1. MAXIM Webster Cash University of Colorado

3. Capella 0.0001”

4. Capella 0.000001”

5. AR Lac Simulation @ 100  as

6. AGN Accretion Disk Simulations @ 0.1  as Courtesy of Phil Armitage, U. Colorado and C. Reynolds, U. Maryland

7. Need Resolution and Signal If we are going to do this, we need to support two basic capabilities: Signal Resolution

8. X-ray Sources Are Super Bright Example: Mass Transfer Binary 10 37 ergs/s from 10 9 cm object That is ~10,000L  from 10 -4 A  = 10 8 B  where B  is the solar brightness in ergs/cm 2 /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!

9. Artist’s impression of Cyg X-1 (NASA) My Impression

10. 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

11. Pathlength Tolerance Analysis at Grazing Incidence A1 A2 S1 S2  A1 & A2 in Phase Here C       If OPD to be < /10 then

12. A Simple X-ray Interferometer Flats Detector

13. Wavefront Interference  d/L =  s (where s is fringe spacing) s

14. Optics Each Mirror Was Adjustable From Outside Vacuum System was covered by thermal shroud

15. X-ray Fringes 1.25keV Cash et al March 1999 0.5keV Gendreau, October 2002

16. Flats Held in Phase Sample Many Frequencies

17. As More Flats Are Used Pattern Approaches Image 2 4 8 16 32 12

18.  Parallel to Source Direction To focus Periscope Configuration Reduces Sensitivity to Baseline Each Periscope in the array is held to  sin  Keeps beam pointed in constant direction like thin lens

19. focus Periscopes allow for delay in each channel. Can sample full UV plane.

20. Periscope Requirements Even Number of Reflections With odd number of reflections, beam direction shifts with mirror tilt With even number, the mirrors compensate and beam travels in same direction.

21. Phase Shift Path Delay = h sin  h so h  < /10 for phase stability  if h~1cm then  < 10 -8 (2 milli-arcsec) This can be done, but it’s not easy.

22. Phase Delay d1d1 d2d2

23. There are Solutions This solution can be direction and phase invariant Dennis Gallagher has verified this by raytrace! Pointing can wander arcseconds, even arcminutes, and beam holds fixed!

24. Array Pointing 4 mirror periscopes solve problem of mirror stability But what about array pointing? Doesn’t the array have to be stable to 1  as if we are to image to 1  as?

25. Thin Lens Behavior As a thin lens wobbles, the image in space does not move Position on the detector changes only because the detector moves

26. Formation Flying If detector is on a separate craft, then a wobble in the lens has no effect on the image. But motion of detector relative to Line of Sight (red) does! Much easier than stabilizing array. Still the toughest nut for full Maxim. Variety of solutions under development.

27. Mirror FEM Mirror Face Mirror Back 3pt Ti Flexure Mount Optic w/Face Sheet Removed

28. Mirror Analysis Summary 1cZ Mirror Deformations (mm) 20gY Mirror Back Stresses (MPa)Mirror First Mode = 278 Hz

29. MAXIM Position Tolerances =1nm, F=20,000km, D=1km, m=30cm,  =1deg,  h=1  m DOFMirror Equation Periscope Equation Mirror Tolerance Periscope Tolerance X ±1.7nm ±4  m Y ±0.3mm± 0.5mm Z ±94.7nm±0.32m X-rot (yaw) ±6.9 arcmin ± 7.8 arcmin Y-rot (pitch) ±2.3 marcsec ± 10 arcsec Z-rot (roll) ±0.13 arcsec ±18.5 arcsec

30. Optical Bench FEM Flexure Fixed Mount Simplified Optics Mounts Main Bench “Daughter” Benches

31. Periscope Assembly Entrance Aperture (Thermal Collimator) Shutter Mechanism (one for each aperture) Assy. Kinematic Mounts (3)

32. Launch Configuration Layout Delta IV ø5m x L14.3m 24 Free Flyer Satellites (4 Apertures ea.) 1 Hub Satellite (12 Apertures) 1 Detector Satellite Ø4.75m

33. Aperture Locations (central area) 26 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18

34. 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.

35. Stars Simulation with Interferometer Sun with SOHO

36. Black hole imager black hole census black hole physics space interferometry The Beyond Einstein Program LIGO Chandra Swift MAP Hubble Science and Technology Precursors Dark Energy Probe optical imaging Constellation-X x-ray imaging LISA gravitational wave detectors Inflation Probe microwave background detection Black Hole Survey Probe hard x-ray detectors Big Bang Observer dark matter physics space interferometry, gravitational wave detection dark energy physics

37. Bottom Line Maxim can be built in an affordable way Achieving 0.1mas can be done with modest control in free-flying Full black hole imaging for under $900M Maxim is in the planning NRA for “Vision Mission Studies” coming out this week.