katsushi arisaka - ucla physics &...

Katsushi Arisaka

University of California, Los Angeles Department of Physics and Astronomy

arisaka@physics.ucla.edu

11/19/12 Katsushi Arisaka 1

4/11/2012 Katsushi Arisaka,UCLA 2 Why are we here?

11/19/12 Katsushi Arisaka 3

Seven Phases of Cosmic Evolution

14 billion years ago

Origin of Particles

Origin of Structure

Origin of Life

Origin of Consciousness

4/11/2012 Katsushi Arisaka,UCLA 4

Unification of Forces

1032

Planck Epoch

1029

100 GeV 1016 GeV 1019 GeV

11/19/12 Katsushi Arisaka 5

Hubble Deep Field Physicists’ View of Early Universe

Symmetry Breaking

Symmetry Break Down

Simple

Complex

Time

2

3

4

5

6

7

8

9

10

11

12

13

14

1B years 0

Zo µ-

d

µ+

νe

u e+ γ e-

W+

νµ

νe νµ

W+

s

u sd τ- τ+ c b

b c

11/19/12 Katsushi Arisaka 6

7

Accelerator Microscope Telescope

Seven steps of cosmic evolution

14B years ago

Spontaneous Symmetry Breaking

4/11/2012 Katsushi Arisaka,UCLA

3/8/2007 Katsushi Arisaka 8

Origin of Elements

11/19/12 Katsushi Arisaka 9

The Solar Interior

Hydrogen Gas

11/19/12 Katsushi Arisaka 10

Solar Energy

m4p > mHe

E = mC2

ε = = 0.007

2/6/2007 Katsushi Arisaka 11

2/6/2007 Katsushi Arisaka 12

The Formation of the Elements

3/8/2007 Katsushi Arisaka 13

Nuclear Burning in High Mass Stars

(times for a 20 Mo star)

Hydrogen 107 yr Helium 106 yr Carbon 103 yr Oxygen 1 yr Neon Magnesium Silicon 1 week Iron < 1 day

2/6/2007 Katsushi Arisaka 14

The End of a High-Mass Star

This graph shows the relative stability of nuclei. On the left, nuclei gain energy through fusion; on the right they gain it through fission.

Iron is the crossing point; when the core has fused to iron, no more fusion can take place.

2/6/2007 Katsushi Arisaka 15

Power of Super Novae

Ø Within a few hours § one billion times solar luminosity

Ø Within a few months § ~ same as the Sun’s total energy during 10

billion years of life

Ø Not only that, > 99.99 % of energy is released by neutrino within ~ 10 seconds. § First observed in 1987 by Kamiokande

experiment in Japan.

2/6/2007 Katsushi Arisaka 16

Supernova 1987A

Before After

2/6/2007 Katsushi Arisaka 17

Super-Kamiokande

• 11,200 of 20” PMTs

2/6/2007 Katsushi Arisaka 18

Nobel Prize in 2002

2/8/2007 Katsushi Arisaka 19

End Results of Stars

Initial Mass End Results

< 8 M☺ White Dwarf < 1.4 M☺

8 – 20 M☺ Type II Supernova

Neutron Star 1.4 – 3 M☺

> 20 M☺ Black Hole > 3 M☺

2/8/2007 Katsushi Arisaka 20

Pauli’s Exclusion Principle

Ø Fermi Statistics: § According to quantum mechanics, each

state is occupied by one particle (Fermion). Another particle can not stay in the same state.

Ø Degenerate matter: § All possible states are occupied.

2/8/2007 Katsushi Arisaka 21

Degenerate Matter

Ø White Dwarf ( < 1.4 M☺) § Carbon Core § Electrons are tightly packed

Ø Neutron Star (1.4 M☺– 3 M☺) § Neutrons are tightly packed

Ø Black Hole ( > 3 M☺) § Gravity wins

e- e- e-

e-

e-

e- e-

n n n

n

n

n n

3/8/2007 Katsushi Arisaka 22

Origin of Elements

Ø Hydrogen, Helium § From “Big Bang”

Ø Carbon – Oxygen – Iron § From “Nuclear fusion” at massive stars

(> 8 Msun )

Ø Heavier than Iron (Cu, Au, Pt, Pb…) § From “Supernovae”

3/8/2007 Katsushi Arisaka 23

We are made from “stardust”

Origin of Life

3/8/2007 Katsushi Arisaka 24

Star’s Life Cycle

Big Bang! (14 B years ago)

Sun (4.6 B years ago)

2/6/2007 Katsushi Arisaka 25

6/23/2011 Katsushi Arisaka 26

Periodic Table of Elements

3/8/2007 Katsushi Arisaka 27

Abundance of Elements

3/13/2007 Katsushi Arisaka 28

Origin of Life

11/19/12 Katsushi Arisaka 29

Seven Phases of Cosmic Evolution

14 billion years ago

Origin of Particles

Origin of Structure

Origin of Life

v

11/19/12 Katsushi Arisaka, UCLA 30

Solar System　（4.6B years ago）

Sun (Hydrogen) Earth (Heavy Elements)

Iron Core of the Earth

3/13/2007 Katsushi Arisaka 32

The Oldest Fossil found by W. Schopf

Generally accepted evidence of bacterial life from the 3.5 Billion Year Apex Formation of Australia has been published by Bill Schopf (UCLA) and others.

3/13/2007 Katsushi Arisaka 33

Origin of Life

Earth was subject to volcanoes, lightning, radioactivity, ultraviolet radiation, and meteoroid impacts.

Over a billion years or so, amino acids and nucleotide bases formed. The process by which this happens has been re-created in the laboratory.

3/13/2007 Katsushi Arisaka 34

Urey-Miller Experiments

3/13/2007 Katsushi Arisaka 35

Urey-Miller Experiments

This is a schematic of the Urey–Miller experiment, first done in the 1950s, that demonstrated the formation of amino acids from the gases present in the early Earth’s atmosphere, excited by lightning.

3/13/2007 Katsushi Arisaka 36

Creation of Amino Acids It is also possible that the source of complex organic molecules could be from outside Earth, on meteorites or comets.

This image shows droplets rich in amino acids, formed when a freezing mix of primordial matter was subjected to harsh ultraviolet radiation.

3/13/2007 Katsushi Arisaka 37

Meteorite

This meteorite, which fell in Australia, contains 12 different amino acids found in Earthly life, although some of them are slightly different in form.

11/19/12 Katsushi Arisaka, UCLA 38

Origin of Life

3/13/2007 Katsushi Arisaka 39

Organic molecules from outer space

3/13/2007 Katsushi Arisaka 40

Life in Deep Ocean?

Even on Earth, organisms called extremophiles survive in environments long thought impossible – here, hydrothermal vents emitting boiling water rich in sulfur.

3/13/2007 Katsushi Arisaka 41

Volcano under deep ocean

Deviation from Thermal Equilibrium

Ø Particles 　 —　Quark, Leptons… § Spontaneous Symmetry Breaking (Higgs Mechanism)

Ø Atoms　　 —　Carbon, Oxygen, Iron … § Explosion of Supernova

Ø Organic Molecules —　Ammonia, Amino Acid … § Evolution of molecules in outer space by UV

Ø Origin of Life —　RNA, Protein, DNA § Volcano under deep ocean

11/19/12 Katsushi Arisaka 42

3/13/2007 Katsushi Arisaka 43

Evolution of Life

3/13/2007 Katsushi Arisaka 44

RNA World

RNA Word (4B à 3.5B years ago)

11/19/12 Katsushi Arisaka 45

3/13/2007 Katsushi Arisaka 46

Evolution of Life

Eukaryote　（~2B years ago）

10 – 50 µm

Up to ~2 m long

2 nm　wide

Cells made by proteins DNA for genetic coding

Spontaneous Symmetry Breaking

11/19/12 Katsushi Arisaka 47

Ø Movie of DNA

11/19/12 Katsushi Arisaka,UCLA 49

How to observe the “Origin of Life”

Ø Exactly the same way as we look for the “Origin of Universe”

Telescope　↔　Microscope

Ø We must look for “Live Life”

Ø Take advantages of the state of art “Photon Detectors” in particle physics.

11/19/12 50

The H33D detector

attaches to a standard

fluorescence microscope

Laser

It will permit to track multicolor qdot-

labeled proteins in live cells virtually background-free

Single Molecule Imaging

Particle Physics Detector

Nano Technology

Katsushi Arisaka,UCLA

How to speed up microscopes

Ø All the existing microscopes are limited by the narrow bandwidth of readout. §  Just one channel of FADC (Flash Analog to Digital

Converter) running at 10 – 50 MHz § So-called Video Rate (30 frame/sec)

Ø The first step is to adopt multiple channels of FADC for massive parallel processing. §  Like high energy experiments (such as LHC)

Ø In addition, we need Single Photon Sensitivity with

high Quantum Efficiency.

4/11/2012 Katsushi Arisaka,UCLA 51

4/11/2012 Katsushi Arisaka,UCLA 52

Principle of High-speed Bio Imaging

Wide Field Confocal

CMOS [ FADC (50 MHz) * 100 ] [ HAPD + FADC (1 GHz) ] * 64

PMT + FADC (10 – 50 MHz) CCD + FADC (10 – 50 MHz)

Pinhole

Sample Sample

4/11/2012 Katsushi Arisaka,UCLA 53

Micron 1.3M-Pixel CMOS Sensor

2 µsec/row 2 msec/frame (10 bits, 66MHz)

Photron SA-5 CMOS Camera

4/11/2012 Katsushi Arisaka,UCLA 54

Gold nano particle (40nm) attached to Transferrin Receptor (TfR) on Cancer Cell

Prof.  Manuel  Penichet  (Oncology)  

(10,  000  frame/sec)

Mean Squire Displacement <r2> of TfR on a Human Multiple Myeloma Cell vs. Time

4/11/2012 Katsushi Arisaka,UCLA 56

10  

100  

1000  

10000  

0.01   0.1   1   10   100  

#1   #2  #3   #4  #5   #6  #7   #8  #9   #10  

T  (msec)  

<r2 >  (n

m2 )  

Type A

Type B

Brownian Motion

?

Arisaka’s Campus-wide Collaborations on High-Speed Bio-imaging

California Nano Systems Institute (CNSI, Laurent Bentolila)

Dept. of Chemistry & Biochemistry (Shimon Weiss)

Dept. of Surgical Oncology (Manuel Penichet)

Dept. of Physics & Astronomy (Dolores Bozovic, Mayank Mehta)

Dept. of Neurology & Neurobiology (Carlos Portera-Cailliau, Jack Feldman, Tom Otis)

Dept. of Electrical Engineering (Bahram Jalali)

4/11/2012 Katsushi Arisaka,UCLA 57

Industrial Partners (Hamamatsu Photonics,

Photron, Leica)

User-shared Core Facility of High-speed Microscopes at CNSI

4D Nano Biophysics 4/11/2012 Katsushi Arisaka,UCLA 58

Nikon Microscope TE200E with TIRF at CNSI

4/11/2012 Katsushi Arisaka,UCLA 59

Laurent Bentolila (CNSI)

CMOS Camera Photron SA-1

5k – 500k fps

4/11/2012 Katsushi Arisaka,UCLA 60

Principle of ICMOS

CMOS Camera CMOS Camera (> 1,000 frame/sec)

GaAsP Photocathode (50% QE)

Multi-channel High-speed Digitization

Photron MCP

(Micro Channel Plate)

MCP (Micro Channel Plate)

4/11/2012 Katsushi Arisaka,UCLA 61

Gain = 100 - 1000

( 5 – 10 μm ϕ)

4/11/2012 Katsushi Arisaka,UCLA 62

ICMOS  Camera  (Photron  SV200i)  

EMCCD Camera (Ando iXon 897)

Confocal  Spinner  (Yokogawa  CSU-­‐X1)  

High-­‐speed  Confocal  Microscope  with  ICMOS  at  CNSI  

Leica Microscope

(1,000  frame/s)

Laurent Bentolila (CNSI)

Yokogawa CSU-X1

4/11/2012 Katsushi Arisaka,UCLA 63

ICMOS Camer

a 2,000 fps

10  

100  

1000  

10000  

100000  

1000000  

10   100   1000  

SA-1 1024PCI iXon 897 Neuro-SMQ ORCA-R2 4-beam 64-beam

Frame Rate vs. Resolution

CMOS (SA-1)

ICMOS (SV200i)

CCD (Neuro-SMQ)

4-beam MMM EMCCD (iXon 897)

CCD (ORCA)

Confocal Scanner (Yokogawa CSU-X1)

Conventional

No. of Pixels (in X-Y)

Fram

e Rat

e (fra

me/s

ec)

New Systems

10 x 10 100 x 100 1000 x 1000

Video Rate (Response of human

eyes)

1 msec

100 µsec

10 µsec

1 µsec

10 msec

64-beam MMM

4/11/2012 Katsushi Arisaka,UCLA 64

E2V-Caeleste scientific-CMOS (in development)

4/11/2012 Katsushi Arisaka,UCLA 65

Photosynthesis and Breathing

6CO2 + 12H2O 　→ 　C6H12O6 + 6H2O + 6O2

Plants Chloroplast

Animals Mitochondria

→ Photosynthesis

Breathing

Spontaneous Symmetry Breaking

11/19/12 Katsushi Arisaka 66

Tree diagrams of evolution Human

~2B years ago（Eukaryote)

~3.8B year ago（First Life)

〜2M years ago

Plants Animals

11/19/12 Katsushi Arisaka 67

Evolution of Humans Human

11/19/12 Katsushi Arisaka 68

3/13/2007 Katsushi Arisaka 69

Summary

3/13/2007 Katsushi Arisaka 70

Summary of Origin of Life

•  The history of the universe can be divided into phases: particulate, galactic, stellar, planetary, chemical, biological, and cultural.

•  This whole process is called cosmic evolution.

•  Living organisms should be able to react to their environment, grow by taking in nutrients, reproduce, and evolve.

•  Amino acids could have formed in the conditions present on the early Earth, or in space.

What is Life?

Ø Emergent Property § Strongly-interacting, complex system § ~104 of different proteins in one cell § ~1014 cells in one life

Ø Continuous, countless “symmetry breaking” towards coherent states § Origin of life § Evolution of life § Growth from a single cell to a multi-cell body

11/19/12 Katsushi Arisaka 71