin Utah
50km
Beaune 2002, Katsushi Arisaka 39June 17, 2002
Surface Detector and the Andes
1,600 Water Tanks x 3 PMTs = 4,800 of 9” PMTs
Beaune 2002, Katsushi Arisaka 40June 17, 2002
EUSO on International Space Station
EUSO
Beaune 2002, Katsushi Arisaka 41June 17, 2002
Night Sky
Beaune 2002, Katsushi Arisaka 42June 17, 2002
EUSO vs. Pierre-Auger
EUSO
Pierre-Auger
~400km
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
Beaune 2002, Katsushi Arisaka 44June 17, 2002
OWL Stereo View from Space
~1,000km
~1,000km
Beaune 2002, Katsushi Arisaka 45June 17, 2002
AMS - Anti-Matter Search
• RICH uses Multi-anode PMT• Hamamatsu R7600-M16• 14k Pixel
Beaune 2002, Katsushi Arisaka 46June 17, 2002
AMS on International Space Station
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
Beaune 2002, Katsushi Arisaka 48June 17, 2002
Super-Kamiokande
• 11,200 of 20” PMTs• Expected to resume end of this year with 50% PMTs
Beaune 2002, Katsushi Arisaka 49June 17, 2002
Future: Hyper-K/UNO
~200k of 20” PMTs
Beaune 2002, Katsushi Arisaka 50June 17, 2002
NESTOR and ANTARES
NESTOR
ANTARES
Beaune 2002, Katsushi Arisaka 51June 17, 2002
AMANDA
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
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
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
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
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!
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!
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
Beaune 2002, Katsushi Arisaka 59June 17, 2002
DEP Hybrid Photodiode (HPD)
• Baseline design for LHC-b RICH• 8cm diameter• 61 Pixel, (5mm view)
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 )
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
Beaune 2002, Katsushi Arisaka 62June 17, 2002
Hamamatsu Flat Panel PMT
64 Pixels
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
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
Beaune 2002, Katsushi Arisaka 65June 17, 2002
Semiconductor Photo-cathodeby HamamatsuInGaN
Beaune 2002, Katsushi Arisaka 66June 17, 2002
Silicon Photomultiplier
Gain~106 DQE~10%ENF=1.0
by P. Buzhan, B. Dolgoshein et. al.
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
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
Beaune 2002, Katsushi Arisaka 69June 17, 2002
Crab Pulsar observed by TES
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!
Beaune 2002, Katsushi Arisaka 71June 17, 2002
Dream Team for Astro-Physics
CCD: ~10m � 1G pixelsSTJ: ~20m � 1M pixelsHAPD: ~1mm � 1K pixels
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
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
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!
Beaune 2002, Katsushi Arisaka 75June 17, 2002
Can “your photo-detector” see the dark side of this picture?