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Flare Observations with TRACE and Yohkoh

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Constraints: Focal Length, Pixel Size, FOV, Resolution. Goal: 2' resolution for the ... Thick Be Shadowgraph. 8/14/09. Solar B X-Ray Telescope. 28. Energy Scans ... – PowerPoint PPT presentation

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Title: Flare Observations with TRACE and Yohkoh


1
XRT Performance Update
Edward DeLuca
2
Science Goals
3
Science Goals
4
Science Goals
5
Requirements Flowdown
6
Mirror Properties
  • Optimized Polynomial Design
  • Constraints Focal Length, Pixel Size, FOV,
    Resolution
  • Goal 2 resolution for the full sun FOV
  • Low Scattering
  • Surface roughness lt 5A RMS
  • Temperature sensitivity lt 1MK (cool coronal plasma

7
Mirror Status
  • Mirror polishing is proceeding at Goodrich.
  • We expect the mirror to meet or exceed all
    requirements.

8
Entrance Filter
  • Requirements
  • White Light Transmission lt 10 -6
  • Heat Rejection
  • 5 year on orbit survival
  • X-Ray transmission gt 0.7 from 1-60A
  • Properties
  • 1600 A Al
  • 2500 A Polyimide

9
Focal Plane Filters
  • Requirements
  • White Light Transmission lt 10 -6
  • 5 year on orbit survival
  • Temperature Diagnostics from 1 to gt 20 MK
  • Morphology for T lt 1MK
  • Properties
  • Science filters are on polyimide or free standing
  • Simple proven design
  • Testing/Verification
  • Environmental
  • Transmission

10
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.

11
Ordered Filter Set
12
Optical Paths Overview
2700 mm
X-RAY
White Light
13
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

14
Mirror Calibration
  • XRCF Available Lines
  • C-K 0.277 keV 44.7A
  • O-K 0.525 keV 23.6A
  • Cu-L 0.933 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.

15
Mirror Requirements
  • Focal Length 2708 /- 5mm
  • Bandwidth 0.2 to 6.0 keV
  • Image Performance 68 encircled energy within 27
    microns _at_ 0.523 keV at focal plane
  • FOV 35 arcmin
  • Effective Area gt3.0 cm2 _at_ 0.56 keV 1 keV
  • Wings of On-Axis PSF - _at_6 keV signal at 1 arcmin
    lt 3x10-5 peak flux.

16
Visible Light Optic Requirements
  • Focal Length 2708 /- 2mm
  • Central Wavelength 4305 /- 20 A
  • Bandpass lt120A FWHM
  • Resolution lt2 half power dia.
  • FOV gt30 arcmin
  • Co-Alignment lt0.5 arcmin
  • Confocality w/ GI optic /- 150 microns

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.
    23 1996.
  • Collura, A. et al. 1996 SPIE 2808, 134.

18
Shadowgraphs
19
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20
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21
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22
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23
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24
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25
Thin Be Shadowgraph
26
Medium Be Shadowgraph
27
Thick Be Shadowgraph
28
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).

29
Energy Scans AXAF Example
Collura, A. et al 1996 SPIE 2808, 134.
30
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.

31
Filter Transmission
32
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33
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34
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35
XRT Exposure Times
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