Overview of Synchrotron
Radiation Research and theAOFSRR
Richard Garrett
Senior Advisor, Synchrotron Science, ANSTO

2015 Cheiron School

Founded - 2006
AOFSRR Objective
The objective of the AOFSRR is to encourage regional collaboration in, andto promote the advancement of, synchrotron radiation research and related
subjects in Asia and Oceania.

Specific Activities:(1) The annual workshop and Cheiron School, and organization of otherscientific collaboration meetings;(2) Exchange of information of facilities and user groups;(3) Provision of a framework for cooperative activities;(4) Any activities that promote and expand the role of synchrotron
light source facilities and synchrotron based research in theAsia – Oceania region.
2015 Cheiron School

ESRF

European Union
DiamondFLASH

Large: ESRF (+PETRA)
Medium: Diamond, Soleil, SLSSoft X 3rg gen: Elettra, Max,BESSY II …
Next generation: FLASH,
European XFEL, FERMI, PSI..
2015 Cheiron School

APS

The Americas

LCLS (Stanford)

CLS
2015 Cheiron School

Large: APS
Medium: CLS, NSLS II,SSRLSoft X 3rd Gen: ALS
2nd gen: NSLS, CHESS,Brazil, Alladin…
Next generation: LCLS,JLab, Cornell ERL(?)

SSRF

Asia Oceania & the AOFSRR
NSRRC

Siam

SPring-8& SACLA

Large: SPring-8
Medium: AS, Indus II,
PLS II, Shanghai, TPS..
Soft X 3rd Gen: TLS,UVSOR, Heifei..
2nd Gen: Beijing, PF,Thailand, Singapore …
Next Gen:SACLA,• Facilities equal or better than Europe& USA
PAL-XFEL, SCSS…

• Many bi-lateral agreements between facilities• Few relationships between user communities• No real regional organisation

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Members:• Australia• China• India• Japan• South Korea• Singapore
Associate Members:• Malaysia• New Zealand• Vietnam
2015 Cheiron School• Taiwan• Thailand

AOFSRR Activities

2015 Cheiron School

Annual Workshop
YearHost2006

Tsukuba, Japan

2007

Hsinchu, Taiwan

2008

Melbourne, Australia

2009

Shanghai, China

2010

Pohang, South Korea

2011/12

Bangkok, Thailand

2013

Himeji, Japan

2014

Hsinchu, Taiwan

2015

Melbourne, Australia

Cheiron School: Always SPring-8 !!
2015 Cheiron School

Promote Synchrotron Research• Nations can build new communities at otherfacilities– Australian soft X-ray program at NSRRC and– NSRRC hard X-ray program at SPring-8– Indian beamline at the Photon Factory• Promote SR research in non-member nations inthe A-O region• Assist SR science in developing nations– Cheiron School– Assistance to attend conferences– Work with other organisations (IUCr etc)
2015 Cheiron School

Synchrotron Radiation

X25 wiggler beam, NSLS

2015 Cheiron School

Outline• What is a synchrotron?
• What are the Applications• How is the light produced & what are its
characteristics?
• Brief Basics of Synchrotron Beamlines• The Future (is here already): “NextGeneration Sources”• A Cool Example

2015 Cheiron School

A brief history• First observed:
1947, General Electric, 70 MeV synchrotron• First user experiments:
1956, Cornell, 320 MeV synchrotron• First insertion Device:
1979, 7 pole wiggler, SSRL
• 1st generation light sources: high energy physics synchrotrons and storage rings
used parasitically for synchrotron radiation – eg DESY (Germany), INS-SOR(Tokyo), SPEAR (USA), (1960’s, 1970’s)• 2nd generation light sources: purpose built synchrotron light sources, eg Photon
Factory, NSLS, Daresbury (1980s onwards)• 3rd generation light sources: optimised for high brilliance with low emittance andInsertion Devices; SPRing-8,ESRF, APS, Diamond, …(1990’s onwards)• Free Electron Laser sources: FLASH (Germany), LCLS (USA), SACLA (Japan),
FERMI (Italy) … (2000’s)• Next??
2015 Cheiron School

A Synchrotron Step by Step
storage ring

Booster Synchrotron

quadrupole
magnets

bendingmagnetbooster
synchrotron

Main
Ring
linac(Storage Ring)

insertion device

beamline

Beamlines and2015 Cheiron School
Experimental
Stations

opticshutchElectron Gun
experimentand LinacUnique Characteristics of Synchrotron Radiation• Extremely high brightness. Modern synchrotron

sources are about 10 billion times as intense as alaboratory X-ray generator: dilute samples; fastmeasurements; trace elements;
 Low divergence: high intensity can be focussed
onto tiny samples: Microscopies• Wide X-ray energy spectrum:
 the optimum X-ray energy to be chosen for eachexperiment;
 X-ray spectroscopies are possible eg EXAFS• Polarisation: various dichroisms; magnetic imaging;molecular orientation;• Time structure: time of flight and very fast timing.
2015 Cheiron School

The Advanced
LightSource, Berkeley
AustralianSynchrotron2015 Cheiron SchoolX-rays and their Interaction with MatterCourtesy SRRC, Taiwan

X-ray Fluorescence trace element analysis

X-ray Diffraction  Structure2015 Cheiron School

Transmitted Photons:
 ImagingAbsorption Spectroscopy Chemical information

Synchrotron

ProtonElectronMicroscope

Sensitivity



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Sub micron

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ChemicalInformation

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





In-situ



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

AtomicStructure





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



2015 Cheiron SchoolSIMS

NeutronSometimes High Intensity = Better Data
Synchrotron Powder XRD

Multi-phase ceramic: α Al2O3, ZrO2, MgO-Al2O3 (spinel).
Top synchrotron data; Bottom: lab data.
B. H. Oconnor, A. van Riessen, J. Carter, G. Burton,R. F. Garrett and D. J. Cookson,
J. American Chemical Soc. 80 (1997) 1373

2015 Cheiron School

Synchrotron Powder Diffraction• Higher Resolution –and single wavelength• Enhanced Sensitivity• Greater “Q” Range(more reflections)• Variable energy/wavelength

Synchrotron data from
APS beamline 11-BM

2015 Cheiron SchoolImpact of Synchrotrons on Structural Biology
Cumulative number of structures in the PDB
ribosome

Structuresvirus

myosinantibody

nucleosometransfer RNAactin
hemoglobin

myoglobin2015 Cheiron SchoolYear

C. Zardecki - PDB
C. Abad-Zapatero - Acta Cryst D68 (2012)

Structure informs Function:
Insulin bound to it’s cell wall receptor
The 3D structure of the insulin
molecule was solved byDorothy Hodgkin in 1969 afteran extraordinary 35 year effort!

The 3D structure of insulin bound to
its target receptor is a huge milestone
towards better diabetes treatment andcould lead to the design of synthetic
insulin compounds.

Menting et al. Nature (2013)
Protein crystallography at Australian Synchrotron2015 Cheiron School

ATP Synthase: a Molecular MotorJohn Walker won the 1997 Nobel
Chemistry prize for solving the F1
catalytic domain using synchrotron2015 Cheiron
Schoolat Daresbury, UK.
radiation

Atomic structure informs biologicalfunction

Broad Energy Spectrum: SR Only Spectroscopies
eg Xray Absorption Spectroscopy
XANES: near edge structure
Sensitive to chemical environment ofabsorbing element.
Often different valence states havemarkedly different XANES spectra.

XANES spectra of Cr III (relativelybenign) and Cr VI, a known carcinogen.

2015 Cheiron School

EXAFS: extended structure to~1 keV above an absorption edge
Nearest neighbour atomic distances,coordination etc. Crystals not
required: disordered systems likesolution species can be measured.

Amorphous GaAs EXAFS and Fouriertransform.

Near Edge Spectroscopy: Chemical Sensitivity

*C=O

30

OH
NH2

Phenylalanine

2Oscillator Strength (10- )*ringO

Benzene + Alanine

20OOH
NH2Alanine

10Benzene

0285

290295

Energy (eV)

Carbon K-edge Spectra2015 Cheiron School

XANES of Pt located in atumour cell Hambley, U Syd

Imaging

Radiography

Mapping

Scanning

Various Imaging Techniques
have become more and more
important in synchrotron researchover the last 10 years
Imaging2015 Cheiron SchoolSome Imaging Needs Focusing optics
Reflective (Kirkpatrick-Baez mirrors)

typical ~1 µm

High efficiency, achromatic, limited to ~10 nm

Diffractive (Fresnel zone plates)
typical ~ 100 nm
Moderate efficiency, limited to ~10 nm

Refractive (compound refractive lenses) 10s µm - ~ 50 nm
Low efficiency, highly chromatic, aberrations
Works well with high energy X-rays

2015 Cheiron School

Contrast mechanisms in x-ray imaging
 Absorption

measure electron density; can be element specific Fluorescencemeasure elemental distribution

 Spectroscopy

extract chemical state, spin state Diffraction

reveal structure, strain, magnetism, charge…

 Phasemeasure real part of refractive index

In general with X-rays:• Natural sample contrast is often possible; staining not required• Image structure of thick samples, sectioning not required• More penetrating, less damage, less charging than with electrons• In situ imaging – image samples in natural environment.
2015 Cheiron SchoolPhase Contrast
Refractive index:

for X-rays it is less than 1 by about 1 part in a million
re 2n 1   i 1  ni fi (0)2i• Absorption contrast:
sensitive to Im(n)• Phase contrast:
sensitive to Re(n)• At high X-ray energies,
phase contrast wins

2015 Cheiron SchoolPhase Contrast
2. Diffraction
Propagation
Phase Contrast
1.
Enhanced
Imaging (DEI)

AS Medical Beamline
Wiggler Source
Phase contrast simulations(Can recover phase shift)Distance from sample
2015 Cheiron SchoolDiffraction Enhanced Imaging• Edge/density
gradient
sensitive• Move on rocking
curve to changecontrast

2015 Cheiron SchoolX-ray phase imaging: Biology and Materials

Rob Lewis, Monash
University/Energy = 20keV

Conventional X-ray

Synchrotron

Synchrotron: propagation phase contrast

DEI “Dark field” phase image ofbonded aluminium sheets @ 33
keVDots are bubbles in the epoxy
bond.
Stevenson, Garrett, Hyodo et.al.

2015 Cheiron SchoolX-ray Fluorescence Microscopy

Conventional Fluorescence Microscope: APS 2ID-D

Advanced fluorescence detector at the AS
Annular geometry• Maximises solid angle, sample @ 90°• 384 Si pixel detector array (BNL,Siddons etal)• No constraint on lateral sample sizeand scan range+ Parallel data processing• CSIRO: HYMOD2 pipelined, parallelprocessor (Ryan etal)• Whole XRF spectrum acquired andanalysed in real time

+ Fast Scanning Stage• Data acquired “on the fly”
• milli-second dwell times

cf 1 second or greater normally= New micro-XRF
capability at the AS X-ray
Fluorescence Microscope
beamline
Chris Ryan, CSIRO, David Paterson, AS,
2015Peter
CheironSidons,
School BNLXFM image definition (number of pixels) limited by dwell timeLong dwell  Low ImageDefinitionFe• ~1 s / pixel (for readout of 1-16detector spectra)• 1.3 hours  67 x 67 pixels
FeShort dwell  Good image definition

YRasterstageX• 32 ms / pixel• 1.3 hours  375 x 375 pixels (30 foldincrease)• New Maia detector

2015 Cheiron School

Courtesy C. Ryan, CSIRO

Golden Gum Leaves

position and size of tiny gold ‘nuggets’
present in gum leaves. This has helped
researchers ascertain how the gold moves
through the tree, potentially leading to new
exploration methods that involve samplingtree leaves rather than digging holes in theground
CSIRO Minerals Down Under Flagship (Mel Lintern)
The Australian Synchrotron2015 Cheiron School

Characteristics ofSynchrotron Radiation
 High brightness/flux
 Wide energy spectrum
 Plane polarised Pulsed2015 Cheiron School

Photon Factory

Generation of Synchrotron Radiation:
Radiation from Accelerating Charge

Low energy electrons
OR electron frame:
Radiation in all directions
Example: Radio waves
from a transmitter.

Opening angle

High energy (relativistic) electrons– Laboratory frame:
Radiation pattern swept into a
narrow cone in the forward
direction = High brightness!
E = electron beam energy

2015 Cheiron School

Singaporeγ = 1400
Light Source.7 mrad
.04º

700 MeVAustralianγ = 6000
Synchrotron.2 mrad.01º

3 GeV

Spring-88 GeV2015 Cheiron Schoolγ = 16000.06 mrad.004º

Third Generation Sources: Undulator Insertion Devices
1st, 2nd Generation

3rd Generation: Insertion Devices

600x1012

Phot/s/0.1%bw

500
400
300
200
10000

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2000

4000
6000
Photon Energy

8000

10000eVεc = .665 E2BK>>1

K=0.934.λu[cm].B[T]2015 Cheiron School

K~1

~ Ne~ Ne x NP

~ Ne x NP2

2015 Cheiron School

Section of the Australian Synchrotron2015 Cheiron SchoolBeamline Design Goals• Deliver the required X-ray beam to the experiment:– Energy and bandwidth– Spot size
– Divergence/convergence• Preserve source characteristics eg intensity,brightness, coherence• Optimise signal / background• Be very stable and reproducible, in position, intensityand energy• Be safe to operate• Be user friendly to operate• Achieve all the above within a reasonable budget !
(Good Luck!)2015 Cheiron School

Hard X-ray Beamline: Si crystal monochromator E > 4 keV(Swiss-Norwegian beamline, ESRF)

Soft X-ray Beamline: Grating monochromator E < 2 keVElettra Schematic Beamline
2015 Cheiron SchoolMirrors for Synchrotron Beamlines• Deflection• Focusing• Harmonic Rejection• Power Reduction2015 Cheiron School

Critical Angle/Reflectivity with Energy:
Rhodium Coated Mirror Example
1 keV
10 keV
20 keV

Harder X-rays need moregrazing angles and longer
mirrors:
2 mm high beam needs:≤ 10 cm mirror at 1 keV≥ 80 cm mirror at 20 keV

Mirrors are a low pass filter

2015 Cheiron SchoolAn example beamline:
the AS Xray Absorption Spectroscopy Beamline

2015 Cheiron School

Brightness
2015 Cheiron SchoolCourtesy M. Ree, PLS

SR Development is towards higherbrightness – why?
Originally (2nd Generation sources) :• High intensity through slits or on sample;• High energy resolution:– Diffraction– Spectroscopy• Focusing optics:– smaller samples– Fluorescence mapping• Small vertical beam of 2nd and especially 3rd generationis good match to vertical dispersion & grazing optics.

2015 Cheiron School

SR Development is towards higher &higher brightness – part 2• Higher spatial resolution:– Tiny samples (protein crystals…)– Nano-structure materials– Non-homogeneous samples…

• Focusing optics image the source– Smaller focus (smaller and smaller xtals) or– More working dist for same focus size

• New imaging techniques – especiallycoherence based imaging• Many techniques
brightness/coherence
limited2015 Cheiron School

New Sources:XFELs

2015 Cheiron School

Next Step - X-ray Lasers? Yes  FELs
SACLA~ Ne~ Ne x NP

Spring-8

PhotonFactory~ Ne x NP2~ Ne2 x NP2

Degree of Coherence（％）

Light Source Performance

XFEL

100
1010-14110-13
10-120.1
0.0
1×103

10-15

10-11

SPring-810-10×10-31010

Photon Factory

×10910201030

Remarkable Features of XFEL producing <0.1 nm X-Rays◎ High Peak Brilliance◎ Narrow Pulse Width◎ High Degree of Coherence

T. Ishikawa, SPring-8
2015 Cheiron School

T. Ishikawa, RIKEN SPring-8 Center

8GeV SCSS XFELSACLA 1st beamline: 90m Undulator

Milestones
World-WideOpen Facility
The same proposal-review process as
SPring-8

T. Ishikawa,
2012
Cheiron SPring-8
School Tour2015 Cheiron School

“Diffract and Destroy”:
Single Shot Imaging at the FLASH Soft X-ray FEL
Diffraction patternfrom second pulse

A coherent diffraction pattern of the object
recorded from a single 25-femtosecond
FEL pulse.
~60 000 °K

Coherent Diffractive Imaging:no lens, no crystal
H. Chapman et al., Nature Physics 2, 839 (2006)

Reconstructed image: no signs ofdamage caused by the pulse.

First serial femtosecond crystallography
experiments at LCLS/AMO/CAMP - 7 A resolution
Chapman et al
Nature 470: 73 (2011)

Gas focussed liquid jet:
4μm diam., flow rate 10- 14 μl min, 10 ms/s
De Ponte et al., J. Phys. D 41, 195505 (2008)

λλ =6.2-6.9 Å, 1.8-2.0 keV
10-300 fs pulse duration
30 (60) Hz
1012 photons/pulse
900 J/cm2Dose/pulse: 300-700 MGy~ 7 μm diam.
~ 4 μm diam.

1800 (3600) patterns/min
5 TB in one nightRadiation damage-free datacollection
563 nmBeitlich et al., JSR (2007)
 on-line spectroscopyshows radiation damage inchloroperoxidase crystal at asynchrotron in seconds at alow dose rate (28 kGy/s)
2015 Cheiron School

Kern et al., Science (2013)
No radiation damage to metal cluster in
Photosystem II during diffraction at LCLS

Time-resolved pump-probe experiments on
photosensitive proteins
Best time-resolved MX (Laue, synchrotron) done by F. Schotte/Ph. Anfinrud
has 100 ps time resolution. With FELs this can be reduced to ps/hundreds offs.

Pump Laser

2015 Cheiron School

Coherent diffractive imaging of single particles
by the diffraction-before-destruction approachparticle injection- 1012-13 photons- 10 keV- 10 fs pulse

100 nmfocus~1021 W/cm2

diffraction
pattern

Measure structure before destroyed?
- biological nano-crystals- virus structures, virus genomes- non-crystallisable proteins: 60 %Calculations. in vacuum Neutze et al., Nature 2000

FELs: Many research areas
Femtosecond experiments- pump-probe experiments on atoms and molecules (femto-chemistry)- sum-frequency generation- serial crystallography

Interaction of ultra-intense XUV pulses with matter- multiphoton excitation of atoms, molecules, clusters…
- creation and characterizaton of dense plasmas- imaging of nano-objects and biological samples

Investigation of extremely dilute samples- photodissociation of molecular ions- highly charged ions
- mass selected clusters

Investigation of surfaces and solids-XUV laser desorption
surface dynamics
femto-magnetism
study of highly correlated materials
luminescence under FEL radiation
meV-resolution photon and photoelectron spectroscopy of surfaces andsolids with nm resolution

2015 Cheiron School

FELs are Great, BUT…
•

Only a few of them and only a few(at the moment one) experiments
at a time– Capacity very limited; difficult toaccess– Each experiment VERY expensive•

Technical challenges at every step
– Source, optics, samples detectors,data etc•••

SASE Process – every pulse
different
Can we make a brighter
synchrotron light source to “fill thegap” ?
Truly enable coherence-based
techniques on storage rings

2015 Cheiron SchoolBrightness
Gap ~105

Brightness Limit is a Diffraction Limited Source
Emittance characterises the brightness of a source; it is the product ofsource size and divergence in a particular dimension.
For SR from a single electron, the emittance/brightness is diffraction limited:

So wavelength corresponding to thediffraction limit for a particular emittance:

Real emittance is combination ofradiation emittance and real sourcesize/divergence:

2015 Cheiron School

10keV Diffraction LimitBrightest 3rd Generation Storage Ring Sources:• Horizontal emittance 3-20 nm.rad• Vertical emittance ~100 times less
• Very asymmetric beam in straightsections: Horizontal ~ 1mm FWHM
 Vertical ~ 10 μm• Far from diffraction limit in Horizontal@ 10keV• Close to diffraction limit in vertical2015 Cheiron School

How to Design a Brighter Ring?
The horizontal emittance is a characteristic equilibrium quantity for each storage ringelectron energy: E; angle per bending magnet: θ;

Lattice dependent quantity:

Emission of SR also reduces emittance – “natural emittance” of astorage ring is equilibrium between SR and energy spread.

Reduce energy (not too much or no X-rays)
Reduce angle of bending magnets
More synchrotron radiation

2015 Cheiron SchoolDiffraction Limited Storage Ring

If the "ultimate" target is a:"Diffraction Limited Source" for 10keV Photons:
We Need x ~ y ~ 10pmrad

Vertical emittance already there: challenge is:
Reduce horizontal or “natural” emittance ~100x∝2015 Cheiron School.

.ΓRound beam = A “Nicer” SourceCurrent 3rd Generation Ring2015 Cheiron SchoolDLSRWhat can be done to makesmall ?

Large ring with lots of cells, reduce electron beam energy
Most 3rd Generation are “double bend achromat” (DBA):

DBA Cell of the Australian Synchrotron

 many cells  large storage rings- ESRF: 32; APS: 40; Spring-8: 48
 High power “damping wigglers”: much more SR produced- NSLS II; PETRA III
2015 Cheiron School

Big is better?

2015 Cheiron School

Large rings, many bending magnets, reduce energy
Wavelength corresponding to the diffraction limit:2015 Cheiron School

What can be done to makesmall ?

Same size Ring, More Bending Magnets“New” Idea: multi bend achromat (MBA)

7BA (MAX IV)• Reduce dispersion and control beam size in the bending magnets• Achieved by refocusing beam ‘inside’ bending magnets:- need space• ‘Split’ bending magnets -> Multi Bend Achromats

2015 Cheiron SchoolTowards Diffraction Limited Storage Rings – MBA Lattices
Wavelength corresponding to the diffraction limit:Study

E (GeV)

Circumf. (m)εx (pm.rad)λDlx(Å)/E(keV)

PEP-X

4.52200111.4/9Tevatron

1162801.30.16/76

2015 Cheiron School

New Storage Ring Projects
PETRA III @ DESYBest emmittance today:
εh = 1 nm rad @ 6 GeV

MAX IV in Lund

NSLS II @ BNL

Under construction
εh = 0.2-0.3 nm rad @ 3.7 GeV

Under construction
εh = 0.55 nm rad @ 3 GeV

UpgradesAPS @ ANLESRF in Grenoble

Spring-8 in Hyogo, Japanεh = 0.07 nm rad @ 6 GeVεh = 0.1-0.15 nm rad @ 6 GeVεh = 0.11 nm rad @ 6 GeV2015 Cheiron SchoolEnjoy the Cheiron School!

Thanks to many people for slidesParticularly Edgar Weckert, DESY
2015 Cheiron School