The X-Ray Telescope for Solar-B Results of the Calibration Tests and Predicted Performance

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The X-Ray Telescope for Solar-BResults of the
Calibration Tests and Predicted Performance

• Edward DeLuca
• for the
• XRT Team

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Contributors

• SAO
• Gerry Austin
• John Boczenowski
• Jay Bookbinder
• Dave Caldwell
• Jon Chappell
• Peter Cheimets
• Jonathan Cirtain
• Florine Collette
• Mario Cosmo
• Bill Davis
• Ed DeLuca
• Ed Dennis
• Leslie Frazier
• Leon Golub
• Mike Harris
• Tom Kent
• Warren Martell
• Sang Park

• J-Side At MSCF
• Taro Sakao (JAXA)
• Hirohisa Hara (NAOJ)
• Kazuyoshi Kumagai (NAOJ)
• Tomonori Tamura (NAOJ)
• Kentaro Yaji (NAOJ)
• Ken Kobayashi (MSFC)
• From Japan
• Saku Tsuneta (NAOJ)
• Ryouhei Kano (NAOJ)
• Kenji Hiyoshi (Meisei)

• MSFC Other
• Dave Lehner
• Alan Shapiro
• J R Griffith
• Bill Jones
• Tommy Thompson
• Cydale Smith
• Martin Smithers
• Thomas Kester
• Gary Thornton
• Dave Zissa
• WS Smith
• John Hraba
• James Carter
• Patricia Puckett

• MSFC XRCF
• Jeff McCracken
• Cary Reily
• Jay Carpenter
• Jeff Kegley
• Rich Siler
• Dave Watson
• Ernie Wright
• Galen Zirstein
• Joey Norwood

• MSFC Other
• Larry Hill
• Barbara Cobb
• Danny Colman
• Robert Jayroe
• Marvin Nowlin
• Jerry Owens
• Tom Perrin
• Phil Stahl
• Alphonse Sterling
• Charlotte Talley

• Palermo
• Marco Barbera
• Sal Varisco

• LMSAL
• Dick Catura
• Mons Morrison
• Brian Gantner

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XRT on the FAM _at_ XRCF
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Test Sequence

• Mirror Calibration Test
• 10 Jan- 10 Feb 2005 X-Ray Calibration Facility _at_
  MSFC
• Determined that mirror was distorted by the
  fixture. Masking around the mirror mounts fixes
  the problem.
• Mirror PSF and EE at two energies
• Effective Area at five energies
• Data from LM SXI CCD and FPC through calibrated
  pinholes
• XRT End-to-End Test
• 1-14 Jun 2005 XRCF _at_ MSFC
• Effective area
• PSF and EE at five energies and two focus
  positions
• Wings of PSF
• Filter throughput
• Alignment visible light optic - X-ray mirror
• Data from XRT flight CCD

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XRT Performance Requirements
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Outline

• Image quality
• PSF
• Encircled Energy
• Scattering
• Image quality over the FOV
• Throughput
• Effective Area
• Filter Throughput
• Diagnostic Capability
• Temperature resolution - isothermal plasma
• Visible Light Imager
• Visible and X-ray optical axes alignment

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PSF Measured By CCD

After sub-pixel analysis
Direct image on CCD
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PSF after corrections for 1-G and finite source
distance.
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Encircled Energy at 1keV
Data from the mirror calibration and end-to-end
test on the encircled energy.
The combined data, corrected for 1-G and finite
source distance, together with predictions based
on Goodrich measurements.
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Scattering at 1keV
Integrated Cu-L flux from 10, 100 300um
pinholes taken from the optical axis to 950um off
axis.
Forward fitting of the observations to a model
GaussianLorentzian, and corrected for finite
source and 1-G effects. Scattering contribution
at 1-arcmin is lt 1e-5.
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Image quality as a function of position at best
focus. XRCF measurements and model predictions.
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FOV Optimized Focus Best On-Axis Focus
Note that the RMD diameter includes CCD
pixelization, 1-G distortions and finite source
effects.
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XRT Effective Area at Five Energies
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X-Ray Filters Temperature Response Curves
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Filter throughput XRCF measurements vs.
calculations based on Luxel thicknesses
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Diagnostics
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Visible and X-ray Optical Axes
Over lay of visible (upper left) and X-ray
images. The light sources were located 54.9
apart. The resulting visible and X-ray optical
axes are 17 5 apart.
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Conclusions

• Image quality
• XRT will be the highest resolution solar X-ray
  telescope ever flown Mirror FWHM lt 0.8
  Scattering at 1 lt 10-5.
• Throughput
• Substantial collecting area (gt 2 cm2) at long
  wavelengths (cool plasma) Significant collecting
  area (gt 0.5 cm2 _at_ 1.5 keV) at short wavelengths
  (high temperatures)
• Diagnostics
• With 9 X-ray filters XRT can identify the
  temperature of an isothermal plasma to within 0.1
  (logT), from 6.1 to 7.5 LogT.

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