1. XRT Performance Update
Edward DeLuca

2. Solar B X-Ray Telescope
Science Goals
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Solar B X-Ray Telescope

3. Solar B X-Ray Telescope
Science Goals
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Solar B X-Ray Telescope

4. Solar B X-Ray Telescope
Science Goals
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Solar B X-Ray Telescope

5. Requirements Flowdown
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6. Solar B X-Ray Telescope
Mirror Properties
Optimized Polynomial Design
Constraints: Focal Length, Pixel Size, FOV, Resolution
Goal: 2” resolution for the full sun FOV
Low Scattering
Surface roughness < 5A RMS
Temperature sensitivity < 1MK (cool coronal plasma
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Solar B X-Ray Telescope

7. Solar B X-Ray Telescope
Mirror Status
Mirror polishing is proceeding at Goodrich.
We expect the mirror to meet or exceed all requirements.
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Solar B X-Ray Telescope

8. Solar B X-Ray Telescope
Entrance Filter
Requirements
White Light Transmission < 10 -6
Heat Rejection
5 year on orbit survival
X-Ray transmission > 0.7 from 1-60A
Properties
1600 A Al
2500 A Polyimide
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Solar B X-Ray Telescope

9. Solar B X-Ray Telescope
Focal Plane Filters
Requirements
White Light Transmission < 10 -6
5 year on orbit survival
Temperature Diagnostics from 1 to > 20 MK
Morphology for T < 1MK
Properties
Science filters are on polyimide or free standing
Simple proven design
Testing/Verification
Environmental
Transmission
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Solar B X-Ray Telescope

10. Solar B X-Ray Telescope
Filter Status
Environmental tests have been performed and flight filters have been chosen.
The flight focal plane filters have been received from LUXEL.
Initial light leak tests have been done on all the flight fp filters.
The flight fp filters are at the XACT Facility in Palermo Italy for calibration tests.
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Solar B X-Ray Telescope

11. Solar B X-Ray Telescope
Ordered Filter Set
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12. Optical Paths Overview
2700 mm
X-RAY
White Light
Things to Note:
Only one optical path is used at a time.
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Solar B X-Ray Telescope

13. Solar B X-Ray Telescope
Mirror Calibration
SAO - Centroid Detector Assembly (CDA)
Focus Determination
Visible light optical axis relative to X-Ray
XRCF
Encircled Energy On-Axis
Encircled Energy Off-Axis
Effective Area
PSF and Effective Area Off-Axis
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Solar B X-Ray Telescope

14. Solar B X-Ray Telescope
Mirror Calibration
XRCF Available Lines
C-K keV 44.7A
O-K keV 23.6A
Cu-L keV 13.3A
Al-K 1.49 keV 8.3A
Ag-L 2.98 keV 4.2A
Ti-K 4.51 keV 2.7A
Cr-K 5.41 keV 2.3A
Fe 6.4 keV 1.9A
Not all lines will be used for all measurements.
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Solar B X-Ray Telescope

15. Solar B X-Ray Telescope
Mirror Requirements
Focal Length /- 5mm
Bandwidth 0.2 to 6.0 keV
Image Performance 68% encircled energy within keV at focal plane
FOV 35 arcmin
Effective Area > keV & 1 keV
Wings of On-Axis PSF keV signal at 1 arcmin < 3x10-5 peak flux.
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Solar B X-Ray Telescope

16. Visible Light Optic Requirements
Focal Length /- 2mm
Central Wavelength /- 20 A
Bandpass <120A FWHM
Resolution <2” half power dia.
FOV >30 arcmin
Co-Alignment <0.5 arcmin
Confocality w/ GI optic +/- 150 microns
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Solar B X-Ray Telescope

17. Filter Calibration Plan
Shadowgraphs
Filters are scanned with a mosaic of exposures at a single energy to measure thickness and uniformity
References
Barbera, M. et al 1996 DOC # OAPA-R5-1996, Sept
Collura, A. et al SPIE 2808, 134.
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18. Solar B X-Ray Telescope
Shadowgraphs
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19. Solar B X-Ray Telescope
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20. Solar B X-Ray Telescope
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21. Solar B X-Ray Telescope
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22. Solar B X-Ray Telescope
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23. Solar B X-Ray Telescope
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24. Solar B X-Ray Telescope
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25. Solar B X-Ray Telescope
Thin Be Shadowgraph
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26. Solar B X-Ray Telescope
Medium Be Shadowgraph
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27. Solar B X-Ray Telescope
Thick Be Shadowgraph
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28. Solar B X-Ray Telescope
Energy Scans
Energy scans will measure the transmission vs. energy.
These measurements are taken at one or two points on the filter.
If time permits opacity at 304A will be measured (1e-6 lower limit).
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Solar B X-Ray Telescope

29. Energy Scans AXAF Example
Collura, A. et al 1996 SPIE 2808, 134.
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Solar B X-Ray Telescope

30. Solar B X-Ray Telescope
Conclusions
XRT will provide high resolution broadband imaging of the corona for the Solar B mission.
The goal of understanding the relationship between photospheric driving and coronal dynamics requires a telescope that can image the response at a wide range of temperatures.
The high throughput of XRT will allow us to follow the coronal evolution with great accuracy.
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Solar B X-Ray Telescope

31. Solar B X-Ray Telescope
Filter Transmission
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32. Solar B X-Ray Telescope
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Solar B X-Ray Telescope

33. Solar B X-Ray Telescope
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34. Solar B X-Ray Telescope
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35. Solar B X-Ray Telescope
XRT Exposure Times
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