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

8-November th Solar-B Science Meeting2 Contributors MSFC XRCF –Jeff McCracken –Cary Reily –Jay Carpenter –Jeff Kegley –Rich Siler –Dave Watson –Ernie Wright –Galen Zirstein –Joey Norwood 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 –Lisa Paton –Bill Podgorski –Alana Sette –Jason Scott (MSU) –Sara Shivers (MIT) –Dave Weaver –Mark Weber 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 –Larry Hill –Barbara Cobb –Danny Colman –Robert Jayroe –Marvin Nowlin –Jerry Owens –Tom Perrin –Phil Stahl –Alphonse Sterling –Charlotte Talley 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 Palermo –Marco Barbera –Sal Varisco LMSAL –Dick Catura –Mons Morrison –Brian Gantner

8-November th Solar-B Science Meeting3 XRT on the XRCF

8-November th Solar-B Science Meeting4 Test Sequence Mirror Calibration Test –10 Jan- 10 Feb 2005 X-Ray Calibration 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 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

8-November th Solar-B Science Meeting5 XRT Performance Requirements

8-November th Solar-B Science Meeting6 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

8-November th Solar-B Science Meeting7 PSF Measured By CCD Direct image on CCD After sub-pixel analysis

8-November th Solar-B Science Meeting8 PSF after corrections for 1-G and finite source distance.

8-November th Solar-B Science Meeting9 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.

8-November th Solar-B Science Meeting10 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 1- arcmin is < 1e-5. Scattering at 1keV

8-November th Solar-B Science Meeting11 Image quality as a function of position at best focus. XRCF measurements and model predictions.

8-November th Solar-B Science Meeting12 FOV Optimized Focus & Best On-Axis Focus Note that the RMD diameter includes CCD pixelization, 1-G distortions and finite source effects.

8-November th Solar-B Science Meeting13 XRT Effective Area at Five Energies

8-November th Solar-B Science Meeting14 X-Ray Filters & Temperature Response Curves

8-November th Solar-B Science Meeting15 Filter throughput XRCF measurements vs. calculations based on Luxel thicknesses

8-November th Solar-B Science Meeting16 Diagnostics

8-November th Solar-B Science Meeting17 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. Visible and X-ray Optical Axes

8-November th Solar-B Science Meeting18 Conclusions Image quality –XRT will be the highest resolution solar X-ray telescope ever flown: Mirror FWHM < 0.8”; Scattering at 1’ < Throughput –Substantial collecting area (> 2 cm 2 ) at long wavelengths (cool plasma); Significant collecting area (> 0.5 cm 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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