X-RAY INSTRUMENTATION FOR ASTRONOMY

1. Istituto Nazionale di AstrofisicaOsservatorio Astronomico di Palermo X-RAY INSTRUMENTATION FOR ASTRONOMY Alfonso Collura

2. Other People Involved (Since) • Marco Barbera - Associate Professor DSFA (1992) • Roberto Candia - Technician (electronics – mechanical) (1996) • Salvatore Varisco - Technician (software – electronics) (1996) • Gaspare Di Cicca - Technician (mechanical) (2001) • Emanuele Perinati - Post Doc (1998) • Ugo Lo Cicero – PhD Student (Electronic Engineer) (2007)

3. I Will Talk About • History of the X-Ray Astronomy Calibration and Testing (XACT) Facility • Activities in the framework of space missions • Instrumentation development and other activities not for a specific mission

4. XACT Facility • Established under the impulse of G.S. Vaiana to partake to the development of CHANDRA instrumentation started operating in 1993 • Designed with CHANDRA in mind, but privileging versatility to allow several other applications

5. XACT Development Personnel (Sc/Tec) Funding Source Year XACT conceivment 1 / 2 400SICILIAN GOV. 1989 30 ASI Rental of building 100 OAPA 1 / 2 1991 100 ASI Beam line and basic equipment 100 OAPA 2 / 2 20 CNR First light 200 SICILIAN GOV. 1993 100 ASI 100 OAPA Upgrade I – Clean room; MCP detector; Transmission grating;UV beam line; 2 / 2 1995 120 ASI 100 OAPA 2 / 3 50 CRA 1997 120ASI 100OAPA ADR Cryostat 2 / 3 1999 70 PRIN-MIUR 90 ASI 100 OAPA 2001 2 / 3 70 PRIN-MIUR 110 ASI Vacuum control 100 OAPA 2003 2180 before upgrade II Upgrade II – See dedicated slide 2 / 3 2007 SEE DEDICATED SLIDE

6. First X-Ray Beamline

7. XACT - Upgrade I GSPC detector MCP detector UV Beamline Clean Room X-Ray Transmission grating Monochromator X-ray Source Test Section 8 m 8 m

8. UPGRADE II (2003-2007) Funding Source XACT DEVELOPMENT PON (co-funding from EU, Ital. Gov. and OAPA) Longer (35 m) Beam Line 2 m diameter Test Chamber X-ray optics micropositioning Double Cristal Monochromator LTD Read-out Electronics Maglev oil-free pumping New Machine Shop Moving to Via Ingrassia 680 85 PRIN-MIUR 70 ASI 60 SICILIAN GOV. 150 OAPA 15 PRIN-INAF 150 MEF (PRISMA) 1210 Not included: works on the building

9. The new beamline

10. Space Missions • CHANDRA • XMM-NEWTON • HINODE • CHANG’E-1 LOXIA • CORONAS PHOTON- SphinX • SIMBOL-X • EDGE

11. Chandra HRC Development of the UV/Ion shields • Design, Vibrational and Acoustic tests, Calibration plan UV transmission measurements of the UV/Ion shields • Out of band rejection X-ray transmission of the UV/Ion shields • X-ray Transmission modeling, XANES and EXAFS X-ray QE of MCP’s at Daresbury Synchrotron • CsI vs. KBr, X-ray QE modeling, Life tests End to End test at Marshall Space Flight Center • HRC-I +HRMA, HRC-S + HRMA + Gratings In Flight Calibration • Out of band sensitivity

12. Aluminum oxidation and interferences UV transmission measurements of the UV/Ion shields at XACT and DSFA-UNIPA New filter design: Polyimide instead of Lexan, and single layer of aluminum (impact also on Chandra ACIS, Newton-XMM EPIC, JET-X CCD).

13. Newton-XMM EPIC Medium and Thin Filter design and calibration plan UV transmission measurements of Medium and Thin Filters • Out of band rejection X-ray transmission measurements of Medium and Thin filters • X-ray Shadowgraphs • X-ray Transmission modeling, XANES and EXAFS Monitoring ageing effects on Medium and Thin filters

14. July 1997 July 2002 Monitoring ageing effects of the Medium and Thin filters Slight increase in transmission in a narrow band. No significant impact on the science with EPIC

15. XRT on board HINODE ( PI: dr. Leon Golub, SAO, Cambridge, MA) Calibration of the Focal Plane 9 Filters • X_ray shadowgraphs • X-ray transm. measurements and modeling Calibration of the Telescope • Participation in the end to end test at Marshall

16. X-Ray Shadowgraphs 6 – 25 μm Al Filter Shadograph at 1.49 keV

17. X-Ray Transmission measurements and modeling 6 – 25 μm Al Filter

18. CHANG’E-1 LOXIAChinese experiment to study the composition of the lunar surface

19. SphinX

20. SIMBOL X Thermal Shields No shields T ~ 7 °C With shields T < 1 °C 20 °C 19.2 °C 15 °C 18.6 °C X-Ray Transmission Polyimide+Al Al

21. EDGEDesign of the Narrow Field Imager Telescope Contribution to the Design and Optimization of the Narrow Field Imager Telescope equipped with an X-Ray Microcalorimeter Array Focal Plane Detector Design of the Baffles for the Wide Field Telescope equipped with an X-Ray CCD Focal Plane Detector in collaboration with INAF-IASFPA

22. R&D Activities (not for a specific mission) • NTD Germanium Microcalorimeters • Plastic Foil light weight X-ray Optics • Bio samples irradiation (next presentation)

23. X-Ray Microcalorimeters with NTD Ge Sensors • In collaboration since 1997with SAO (PI: Eric Silver) we are investigating X-ray microcalorimeters with NTD Germanium sensors for laboratory and astrophysical applications. • More recently we have started a collaboration with UNIPA-DIEET to develope a fully Planar approach for the construction of 2-D arrays with a large number of pixels.

24. State of the Art • Energy Resolution: - 3.1 eV FWHM at 6 keV - 50 eV FWHM at 60 keV • Time Resolution: - Counting Rate up to ~ 50 Hz per pixel without significant energy resolution degradation. • Construction Technique: - Micromachining. 2x2 arrays currently in use. The proposed approach for 2-D arrays with large number of pixels is based on the superposition of linear arrays.

25. Study of Absorber Materials • Single Stage ADR Cryostat built in house. Minimum Temperature 42 mK. Hold Time at 60 mK longer than 2 days. • Four channel fully wired read-out electronics to operate small arrays of Semiconductor Thermistor Microcalorimeters.

26. (a) Lapped doped NTD-Ge wafer (b) Attachment of a monolithic absorber foil Resist coating - Laser Microlithography (c) Deep Wet Etching of Ge (~ 100 μm) (d) (e) Evaporation of electrical contacts on Ge Evaporation of electrical circuit on support thin membrane (f) Electrical connection to the support membrane (g) Proposed Fully Planar Approach for the Construction of Arrays of Microcalorimeters with Ge Sensors (h) Separation of absorbers

27. Deep Wet Etching of Ge Pyramidal Geometry Toroidal Geometry • Orientation (100) • 3 hours etching • Orientation (100) • 4 hours etching

28. Plastic foils grazing incidence X-ray Optics (Collaboration with SAO and DSRI) • Plastic is very light, elastic, cheap • Plastic foils from common industrial applications have high surface smoothness by a combination of stretching and rolling • Plastic foils replicate the figure of the mandrel but not the smoothness. Expensive superpolished mandrels not required • Plastic has strong affinity to coating (single and multilayer)

29. Surface roughness AFM measurements show micro roughness of uncoated foils of 4 ÷ 7 Å (Chandra-HRMA has 3 ÷4 Å)

30. Mounting the foils • Vacuum hold-down mandrels to form cylindrical or conical shells • Foils hold inside grooves of the supporting wheels • Epoxy cured while foils are still inside the mandrel

31. 8 m 8 m Imaging detector X-ray Source FWHM ~ 10” HPD ~ 2’ X-ray imaging tests of Cylindrical optics at XACT

32. Irradiation of Organic Samples The XACT FACILITY is being used for the irradiation of organic samples in a program of Astrobiology that will be the subject of next talk