x -ray interferometrywcash/maxim/documents/niac01.pdf · x -ray sources are super bright example:...
TRANSCRIPT
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X-ray Interferometry
Webster CashUniversity of Colorado
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Collaborators
• Ann Shipley, Karen Doty, Randy McEntaffer, & Steve Osterman at CU
• Nick White – Goddard
• Marshall Joy – Marshall
• David Windt and Steve Kahn - Columbia
• Mark Schattenburg - MIT
• Dennis Gallagher – Ball Aerospace
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X-ray Telescopes
X-ray telescopes are sensitiveto material at millions of degrees.
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Capella 0.1”
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Capella 0.01”
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Capella 0.001”
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Capella 0.0001”
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Capella 0.00001”
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Capella 0.000001”
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AR LacSimulation @ 100µas
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AGN Accretion DiskSimulations @ 0.1µas
C. Reynolds, U. Colorado
M. Calvani, U. Padua
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Need Resolution and Signal
If we are going to do this, we need to support two basic capabilities:
• Signal
• Resolution
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X-ray Sources Are Super Bright
Example: Mass Transfer Binary1037ergs/s from 109cm object
That is ~10,000L¤ from 10-4A¤ = 108 B¤where B¤ is the solar brightness in ergs/cm2/s/steradian
Brightness is a conserved quantity and is the measure of visibility for a resolved object
Note: Optically thin x-ray sources can have very low brightness and are inappropriate
targets for interferometry. Same is true in all parts of spectrum!
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Minimum Resolution
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Status of X-ray Optics
• Modest Resolution– 0.5 arcsec telescopes
– 0.5 micron microscopes
• Severe Scatter Problem– Mid-Frequency Ripple
• Extreme Cost– Millions of Dollars Each
– Years to Fabricate
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Classes of X-ray Interferometers
Dispersive
Non-Dispersive
Elements are Crystals or Gratings
Elements are Mirrors & Telescopes
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Achieving High Resolution
R=λ/20000D
R in Arcsecλ in AngstromsD in Meters
Michelson Stellar Interferometer
Use Interferometry to Bypass Diffraction Limit
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Creating Fringes
Requirements• Path Lengths Nearly Equal
• Plate Scale Matched to Detector Pixels
• Adequate Stability
• Adequate Pointing
• Diffraction Limited Optics
dD
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θ
δ
sin1 =B
( )θ2cos12 BB =
( )[ ]θδ
θ
θδsin2
sin
2cos121 =
−=−= BBOPD
θ
λδ
sin20<
( )θθ
λ
cossin20<Baselined
( )θ
λ2sin20
<focald
Pathlength Tolerance Analysis at Grazing Incidence
A1 A2
S1S2
δδ
A1 & A2 in Phase Here
C
θ
θ
θ
Β1Β2θ
If OPD to be < λ/10 then
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A Simple X-ray Interferometer
Flats Beams Cross
Detector
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Wavefront Interference
θ=d/L
λ=θs (where s is fringe spacing)
d
Ls
λ=s
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Optics
Each Mirror Was AdjustableFrom Outside Vacuum
System was covered by thermal shroud
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Stray Light Facility MSFC
16m
Source, filter and slit
100m
Interferometer CCD
Used Long Distance ToMaximize Fringe Spacing
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CCD Image @ 1.25keV
2 Beams Separate 2 Beams Superimposed
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Fringes at 1.25keV
Profile Across Illuminated Region
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Test Chamber at CU
Ten Meter Long VacuumChamber for Testing
Came on-line early May
EUV results goodUpgrade to x-ray next
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Actual Image at 30.4nm
Image of SlitReconstructed from 4 azimuths
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MAXIMThe Micro Arcsecond X-ray Imaging Mission
Webster Cash ColoradoNicholas White GoddardMarshall Joy Marshall
http://maxim.gsfc.nasa.gov
PLUS Contributions from the Maxim Team
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Goal
Resolve the winds of OB stars: What kind of shocks drive the x ray emission?Resolve pre-main sequence stars: How does coronal activity interact with disk?I ma g e o f c ent er of Mi l ky Wa y : Detect and resolve accretion disk? Detailed images of LMC, SMC, M31: Supernova morphology and star formation in other settingsImage jets, outflows and BLR from AGN: Follow jet structure, search for scattered emission from BLRDetailed view of starbursts: Resolve supernovae and outflowsMap center of cooling flows in clusters: Resolve star formation regions?Detailed maps of clusters at high redshift: Cluster evolution, cooling flows
Image Event Horizons in AGNS: Probe Extreme Gravity Limit
Maxim:A Few Science Goals
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Flats Held in PhaseSample Many Frequencies
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As More Flats Are UsedPattern Approaches Image
2 4 8
16 3212
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rces in the same e source that is
di splaced to the lower left. The image on the right shows 9000 total events for ity of the higher
energy source. Even though the higher energy source is in the first maxima of the other, the two can still be easily distinguished.
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Clockwise from upper left: Probability distribution; 100 photons randomly plotted; 9000 photons; and 5000 photons.
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tion of the continuum and the contribution of photons with energies between 5-6keV to
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These figures show the probability distribution for the 1keV portion of the continuum and the contribution of photons with energies between 0-1keV to the data simulation.
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T he probability distribution on the left represents a continuum of energies between 1keV and 6keV. In the right figure, 16000 random events were recorded according to this distribution.
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Stars
S imu lat ion with Int erf erome t er
Su n wi th SOH O
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3C273 with Chandra
Simulation with Interferometer
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Four Difficult Areas
• Fabrication of Interferometer
• Formation Flying– Hold Detector Craft in Position
• Pointing– Hold Interferometer on Target
• Internal Metrology– Hold Mirrors Flat and In Position
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Ma xim
0.1µ10,000cm2 Eff ect ive Ar ea0.4 -7. 0 k eV
“T he Bla ck Hol e I mag er ”
DETECTORSPACECRAFT
CONVERGERSPACECRAFT
200M
COLLECTORSPACECRAFT(32 PLACESEVENLY SPACED)
10KM
5000KM
CONSTELLATIONBORESIGHT
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Maxim Pathfinder
100µas Resolution100cm2 Effective Area0.4-2.0keV + 6keV
Two SpacecraftFormation Flying at450km Separation
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2.5m
10m
Optics SpacecraftCarries: -
Finder X ray Telescopes
Laser Ranging System
Size: 2.5x2.5x10mPitch&Ya w St ability: 3x10- 4 arcsecPitch&Yaw Knowledge: 3x10-5 arcsecRoll Stability: 20 arcsecPosition Stability: -----
Detector SpacecraftCarries: X-ray Detector Array
Laser Retro ReflectorsPrecision Thrusters
Size: 1x1x1mPitch&Yaw Stability: 20 arcsecRoll Stability: 20 arcsecLateral Stability: 5mmLateral Knowledge: 50 micronsFocal Stability: 10 meters
1m
1m
Sepa
rati
on 4
50km
Maxim Pathfinder Mission Concept
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P rime Interferometer
Y aw Sensor
Optics CraftF ront View
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Consider, instead, line F.Mount the visible light interferometer on structuresat the ends of line F. They then maintain 1nm precisionwrt to guide star that lies perpendicular to F. This definespointing AND maintains lateral position of convergers. (40pm not needed in D and E after all.)A, B, C, D and E all maintain position relative to F.
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Detector
• En e rgy Re sol uti on Nec ess ary fo r F rin ge I nve rsi on
• CC D i s a deq uat e
• To get large field of view use imaging quantum calorimeter
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Metrology
Tightest Tolerance is Separation of Entrance Apertures
d = λ/20θ for tenth fringe stability
At 1keV and 2deg, d=1.7nmAt 6keV and 0.5deg, d=1.1nm
Requires active thermal control and internal alignment
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Laser
Collimated BeamsCross at 450km
Collimator
Laser BeamSplit and Collimated
Optics Craft450km toDetector Craft
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I nterference Pattern
I nterference Pattern
Detection of Pattern
Fringes have 14cm period at 450km
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Need stability and information wrt to the celestial sphere at level of required resolution.
L2 or Fly-away orbit probably necessary
Baseline design calls for two stellar interferometers.One each for pitch and yawSIM class interferometers more than adequate
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Delta IV (H) 5m diameter x 19.8m long
Launch Fairing Removed
Detector Spacecraft(2.2m)
Optics Instruments(10m)
Optic Spacecraft Systems(2.2m)
Baffling
LAUNCHCONFIGURATION
15.5 m
16.4 m
Payload
Spacecraft
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ORBIT CONFIGURATION
Optic Spacecraft
Detector Spacecraft
Solar Array(7 m^2, projected area)
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Stowed
Orbit
Payload
Spacecraft
Spacecraft Subsystems are mounted inthis volume
FixedSolar Array
(6m^2 shown)
DETECTOR SPACECRAFT
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Maxim Design
DETECTORSPACECRAFT
CONVERGERSPACECRAFT
200M
COLLECTORSPACECRAFT(32 PLACESEVENLY SPACED)
10KM
5000KM
CONSTELLATIONBORESIGHT
Hub Spacecraft
SPACECRAFTDELAY LINE
Hub Craft Converger Craft Delay Craft
Light from Star
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Full Maxim
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Maxim Limitations
• If pri mar y f lat s a re on sep ara te spa ce c raf t the n t hey ca n b e f low n f art her ap art . Resolution increases.
• Limited by visible light aspect from stars– They’re all resolved at 30nano-arcsec!
• Find non-thermal visible sources
• Use x-ray interferometry for aspect too.
• Solve aspect problem and reach 10-9 arcsec
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Integrated System Modeling
Ball Aerospace Technologies Corporation
M. Lieber
D. Gallagher
Will lead to single most important tool in developmentand definition of x-ray interferometry
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• Integrated modeling seamlessly combines the subsystem models from well established software tools.
• Allows one to rapidly study parameter interaction of disparate variables from different disciplines. Integrated models facilitate GUI development - muliti-user system tool.
• Standard interfaces minimizes errors and miscommunications between disciplines
Structure Design
Structure Design
Control System Design
Control System Design
Optics/Sensor Design
Optics/Sensor Design
NASTRANNASTRAN Simulink/MATLAB
Simulink/MATLAB CODE V/ various
CODE V/ various
STRUCTURE OPTICS/SENSOR
ThermalDisturbances
ThermalDisturbances
MechanicalDisturbances
MechanicalDisturbances
Optical ErrorsOptical Errors
TRASYS/SINDA
TRASYS/SINDA
MATLABMATLAB
CODE VCODE V
MODELINGTOOLS
DESIGN PARAMETERS
ENVIRONMENTINPUTS
SYSTEM PERFORMANCEVS.
SCIENCE METRICS
SensorNoise
SensorNoise
MATLABMATLAB
SYSTEM MODELSimulink/MATLAB
CONTROLS
Integrated End-to-End Modeling Environment
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Ex ample of MAXIM Pathfinder
Maxim Pat hfi nder I M
2
1
Wavefront & tilt sensor models
Structural dynamics
Telescope mechanism tip/tilt and
wavefront control systems
Spacecraft attitude control
Signal processing
Optics model
Image processing
Imaging sensor models3
2
1
In1
sav_psf
To Workspace2Sp arse
array
Sparse
array
Optical raybundle1
RB offsets
Deform mapOut3
Offsets1
RB offsets
Deform mapOut3
Offsets
Image plane
[ttt,uuu]
[ttt,uuu2]
u_surf2
u_surf1
1
Out1
Sparse reflective mirror4
Sparse reflective mirror3
Sparse reflective mirror2
Sparse reflective mirror1{a1}
{b1}
[c4]
[c3]
[c2]
[c1]
{b1}{a1}
[c4]
[c3]
[c2]
[c1]
2
Opticsmotion
1
Ray bundle
Optical subsystem
• Structures, optics, controls, signal processing, disturbances
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Optical Toolbox:Key Element of Optical Performance Modeling
• Geometric ray trace• Diffraction analysis (PSF outputs)• Easy introduction of mirror distortions from thermal or
vibration• Optics tied to NASTRAN structural model• Active control modeling of metrology system and active
optics• Interfaces with imaging and detection modules
sav_psf
To Workspace2Sparse secondary mirror
array
Sparse primary mirror
array
Optical raybundle1
RB offsets
Deform mapOut3
Offsets1
RB offsets
Deform mapOut3
Offsets
Image plane
[ttt,uuu]
[ttt,uuu2]
u_surf2
u_surf1
See next slide
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MAXIM Pathfinder PSFs with Different Number of Optical Elements
2 segments
4 segments
32 segments
PSF Image Log image
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MAXIM Physical Model
MAXIM Integrated Model
Celestrial objects
Detector S/C
Converger and Delay Line S/C
Collectors & Hub S/C
Command and Control
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MAXIM System Modeling Leveraged From NASA and Other Programs
GSFC - Expertise and models for formation flying - FF lab
Optical metrology - Ball/GSFC Cross Enterprise contract, Ball/JPL Starlight program
Integrated modeling environment and MATLAB/Simulink toolset -NGST, TPF, VLT
Wavefront control - see next slide
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Example Wavefront Control Modeling -Initial Phase Map of NGST
10 20 30 40 50 60
10
20
30
40
50
60
10 20 30 40 50 60
10
20
30
40
50
60
[ x-decenter y-decenter piston tip tilt clocking]
• RMS random = primary segments
[ 1e-4 1e-4 4e-5 1e-5 1e-4 0]
• Secondary = offsets
[ x-decenter y-decenter piston tip tilt clocking]
[ 1e-3 5e-4 1.5e-5 -3e-5 8e-4 0]
Random errors for 36 segments
1 2 3 4 5 6-4-202468
10x 10-4
x-decenter
y-decenter
piston
tip
tilt
• Wavefront control tools from NGST program and extensive work on phase retrieval by JPL
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Status: X-ray Interferometry in NASA Planning
Structure and Evolution of the Universe (SEU) RoadmapMaxim Pathfinder Appears as Mid-Term Mission
Candidate Mission for 2008-2013Maxim Appears as Vision Mission
Candidate Mission for >2014
McKee-Taylor ReportNational Academy Decadal Review of AstronomyReleased May 19, 2000Prominently Recommends Technology Development
Money for X-ray Interferometry
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“X-ray Roadmap” to Image a Black Hole
Do they exist?
2000 2008 2014 2020
X-ray Interferometry Demonstration
Black hole Imager!
Where are they?
Conditions in the inner disk
ROSATEinstein
ASCARXTE
Imaging
Spectroscopy
1000 times finer imaging
MAXIM Pathfinder
100 cm2
2 m baseline100 µarc sec
MAXIM
1000 cm2
100-1000 m baseline100 nas
Million times finer imaging
Chandra
100-1000 cm2
0.5 arc sec
XMMAstro-E
Constellation-X
3 m2
Indirect imaging via spectroscopy
Optimize MAXIM
Parameters
Spectrally Resolved
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Plan• Technology Development
– Start with NIAC and SR&T Funding– Mission Specific Funding
• Maxim Pathfinder– New Start 2008– Develop & Test Technology for Maxim
• MAXIM– Five Years after Pathfinder
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The Black Hole Disney, 1979
We have already found this black hole and will have thesepictures before 2020.