Katsushi Arisaka - UCLA Physics &...
Transcript of Katsushi Arisaka - UCLA Physics &...
Katsushi Arisaka
University of California, Los Angeles Department of Physics and Astronomy
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4/11/2012 Katsushi Arisaka,UCLA 2 Why are we here?
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Seven Phases of Cosmic Evolution
14 billion years ago
Origin of Particles
Origin of Structure
Origin of Life
Origin of Consciousness
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Unification of Forces
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Planck Epoch
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100 GeV 1016 GeV 1019 GeV
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Hubble Deep Field Physicists’ View of Early Universe
Symmetry Breaking
Symmetry Break Down
Simple
Complex
Time
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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
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Accelerator Microscope Telescope
Seven steps of cosmic evolution
14B years ago
Spontaneous Symmetry Breaking
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Origin of Elements
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The Solar Interior
Hydrogen Gas
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Solar Energy
m4p > mHe
E = mC2
ε = = 0.007
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The Formation of the Elements
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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
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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.
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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.
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Supernova 1987A
Before After
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Super-Kamiokande
• 11,200 of 20” PMTs
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Nobel Prize in 2002
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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☺
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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.
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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
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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”
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We are made from “stardust”
Origin of Life
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Star’s Life Cycle
Big Bang! (14 B years ago)
Sun (4.6 B years ago)
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Periodic Table of Elements
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Abundance of Elements
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Origin of Life
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Seven Phases of Cosmic Evolution
14 billion years ago
Origin of Particles
Origin of Structure
Origin of Life
v
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Solar System (4.6B years ago)
Sun (Hydrogen) Earth (Heavy Elements)
Iron Core of the Earth
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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.
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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.
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Urey-Miller Experiments
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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.
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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.
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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.
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Origin of Life
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Organic molecules from outer space
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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.
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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
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Evolution of Life
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RNA World
RNA Word (4B à 3.5B years ago)
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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
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Ø Movie of DNA
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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.
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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.
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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
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Micron 1.3M-Pixel CMOS Sensor
2 µsec/row 2 msec/frame (10 bits, 66MHz)
Photron SA-5 CMOS Camera
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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
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#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)
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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
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Laurent Bentolila (CNSI)
CMOS Camera Photron SA-1
5k – 500k fps
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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)
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Gain = 100 - 1000
( 5 – 10 μm ϕ)
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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
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ICMOS Camer
a 2,000 fps
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10000
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1000000
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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
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E2V-Caeleste scientific-CMOS (in development)
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Photosynthesis and Breathing
6CO2 + 12H2O → C6H12O6 + 6H2O + 6O2
Plants Chloroplast
Animals Mitochondria
→ Photosynthesis
Breathing
Spontaneous Symmetry Breaking
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Tree diagrams of evolution Human
~2B years ago(Eukaryote)
~3.8B year ago(First Life)
〜2M years ago
Plants Animals
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Evolution of Humans Human
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Summary
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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
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