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

arisaka@physics.ucla.edu

Katsushi Arisaka

Trends, Needs and Dreams in Astro-

Physics

Talk Outline

Astro-Physics Cosmology High-energy Particle Astro-physics

Experiments Ongoing Future

Photo-detectors Demands New Detectors on Horizon Dream Detectors

Talk Outline

Hubble Deep Field

~100 Billion GalaxiesRed shift up to 10

Evolution of the Early Universe

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Radius of Universe (cm)

Golf Ball

People

Mountain

1 A.U.

1 Light Year

Galaxy

10-33 Big Bang!

Tools to explore the Early Universe

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Accelerator

Telescope

Unification of Fundamental Forces

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Planck

FundamentalInteraction

Hubble Deep FieldPhysicists’ View of Early Universe

Symmetry Breaking

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Simple

SymmetryBreak Down

Complex

Relics from the Earliest Universe

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Gravitational Wave

Neutralino(Cold Dark Matter)

Relic Neutrino(Hot Dark Matter)

GUT Particle

Planck

Big Bang

CMB : Matter-Radiation Decoupling

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Planck

Matter-RadiationDecoupling CMB

Time = 300,000 years

Temperature = 3,000 oK

Energy = 0.3 eV

Z = 1,100

CMB Anisotropy by COBE DMR

CMB Anisotropy by Boomerang

Recent Results of CMB Anisotropy

The Accelerating Universe

Density of Our Universe

Matter

Universe is Flat. Inflation

70% is Dark Energy. Accelerating

Talk Outline

Relics from the Earliest Universe

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Gravitational Wave

Neutralino(Cold Dark Matter)

Relic Neutrino(Hot Dark Matter)

GUT Particle

Dark Energy

Planck

Big Bang

The Extreme Universe

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Planck

Big Bang

Active Galactic Nuclei

Gamma Ray Burst

Supernova Neutron Star Black Holes

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

Dark Matter Gravitons

SDSS (Sloan Digital Sky Survey)

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

Focal Plane

SDSS Early Data Release

Distance record-holderGoal:

500 sq. degree of the sky.

14 million objects.

Spectra for 50,000 galaxies5,000 quasars.

LSST (Large-aperture Synoptic Survey Telescope)

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

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

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”

SNAP – Dark Energy Sensitivity

Deep Sky Survey by Telescopes

HSTKeck

Larger MirrorLarger FOV

Ground

The Extreme Universe

Pulsar

Radio Galaxy

GLAST - Gamma Ray Sky Survey

CsI + Photo Diode

Si Strip

Gamma ray Telescopes

VERITAS HESS

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

MAGIC under Construction

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

-ray Wide-FOV Telescope

• >3m diameter• >30o FOV• Mega pixel

Energy Spectrum of Cosmic Rays

• Energy Spectrum ~ E-3

• The spectrum extends beyond 1020eV

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

Tools to explore the Early Universe

10-45sec

105 sec

1 year103

109 year

Time (sec)

Temp. (oK)

Energy (GeV)

10-3eV

Accelerator

Telescope

UHE Cosmic Rays

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?

Pierre-Auger Observatory

Southern Augerin Argentina

Northern Augerin Utah

Surface Detector and the Andes

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

EUSO on International Space Station

Night Sky

EUSO vs. Pierre-Auger

Pierre-Auger

~400km

EUSO Detector16:16:09

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

Scale:

DJL 06-Jan-00

735.29 MM

• 2.5m Diameter• 60o FOV• f/1.25

Hamamatsu R7600-M16/64250k Pixel

OWL Stereo View from Space

~1,000km

AMS - Anti-Matter Search

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

AMS on International Space Station

Charged Particles• High Energy Cosmic Rays• Anti-particles

Super-Kamiokande

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

Future: Hyper-K/UNO

~200k of 20” PMTs

NESTOR and ANTARES

NESTOR

ANTARES

AMANDA

ICECUBE

10 TeV Muon Event

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

Detection of Cosmic Radiation

Super-K

AMANDA

Pierre-Auger

Hyper-K

ICECUBE

EUSOOWL

Zeplin

Larger VolumeLower Threshold

Dark Matter

Neutrino

Cosmic Ray

Talk Outline

Photon Detector

VERITAS

Super-K

Wide FOV

Hyper-K

More PixelsBetter Sensitivity

Auger-FD

Auger-SD

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!

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!

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

DEP Hybrid Photodiode (HPD)

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

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 )

Energy Resolution

No.of Photons

100 101 102 103 104 105 106 107

Poisson Limit

Photo Diode

APDHPD

Hamamatsu Flat Panel PMT

64 Pixels

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

2270V 2400V

by Paul Hink

Silicon MCP

By O. Siegmund, U.C. Berkeley

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

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)

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

Semiconductor Photo-cathodeby HamamatsuInGaN

Silicon Photomultiplier

Gain~106 DQE~10%ENF=1.0

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

Superconducting Tunneling Junctions (STJ)

Energy resolution

Developed by ESTEC, ESA Detect Photon by Photon:

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

Transition Edge Sensor (TES)

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

20 x 20 m2

Crab Pulsar observed by TES

Mega-Pixel TES/STJ

Detect Photon by Photon:

Energy < 0.1 eVTime < 1 nsecPosition < 10 m

Ultimate Photon Detector!

Dream Team for Astro-Physics

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

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

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

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!

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

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

Documents

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

A 3D-Object Reconstruction System Integrating … · A 3D-Object Reconstruction System Integrating Ran e-Image Processing and Rapif Prototyping Carlos Cerrada, Katsushi Ikeuchi, ...

Katsushi Arisaka · The Lead TA of Physics 4BL, Javier Carmona, is running his morning section at his home. 10 TA + 10 LA Developing TA Instructor Lead TA. Physics 4BL –Javier teaching

Katsushi Imai Md. Shafiul Azam - University of Manchesterhummedia.manchester.ac.uk/schools/soss/economics/discussionpaper… · 1 Does Microfinance Reduce Poverty in Bangladesh? New

Daisuke Miyazaki, Masataka Kagesawa, Katsushi Ikeuchi ...

The Cosmic Ray Spectrum as Measured by the Surface Detector …home.physics.ucla.edu/~arisaka/Thesis/Joong_Lee_Thesis.pdf · 2004. 1. 1. · \The Cosmic Ray Spectrum with 2 Years

1/27/2016Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy Katsushi Arisaka XAX 10.

Illumination Normalization with Time-dependent Intrinsic ... · Yasuyuki Matsushitay Ko Nishinoz Katsushi Ikeuchiy Masao Sakauchiy y Institute of Industrial Science, The University

G. Travish FAC Meeting travish@physics.ucla.edu 28OCT05 The LCLS BC1 Bunch Length Monitor System Eric Bong 1 Mike Dunning 2 Paul Emma 1 Patrick Krejcik.

Optimization of OWL-AirWatch Optics & Photo-Detectors · 2010. 6. 26. · Katsushi Arisaka University of California, Los Angles Department of Physics and Astronomy Los Angles, California

Katsushi Arisaka - University of California, Los Angelesarisaka/Talks/2012/Arisaka_120224... · 2012. 11. 16. · Katsushi Arisaka, UCLA 1 University of California, Los Angeles Department

Polarization-based Inverse Rendering from Single View Daisuke Miyazaki Robby T. Tan Kenji Hara Katsushi Ikeuchi.

Sonoluminescence: How Bubbles Turn Sound into Light · Physics Department, University of California, Los Angeles, California 90095; e-mail: putterman@physics.ucla.edu Key Words energy

Atsushi Nakazawa, Takeshi Oishi, Jun Takamatsu, Kiminori Hasegawa, Katsushi Ikeuchi

ARISAKA TYPE 38.pdf

ECON60022 Development Microeconomics Lectures 6 & Tutorial 4: ‘Models on Rural Credit Markets’ Katsushi Imai Email: katsushi.imai@manchester.ac.ukkatsushi.imai@manchester.ac.uk.

Katsushi S. Imai1 Takahiro Sato November 2008hummedia.manchester.ac.uk/institutes/gdi/publications/working... · Fertility, Parental Education and Development in India: Evidence from

The Effects of the Environmental Stress on the Wood Formation in Acacia mangium Chunhua ZHANG, Hisashi ABE Katsushi KURODA & Takeshi FUJIWARA Wood Anatomy.

Art & Robotics: Toward Robot artists - Through Learning-from-observation - Katsushi Ikeuchi University of Tokyo.

9/26/2006Katsushi Arisaka, UCLA 1 Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Unveiling.

IEEE Robotics and Automation Society Ad-Hoc Committee on New Publications Ken Goldberg, Chair Srinivas Akella Hideki Hashimoto Bill Hamel Katsushi Ikeuchi.