1. An X-ray Interferometry Technology Roadmap Keith Gendreau NASA/GSFC Webster Cash U. Colorado

2. MAXIM Requirements Flowdown SEU Science Objective MAXIM Approach Measurement Requirement Key Technologies Understand the ultimate endpoint of matter. To explore the ultimate limits of gravity and energy in the universe. Make a “movie” of a black hole, its accretion disk, and its jets. Map doppler and gravitational redshifts of important lines in the vicinity of a black hole. Angular Resolution: 0.3  as  rs ~ 2M 8 /D - 6M 8 /D Time Resolution ~ 1 hour 2  R s /c~10 hours Bandpass: 0.1-10 keV K-lines from Carbon to Iron E/  50 ASCA, Chandra, and XMM obs Area >1000 cm 2 ~10  Photons/frame (~10 Photons/pixel/frame) Diffraction limited optics >  Flat long and skinny Thermal /Mechanical Stability CTE ~< 10 -7 /K Precision Formation Flying X-ray CCDs Larger Arrays of ~< 10 micron pixels Fast Readout (msec) ~0.1  as Line-of-Sight alignment knowledge. 100,000 finer than HST

3. Basic MAXIM Design Each Channel Consists of 2 flats Primary mirrors determine baseline Secondary mirrors combine channels at detector. To implement this basic design, you choose how to group the mirrors. Fringes Form Here Baseline

4. Original MAXIM Implementations MAXIM Pathfinder Full MAXIM- the black hole imager “Easy” Formation Flying Optics in 1 s/c act like a thin lens Nanometer formation flying Primaries must point to milliarcseconds

5. Improved MAXIM Implementation Group and package Primary and Secondary Mirrors as “Periscope” Pairs “Easy” Formation Flying (microns) All s/c act like thin lenses- Higher Robustness Possibility to introduce phase control within one space craft- an x-ray delay line- More Flexibility Possibility for more optimal UV-Plane coverage- Less dependence on Detector Energy Resolution Each Module, self contained- Lower Risk.

6. An Alternate MAXIM Approach: Normal incidence, multilayer coated, aspheric mirrors Optics demonstrated today with 1-2 Angstrom figure Multilayer Coatings yield narrow bandpass images in the 19-34 Angstrom range Could be useful as elements of the prime interferometer or for alignment Offer focusing and magnification to design May require tighter individual element alignments and stiffer structures.

7. Technologies: Status, Metrics, Mutual Needs Technology Has there been a demo? Metrics Will we test on ground? Current Status Vs. Requirement Is it a big leap? Related Missions MirrorsYes > /100 YesNeed longer, skinnier to maximize area/mass NoSI, TPF*, NGST, SIM Thermal control YesMaintain > /100. TBD from LOS YesMission SpecificNoSIM*, SI, TPF, NGST, SPECS, LISA*,… Formation Flying (a system requiring many components) Yes, but…  m formation flying control Partial-Autonomy required. -Need higher precision -Metrology exists at component level -Must work at longer distances YesSI*, TPF*, LISA, XEUS, Grace, MMS, Starlight, Darwin,… Line-Of-Sight (LOS) NoSee Other Slide PartialSee Other SlideYes All  as missions: SI, iARISE, & TPF, GP-B

8. Technical Components: Mirror Modules Grazing Incidence Mirrors Grazing Incidence loosens our surface quality and figure requirements by 1/sin  Flatness >  “Simple” shapes like spheres and flats can be made perfect enough At grazing angles, mirrors that are diffraction limited at UV are also diffraction limited at X-ray wavelengths Long and Skinny Bundled in Pairs to act as “Thin Lens” Thermal/mechanical Stability appropriate to > 

9. What would one of these modules look like? m msin(g) m/6 Gap~msin(g) Pitch Control msin(g) 3/2m+d m/3 + msin(g) 2(w+gap)+msin(g) By 2(w+gap)+msin(g)+m/3+actuator+encoder ASSUME: w+gap~5 cm Encoder+encoder~5cm Sin(g)~1/30 -->(10cm+m/30)x(15cm+m/3+m/30) -->m=30cm-> 13cmx26cm

10. Technical Components: Arrays of Optics Baselines of > 100 m required for angular resolution. Formation flying a must for distance >~20 m. Miniaturization of ALL satellite subsystems to ease access to space. S/C Control to 10  m- using “periscope” configuration (metrology to better than 1  m). –A system spanning from metrology to propulsion Individual optic modules are thin lenses with HUGE fields of view

11. Technical Components: The detector In Silicon, the minimum X-ray event size is ~1  m Large CCD arrays possible with fast readout of small regions. Pixel size determines the focal length of the interferometer F~s/  res –10  m pixels -> Focal lengths of 100s to 1000s of km. Formation Flying Necessary –Huge Depth of focus loosens longitudinal control (meters) –Large array sizes loosen lateral control (inches). –High angular resolution requirement to resolve a black hole: The Line-Of-Sight Requirement.

12. Technical Components: Line-of-Sight We must know where this telescope points to 10s- 100s of nanoarcseconds –Required for ALL microarcsecond imagers The individual components need an ACS system good to only arcseconds (they are thin lenses) We only ask for relative stability of the LOS- not absolute astrometry This is the largest technical hurdle for MAXIM- particularly as the formation flying tolerance has been increased to microns

13. dX dd Using a “Super Startracker” to image reference stars and a laser beacon. Super Star Tracker Sees both Reference stars and the beacon of the other space craft. It should be able to track relative drift between the reference and the beacon to 0.1 microarcseconds. oo Both the optics spacecraft and the detector spacecraft can rotate to arcseconds- they are “thin lenses” Imaging problems occur when one of these translates off the line of sight We need to KNOW dx/F to 0.1 microarcseconds. AND We need to know a reference direction to the same level The CONTROL of the Line-of-Sight is driven by the detector size. Beacon F

14. Options to Determine Line-Of-Sight All options require beacons and beacon trackers to know where one s/c is relative to another. OPTION 1: Track on guide stars –Use a good wavelength (radio, optical, x-ray) –Use a good telescope or an interferometer OPTION 2: Use an inertial reference –Use a VERY good gyroscope or accelerometer –GP-B

15. Summary of Key Technical Challenges The mirrors and their associated thermal control are not a tremendous leap away. “Periscope” implementation loosens formation flying tolerance from nm to  m. This makes formation flying our second most challenging requirement. Determination of the line-of-sight alignment of multiple spacecraft with our target is the most serious challenge- and MAXIM is not alone with this.

16. Using Stars as a Stable Reference A diffraction limited telescope will have a PSF ~ /D If you get N photons, you can centroid a position to /D / N 1/2 Nearby stars have  as and mas structure Stars “move” so you need VERY accurate Gimbals –Parallax (stars @500 pc can move up to 40  as in a day) –Aberration of Light (as big as 40  as in a minute) –Stellar orbits, wobble due to planets –Other effects…

17. An Optical Star Tracker A “reasonable” size telescope (<1m diam.) @ optical wavelengths will require 10 12 photons to centroid to 0.1  as. Practical limits on centroiding (1/1000) will need large F numbers Lack of bright stars requires complicated gimbals to find guide stars HST would barely squeak by with 15th mag stars

18. An 100  as X-ray Star Tracker A 1 m diffraction limited X-ray telescope (probably an interferometer) would need only 10 6 photons to centroid to 0.1  as A 1000 cm 2 telescope would get ~ 100 photons/sec from reasonable targets. –10 4 second integration times needed to get enough photons –This is too big…. And even then, there are not that many targets

19. An 10  as X-ray Star Tracker A 10 m baseline X-ray interferometer would need only 10 4 photons to centroid to 0.1  as A 1000 cm 2 telescope would get ~ 100 photons/sec from reasonable targets. –100 second integration times –This is too big….possibly… –And even then, there are not that many targets

20. An Optical Interferometer Eg. SIM Metrology at picometers demonstrated in lab OPD control to nanometers Expensive?

21. Local Inertial References Superconducting Gyroscopes –Eg. GP-B Gyros will have drift < 1/3  as /day Superconducting Accelerometers –Eg. UMD accelerometer sensitive to 10 -15 m/s 2 Kilometric Optical Gyroscope –Eg. Explored for “Starlight”- a BIG laser ring gyroscope Atomic Interferometer Gyroscopes –Like a LRG, but with MUCH smaller wavelengths –Laboratory models ~10  as/sec drifts –ESA proposed “Hyper” mission

22. Superconducting Gyroscopes Capitalize on GP-B technology –Of all our options, this one has had a CDR Improve with better squids –Readout is white noise limited Improve by requiring only hours-days of stability at a time –Make the rotor have a larger moment- easier to read, but less stable over long times Use NGST/ConX Cryocoolers to replace cryogen –Get rid of “Lead bags” –Make lighter No need to find stars (no Gimbals)

23. Superconducting Accelerometers 10 -15 m/s 2 sensitivity exist now Need integrators Need higher sensitivity, unless used with other things

24. Kilometric Optical Gyroscopes A Laser-Ring-Gyroscope with BIG area/perimeter ratio –Resolution ~ /(area/perimeter) –Use area bounded within space between multiple spacecraft Proposed for Starlight- but rejected in the end –“cost” and “technical” reasons

25. Atomic Interferometer Gyroscopes Same principle as a LRG, but use matter waves to make many orders of magnitude smaller Benchtop demonstrations in lab are as good as best LRGs (10  as/sec)- but should be much better ESA proposed mission “Hyper” based on these to do GR physics.