The X-Ray Telescope for Solar-B
Results of the Calibration Tests
and Predicted Performance
Edward DeLuca
for the
XRT Team
Contributors
•
MSFC XRCF
–
–
–
–
–
–
–
–
–
MSFC Other
–Larry Hill
–Barbara Cobb
–Danny Colman
–Robert Jayroe
–Marvin Nowlin
–Jerry Owens
–Tom Perrin
–Phil Stahl
–Alphonse Sterling
–Charlotte Talley
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SAO
–
–
–Dave Lehner
–Taro Sakao (JAXA)
–
–Alan Shapiro
–Hirohisa Hara (NAOJ)
–
–J R Griffith
–Kazuyoshi Kumagai (NAOJ) –
–Bill Jones
–Tomonori Tamura (NAOJ)
–
–Tommy Thompson
–Kentaro Yaji (NAOJ)
–
–Cydale Smith
–Ken Kobayashi (MSFC)
–
–Martin Smithers From Japan
–
–Thomas Kester
–
–Saku Tsuneta (NAOJ)
–Gary Thornton
–
–Ryouhei Kano (NAOJ)
–Dave Zissa
–
–Kenji Hiyoshi (Meisei)
–WS Smith
–
–John Hraba
–
–James Carter
–
–Patricia Puckett
•Palermo
–
–Marco Barbera
–
–Sal Varisco
–
•LMSAL
–
–Dick Catura
–
–Mons Morrison
–
–Brian Gantner
–
–
6th Solar-B Science Meeting
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–
MSFC Other
Jeff McCracken
Cary Reily
Jay Carpenter
Jeff Kegley
Rich Siler
Dave Watson
Ernie Wright
Galen Zirstein
Joey Norwood
•
•J-Side At MSCF
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
Lisa Paton
Bill Podgorski
Alana Sette
Jason Scott (MSU)
Sara Shivers (MIT)
Dave Weaver 2
Mark Weber
XRT on the FAM @ XRCF
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Test Sequence
• Mirror Calibration Test
– 10 Jan- 10 Feb 2005 X-Ray Calibration Facility @ 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 @ 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
Verification #
XRT Performance Requirement Approach
3
T
0.2 to 2.0keV
Image performance: 50%
encircled energy with in 1"
4
radius from an on-axis source
at 1keV
T
52%
Effective area > 1.0cm^2 at
0.5keV
T
> 2.0 cm^2
Confocality X-ray and Visible
13
light image +/- 150micorns
T
VLI depth of
focus
~700microns
XRT filter shall provide a
temperature resolution of
17
0.2(logT) over the range 6.1 <
log(T) < 7.5
A
0.1 (logT)
resolution
T
17+/-5"
separation
7
25
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X-ray performance bandwidth
0.2 to 1.2keV
Result
X-ray and VLI shall be
coalligned to within 1'
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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
Direct image on CCD
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After sub-pixel analysis
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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 1G 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 Gaussian+Lorentzian, and
corrected for finite source and 1-G
effects. Scattering contribution at 1arcmin is < 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
Filter #
Filter Name
Materials
1
Entrance
Al2O3
Al
Al2O3
polyimide
75
1600
25
2200
2
Thin Al
Mesh
Al2O3
Al
Al2O3
50
1600
50
3
Thin Al
poly
Al2O3
Al
Al2O3
polyimide
75
1250
25
2500
4
C poly
C
polyimide
6000
3500
Ti poly
TiO2
Ti
TiO2
polyimide
75
3000
25
2500
5
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Thickness (A)
Filter #
Filter Name
Materials
Thickness (A)
6
Thin Be
BeO
Be
BeO
7
Med Al
Al2O3
Al
Al2O3
75
125000
75
8
Medium Be
BeO
Be
BeO
75
300000
75
9
Thick Al
Al2O3
Al
Al2O3
75
250000
75
10
Be 300um
BeO
Be
BeO
3000
3000000
3000
14
75
90000
75
Filter throughput XRCF measurements vs.
calculations based on Luxel thicknesses
Source
Energy (keV)
CΠK
0.277
OΠK
0.525
Filter
%
%
24
Al Mesh
+/-7
21.2
24
Al Poly
+/-8
19.4
64
C Poly
+/-6
65.3
42
Ti Poly
+/-7
34.0
--Be Thin
--0
--Be Med
--0
--Al Med
--0
--Al Thick
--0
--Be Thick
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--0
81
+/- 9
72.1
51
+/- 9
50.3
8
+/- 5
10
5
+/- 3
3.1
----0.1
----0
----0
----0
----0
Cu Π L
0.933
Transmission
%
94
+/- 6
91.9
77
+/- 7
82.0
61
+/- 5
57.9
34
+/- 3
33.0
26
+/- 4
27.8
5
+/- 3
1.5
2
+/- 2
0.6
----0
----0
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Al Π K
1.49
Mo Π L
2.5
%
81
+/- 4
97.6
94
+/- 5
94.6
79
+/- 3
86.3
69
+/- 4
71.7
78
+/- 6
72.6
49
+/- 7
32.6
23
+/- 4
23.6
5
+/- 2
6.0
----0
%
+/- 7
93
92
90
+/- 7
91.2
94
+/- 7
95.6
91
+/- 6
89.3
91
+/- 7
91.14
77
+/- 5
73.66
3
+/- 2
0.2
----0
8
+/- 3
6.73
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Diagnostics
8-November-2005
Model T
(Log(T))
Peak of Best
Fit Gaussian
Sigma of
Gaussian
Peak Offset
(T_fit-T_model)
6.1
6.2
6.3
6.4
6.5
6.6
6.7
6.8
6.9
7
7.1
7.2
7.3
7.4
7.5
6.08
6.2
6.3
6.4
6.48
6.58
6.68
6.79
6.89
7
7.11
7.22
7.31
7.39
7.44
0.07
0.06
0.04
0.05
0.07
0.08
0.07
0.06
0.07
0.07
0.06
0.05
0.09
0.1
0.1
-0.02
0
0
0
-0.02
-0.02
-0.02
-0.01
-0.01
0
0.01
0.02
0.01
-0.01
-0.06
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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 < 0.8”; Scattering
at 1’ < 10-5.
• Throughput
– Substantial collecting area (> 2 cm2) at long
wavelengths (cool plasma); Significant collecting area
(> 0.5 cm2 @ 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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