MAXIM The Micro-Arcsecond X-ray Imaging Mission

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MAXIMThe Micro-Arcsecond X-ray Imaging Mission
Webster CashUniversity of Colorado
Imaging a Black Hole
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Collaborators

• Ann Shipley, Randy McEntaffer, Steve Osterman at
  CU
• Keith Gendreau, Nick White Goddard
• Marshall Joy Marshall
• Dennis Gallagher, Mike Leiber Ball
• The Maxim Team http//maxim.gsfc.nasa.gov

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Maxim Heritage

• 1995 Future Concepts for X-ray Astronomy Chosen
  by Competition
• Tananbaum, White, Gorenstein, Cash
• 1996 Leicester Meeting -- Observatories for
  21st Century
• Con-X and Xeus emerged as leaders
• First Public Presentation on X-ray Interferometry
  (Deeper into 21st)
• 1998 Formation of Maxim Committee
• Reviewed Feasibility
• Set Imaging of Black Hole as Long Term Goal
• 1999 Creation of Fringes
• Support from NASA Institute for Advanced Concepts
• 2000 Support from SEU and Decadal Committee

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Clusters of Galaxies
Galaxies
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Star Clusters
20
AGN Jets
18
16
AGN BLR
GRB Afterglow
AGN Event Horizons
14
Interacting Binaries
Log Diameter (cm)
12
Stellar Coronae
XRB Orbits
10
CV
XRB Disks
8
6
NS Disks
0
1
2
6
5
4
3
9
8
7
10
Log Distance (pc)
5
10
Going Deep!
Earth
9
8
Jupiter
7
Binary Pulsar
6
Sun
Log(Rc2/GM)
5
Galaxies
4
Sirius B
3
BLR M87
2
Strong Gravity
1
Crab
SgrA/M87
CygX-1
Event Horizon
0
6
4
2
-6
-4
-2
0
-8
-10
-12
Log Resolution (arcsec)
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Capella 0.1
7
Capella 0.01
8
Capella 0.001
9
Capella 0.0001
10
Capella 0.00001
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Capella 0.000001
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AR LacSimulation _at_ 100mas
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NASA/Dana Berry
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AGN Accretion DiskSimulations _at_ 0.1?as
Courtesy of C. Reynolds, U. Maryland
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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 Binary 1037ergs/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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Artists impression of Cyg X-1 (NASA)
My Impression
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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

Need Easier Approach
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Pathlength Tolerance Analysis at Grazing Incidence
A1
A2
q
A1 A2 in Phase Here
If OPD to be lt ?/10 then
q
B2
q
B1
q
C
S2
S1
d
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A Simple X-ray Interferometer
Flats
Detector
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Wavefront Interference
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Optics
Each Mirror Was Adjustable From Outside
Vacuum System was covered by thermal shroud
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X-ray Fringes
0.5keV Gendreau, October 2002
1.25keV Cash et al March 1999
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Flats Held in PhaseSample Many Frequencies
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As More Flats Are UsedPattern Approaches Image
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On the left is the probability distribution
function for two sources in the same field of
view. The central source has an energy half that
of the source that is displaced to the lower
left. The image on the right shows 9000 total
events for this system with the lower energy
source having twice the intensity 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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Stars
Simulation with Interferometer
Sun with SOHO
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Maxim
The Black Hole Imager
0.1?as Resolution 10,000cm2 Effective
Area 0.4-7.0 keV
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Maxim Pathfinder
100?as Resolution 100cm2 Effective
Area 0.4-2.0keV 6keV
Two Spacecraft Formation Flying at 450km
Separation
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MAXIM Pathfinder Stowed Internal Metrology Not
Shown
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MAXIM Pathfinder in Deployed Configuration
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Primary and Secondary Optical Ring Layout
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Detailed View of Primary and Secondary Optical
Rings
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Effect of Tilt
0.25
0.12
0.12
0.2
0.1
0.1
0.08
0.08
0.15
Percent encircled energy
Percent encircled energy
Percent encircled energy
0.06
0.06
0.1
0.04
0.04
0.05
0.02
0.02
0
0
0
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.05
0.1
0.15
0.2
0.25
0.3
0.35
Angular distance from peak (mas)
Angular distance from peak (mas)
Angular distance from peak (mas)
-3
-3
-6
-2
-2
-4
-1
-1
-2
0
0
0
1
1
2
2
2
4
3
3
6
-3
-2
-1
0
1
2
3
-3
-2
-1
0
1
2
3
Angular coordinates (mas)
Angular coordinates (mas)
-6
-4
-2
0
2
4
6
Angular coordinates (mas)
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MAXIM Structural Dynamics Model

• Frequency response curve shows first 50
  structural modes
• Damping of 0.5 assumed for all modes
• Transfer function from RW force inputs to x and y
  tilt (2 curves) at focal plane - only largest TF
  in tip/tilt shown.
• Thermal, RW and thruster disturbances to
  structural stability

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First 5 Structural Mode Shapes
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Tackling Full Maxim --- The Periscope
Configuration
Keeps beam pointed in constant direction like
thin lens
Reduces Sensitivity to Baseline Each Periscope in
the array is held to l/20siny ? 10m
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Periscopes allow for delay in each channel. Can
sample full UV plane.
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Integrated Mission Design CenterGoddard Space
Flight Center
Delta IV 5m X 14.3m fairing
Delta IV Heavy 5m X 19.1m fairing
Propulsion/Hub SpaceCraft
Sta. 7600
Delta IV 5m X 14.3m fairing
Sta. 4300
Hub SpaceCraft/Detector SpaceCraft
C.G. Sta. 2500
Sta. 1550
Propulsion/Hub SpaceCraft
P/L Sta. 0.00
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Mission Sequence
1 km
Science Phase 2 High Resolution
Science Phase 1 Low Resolution
Launch
200 km
20,000 km
Transfer Stage
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Component LayoutDetector
Solar Array (4.5 m2)
Comm Antenna (Ground/SpaceCraft 0.5 m)
Thermal Shade (2.3 m2)
Comm Antenna (S/C to S/C 0.3 m)
Comm Antenna (Ground/SpaceCraft 0.5 m)
CCD Electronics
CCD Camera
LOS laser receiver
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Hub/Detector Sensor Configuration
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Status X-ray Interferometry in NASA Planning
McKee-Taylor Report National Academy Decadal
Review of Astronomy Released May 19,
2000 Prominently Recommends Technology
Development Money for X-ray Interferometry Stru
cture and Evolution of the Universe (SEU)
Roadmap Major Goal of the Beyond Einstein
Initiative Near Term Technology Program
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X-ray Roadmap to Image a Black Hole
1000 times finer imaging
Imaging
Optimize MAXIM Parameters
MAXIM Pathfinder
Million times finer imaging
MAXIM
100 cm2 2 m baseline 100 marc sec
Constellation-X
Spectroscopy
1000 cm2 100-1000 m baseline 100 nas
ASCA RXTE
3 m2 Indirect imaging via spectroscopy
Spectrally Resolved