Trends, Needs and Dreams
in Astro-Physics
Katsushi Arisaka
University of California, Los Angeles
Department of Physics and Astronomy
arisaka@physics.ucla.edu
June 17, 2002
Beaune 2002, Katsushi Arisaka
1
Talk Outline
 Astro-Physics
 Cosmology
 High-energy Particle Astro-physics
 Experiments
 Ongoing
 Future
 Photo-detectors
 Demands
 New Detectors on Horizon
 Dream Detectors
June 17, 2002
Beaune 2002, Katsushi Arisaka
2
Talk Outline
 Astro-Physics
 Cosmology
 High-energy Particle Astro-physics
 Experiments
 Ongoing
 Future
 Photo-detectors
 Demands
 New Detectors on Horizon
 Dream Detectors
June 17, 2002
Beaune 2002, Katsushi Arisaka
3
Hubble Deep Field
June 17, 2002
~100 Billion Galaxies
Red
Beaune 2002, Katsushi
Arisaka shift up to 104
Evolution of the Early Universe
Time
(sec)
Temp. Energy Radius of
(oK) (GeV)
Universe
-45
-33
10 sec
(cm) 10
18
10
30
-40
10
10
1015
10-35
10-30
1025
10-25
10-20
1012
1
Big Bang!
Golf Ball
People
105
Mountain
109
1020
1PeV
1010
Earth
10-15
10-10
1015
1TeV
1015
1GeV
10-5
1 Light Year
1010
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
1
June 17, 2002
1 A.U.
1020
Galaxy
1eV
1025
10-3eV
1028
Beaune 2002, Katsushi Arisaka
Now
5
Tools to explore the Early Universe
Time
(sec)
Temp. Energy
(oK) (GeV)
-45
10 sec
18
10
30
-40
10
10
1015
10-35
10-30
1025
10-25
10-20
1012
109
1020
1PeV
10-15
10-10
1015
1TeV
1GeV
10-5
1010
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
1
June 17, 2002
1eV
10-3eV
Accelerator
Telescope
Beaune 2002, Katsushi Arisaka
6
Unification of Fundamental Forces
1015
10-35
10-30
1025
10-25
10-20
Fundamental
Interaction
Planck
GUT
Electro-Weak
Temp. Energy
(oK) (GeV)
-45
10 sec
18
10
30
-40
10
10
GUT
Time
(sec)
1012
109
1020
1PeV
10-15
1TeV
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
June 17, 2002
1eV
10-3eV
Now
Beaune 2002, Katsushi Arisaka
Weak
1010
Strong
1GeV
10-5
1
EW
Electromagnetic
1015
Gravitation
10-10
7
Hubble
Field
Physicists’
ViewDeep
of Early
Universe
June 17, 2002
Beaune 2002, Katsushi Arisaka
8
Symmetry Breaking
Time
(sec)
Temp. Energy
(oK) (GeV)
-45
10 sec
18
10
30
-40
10
10
1015
10-35
10-30
1025
10-25
10-20
1012
109
1020
1PeV
10-15
10-10
1015
1TeV
1010
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
June 17, 2002
Symmetry
Break Down
1GeV
10-5
1
Simple
1eV
10-3eV
Complex
Beaune 2002, Katsushi Arisaka
9
Relics from the Earliest Universe
Time
(sec)
Temp. Energy
(oK) (GeV)
-45
10 sec
18
10
30
-40
10
10
1015
10-35
10-30
1025
10-25
10-20
Planck
GUT
Big Bang
Gravitational Wave
GUT Particle
1012
109
1020
1PeV
10-15
10-10
1015
1TeV
1GeV
10-5
1010
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
1
June 17, 2002
EW
Relic Neutrino
(Hot Dark Matter)
CMB
1eV
10-3eV
Neutralino
(Cold Dark Matter)
Now
Beaune 2002, Katsushi Arisaka
10
CMB : Matter-Radiation Decoupling
Time
(sec)
Temp. Energy
(oK) (GeV)
-45
10 sec
18
10
30
-40
10
10
1015
10-35
10-30
1025
10-25
10-20
Planck
GUT
1012
109
1020
1PeV
10-15
10-10
1015
1TeV
1010
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
June 17, 2002
Z = 1,100
1GeV
10-5
1
EW
1eV
10-3eV
Time = 300,000 years
Temperature = 3,000 oK
Energy = 0.3 eV
Now
Matter-Radiation
Decoupling  CMB
Beaune 2002, Katsushi Arisaka
11
CMB Anisotropy by COBE DMR
June 17, 2002
Beaune 2002, Katsushi Arisaka
12
CMB Anisotropy by Boomerang
June 17, 2002
Beaune 2002, Katsushi Arisaka
13
Recent Results of CMB Anisotropy
June 17, 2002
Beaune 2002, Katsushi Arisaka
14
The Accelerating Universe
June 17, 2002
Beaune 2002, Katsushi Arisaka
15
Density of Our Universe

 Universe
is Flat.
 Inflation
 70%
is Dark
Energy.
 Accelerating
June 17, 2002
Beaune 2002, Katsushi Arisaka
Matter
16
Talk Outline
 Astro-Physics
 Cosmology
 High-energy Particle Astro-physics
 Experiments
 Ongoing
 Future
 Photo-detectors
 Demands
 New Detectors on Horizon
 Dream Detectors
June 17, 2002
Beaune 2002, Katsushi Arisaka
17
Relics from the Earliest Universe
Time
(sec)
Temp. Energy
(oK) (GeV)
-45
10 sec
18
10
30
-40
10
10
1015
10-35
10-30
1025
10-25
10-20
Planck
GUT
Big Bang
Gravitational Wave
GUT Particle
1012
109
1020
1PeV
10-15
10-10
1015
1TeV
1GeV
10-5
1010
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
1
June 17, 2002
EW
Relic Neutrino
(Hot Dark Matter)
CMB
1eV
10-3eV
Neutralino
(Cold Dark Matter)
Now
Dark Energy
Beaune 2002, Katsushi Arisaka
18
The Extreme Universe
Time
(sec)
Temp. Energy
(oK) (GeV)
-45
10 sec
18
10
30
-40
10
10
1015
10-35
10-30
1025
10-25
10-20
Planck
Big Bang
GUT
1012
Gamma Ray Burst
109
1020
Active Galactic Nuclei
1PeV
10-15
10-10
1015
1TeV
1GeV
10-5
1010
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
1
June 17, 2002
EW
Supernova
Neutron Star
Black Holes
1eV
10-3eV
Now
Beaune 2002, Katsushi Arisaka
19
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
not covered
in this talk
 Gravitons
June 17, 2002
Beaune 2002, Katsushi Arisaka
20
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
June 17, 2002
Beaune 2002, Katsushi Arisaka
21
SDSS (Sloan Digital Sky Survey)
•2.5m Diameter
•3o x 3o FOV
• f/2.25
•30 x 4Mega-pixel CCD
Focal Plane
June 17, 2002
Beaune 2002, Katsushi Arisaka
22
SDSS Early Data Release
Distance record-holder
Goal:
500 sq. degree
of the sky.
14 million
objects.
Spectra for
50,000 galaxies
5,000 quasars.
June 17, 2002
Beaune 2002, Katsushi Arisaka
23
LSST (Large-aperture Synoptic Survey
Telescope)
•8m Diameter
•3o x 3o FOV
•f/1.2, 50cm Focal plane
•1.4Giga-pixel CCD
June 17, 2002
Beaune 2002, Katsushi Arisaka
24
NGST (Next Generation Space
Telescope)
•Mirror Diameter:
•FOV:
•Wavelength:
•Orbit:
•Payload mass:
•Mission duration:
~6.5 m
4’ x 4’
0.6-28 m
L2 point
~3000 kg
5-10 years
GSFC Design
June 17, 2002
Beaune 2002, Katsushi Arisaka
25
SNAP (SuperNova Acceleration
Probe)
•Mirror Diameter:
•FOV:
•Wavelength:
•IR Photometry:
HgCdTd
•IR Spectroscopy:
June 17, 2002
2m
1o x 1o
0.35-1 m
10’x10’,
2”x2”
Beaune 2002, Katsushi Arisaka
26
SNAP – Dark Energy Sensitivity
June 17, 2002
Beaune 2002, Katsushi Arisaka
27
Deep Sky Survey by Telescopes
Larger Mirror
Larger FOV
LSST
SDSS
SNAP
Ground
Space
NGST
HST
June 17, 2002
Keck
Beaune 2002, Katsushi Arisaka
28
The Extreme Universe
AGN
Pulsar
SNR
Radio
Galaxy
June 17, 2002
GRB
Beaune 2002, Katsushi Arisaka
29
GLAST - Gamma Ray Sky Survey
Si Strip
CsI +
Photo Diode
June 17, 2002
Beaune 2002, Katsushi Arisaka
30
Gamma ray Telescopes
VERITAS
HESS
•10m Diameter
•~500PMT/Camera
•4-7 Telescopes
80 m
June 17, 2002
Beaune 2002, Katsushi Arisaka
31
MAGIC under Construction
•17m mirror
•3.6o FOV
•600 PMTs
•Upgrade to GaAsP HAPD
June 17, 2002
Beaune 2002, Katsushi Arisaka
32
-ray Wide-FOV Telescope
•>3m diameter
•>30o FOV
•Mega pixel
June 17, 2002
Beaune 2002, Katsushi Arisaka
33
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
June 17, 2002
Beaune 2002, Katsushi Arisaka
34
Energy Spectrum of Cosmic Rays
• Energy Spectrum
~ E-3
• The spectrum
extends beyond
1020eV
• Beyond 1020eV,
Flux is only one
particle per km2century
1TeV
June 17, 2002
Beaune 2002, Katsushi Arisaka
35
Tools to explore the Early Universe
Time
(sec)
Temp. Energy
(oK) (GeV)
-45
10 sec
18
10
30
-40
10
10
1015
10-35
10-30
1025
10-25
10-20
1012
109
1020
UHE Cosmic Rays
1PeV
10-15
10-10
1015
1TeV
1GeV
10-5
1010
1MeV
105 sec
1 year 105
103
106
109 year 1
1KeV
1
June 17, 2002
1eV
10-3eV
Accelerator
Telescope
Beaune 2002, Katsushi Arisaka
36
Why is
20
10 eV
so special?
 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
June 17, 2002
Beaune 2002, Katsushi Arisaka
37
Pierre-Auger Observatory
Northern Auger
in Utah
S
#
N
Southern Auger
in Argentina
#S
S
50km
June 17, 2002
Beaune 2002, Katsushi Arisaka
38
Surface Detector and the Andes
1,600 Water Tanks
x 32002,
PMTs
= 4,800
Beaune
Katsushi
Arisaka of 9” PMTs
June 17, 2002
39
EUSO on International Space Station
EUSO
June 17, 2002
Beaune 2002, Katsushi Arisaka
40
Night Sky
June 17, 2002
Beaune 2002, Katsushi Arisaka
41
EUSO vs. Pierre-Auger
Pierre-Auger
EUSO
~400km
June 17, 2002
Beaune 2002, Katsushi Arisaka
42
06-Jan-00
DJL
f/1.25, 7mm pixel, 2.8m EPD, Dmax < 3.75 Scale: 0.03
735.29
MM
EUSO Detector
June 17, 2002
•2.5m Diameter
•60o FOV
•f/1.25
Hamamatsu
R7600-M16/64
250k Pixel
Beaune 2002, Katsushi Arisaka
43
OWL Stereo View from Space
~1,000km
June 17, 2002
~1,000km
Beaune 2002, Katsushi Arisaka
44
AMS - Anti-Matter Search
•RICH uses Multi-anode PMT
•Hamamatsu R7600-M16
•14k Pixel
June 17, 2002
Beaune 2002, Katsushi Arisaka
45
AMS on International Space Station
June 17, 2002
Beaune 2002, Katsushi Arisaka
46
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
June 17, 2002
Beaune 2002, Katsushi Arisaka
47
Super-Kamiokande
•11,200 of 20” PMTs
•Expected to resume end of
this year with 50% PMTs
June 17, 2002
Beaune 2002, Katsushi Arisaka
48
Future: Hyper-K/UNO
~200k of 20” PMTs
June 17, 2002
Beaune 2002, Katsushi Arisaka
49
NESTOR and ANTARES
ANTARES
NESTOR
June 17, 2002
Beaune 2002, Katsushi Arisaka
50
AMANDA
June 17, 2002
Beaune 2002, Katsushi Arisaka
51
ICECUBE
AMANDA-II
10 TeV Muon Event
1 km
June 17, 2002
60 PMTs/string x 80
strings
= 4,800PMTs
Beaune 2002, Katsushi Arisaka
52
Detection of Cosmic Radiation
Larger Volume
Lower Threshold
OWL
EUSO
ICECUBE
Pierre-Auger
Hyper-K
AMANDA
Cosmic Ray
Neutrino
Super-K
Zeplin
Dark Matter
CDMS
June 17, 2002
Beaune 2002, Katsushi Arisaka
53
Talk Outline
 Astro-Physics
 Cosmology
 High-energy Particle Astro-physics
 Experiments
 Ongoing
 Future
 Photo-detectors
 Demands
 New Detectors on Horizon
 Dream Detectors
June 17, 2002
Beaune 2002, Katsushi Arisaka
54
Photon Detector
More Pixels
Better Sensitivity
LSST
SDSS
OWL
 Wide FOV
CCD
PMT
Hyper-K
EUSO
Auger-FD
Super-K
AMS
VERITAS
June 17, 2002
Beaune 2002, Katsushi Arisaka
Auger-SD
55
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
June 17, 2002
Costs!
Beaune 2002, Katsushi Arisaka
56
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
June 17, 2002
Costs!
Beaune 2002, Katsushi Arisaka
57
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
 STJ
 TES
June 17, 2002
Russia
ESTEC
Stanford
Beaune 2002, Katsushi Arisaka
58
DEP Hybrid Photodiode (HPD)
•Baseline design for LHC-b RICH
•8cm diameter
•61 Pixel, (5mm view)
June 17, 2002
Beaune 2002, Katsushi Arisaka
59
Energy Resolution





June 17, 2002
QE
Col
ENF
G
NBG
as high as possible.
as close as 100%
as close as 1.0
>> ENC (~1000e-)
<< N
Beaune 2002, Katsushi Arisaka
( > 30% )
( > 0.9 )
( < 1.2 )
( >> 104 )
( << 1 )
60
Energy Resolution
10
APD
HPD
Energy Resolution
1
PMT
0.1
Photo Diode
Poisson Limit
0.01
0.001
100
June 17, 2002
101
102
103
104
No.of Katsushi
PhotonsArisaka
Beaune 2002,
105
106
107
61
Hamamatsu Flat Panel PMT
64 Pixels
June 17, 2002
Beaune 2002, Katsushi Arisaka
62
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
10000
Counts
8000
2270V
2400V
6000
4000
2000
0
0
5e+5
1e+6
2e+6
2e+6
Charge (e)
June 17, 2002
Beaune 2002, Katsushi Arisaka
by Paul Hink
63
Silicon MCP
•~7µm pores
•>75% open area
•Diamond coated
Gain > 1,000
Glass MCP
Si MCP
By O. Siegmund, U.C. Berkeley
June 17, 2002
Beaune 2002, Katsushi Arisaka
64
Semiconductor Photo-cathode
by Hamamatsu
InGaN
June 17, 2002
Beaune 2002, Katsushi Arisaka
65
Silicon Photomultiplier
by P. Buzhan, B. Dolgoshein et. al.
Gain~106
June 17, 2002
ENF=1.0
Beaune 2002, Katsushi Arisaka
DQE~10%
66
Superconducting Tunneling Junctions
(STJ)

Developed by ESTEC, ESA

Detect Photon by Photon:
 Energy
 Time
 Position
< 0.1 eV
< 1 nsec
< 10 m
Energy resolution
June 17, 2002
Beaune 2002, Katsushi Arisaka
67
Transition Edge Sensor (TES)
The Astrophysical Journal, 563:
221È228, 2001 December 10
R. Romani ,et al.
20 x 20 m2
June 17, 2002
Beaune 2002, Katsushi Arisaka
68
Crab Pulsar observed by TES
June 17, 2002
Beaune 2002, Katsushi Arisaka
69
Mega-Pixel TES/STJ
Detect
Photon by Photon:
 Energy
 Time
 Position
Ultimate
June 17, 2002
< 0.1 eV
< 1 nsec
< 10 m
Photon Detector!
Beaune 2002, Katsushi Arisaka
70
Dream Team for Astro-Physics
CCD:
~10m• 1G pixels
STJ:
~20m• 1M pixels
HAPD:
~1mm• 1K pixels
June 17, 2002
Beaune 2002, Katsushi Arisaka
71
Multi-pixel Hybrid APD
Glass Window (1mmt)
APD Array
InGaN Photo Cathode
(32 x 32 = 1024 Pixel)
Readout Electronics
HV
Ceramic
Case
Optical Fiber for
Signal Readout
LV
47.6mm•
50.5mm•
•1.4mm• Pixel Size, 1.5mm Pitch
•32 x 32 = 1,024 Pixels
•QE ~ 50% at 350 ~ 400nm
•Gain ~105
June 17, 2002
Beaune 2002, Katsushi Arisaka
72
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
June 17, 2002
Beaune 2002, Katsushi Arisaka
73
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!
June 17, 2002
Beaune 2002, Katsushi Arisaka
74
Can “your photo-detector” see
the dark side of this picture?
June 17, 2002
Beaune 2002, Katsushi Arisaka
75