1. E > 100 keV activities at DTU Space ½ MeV Telescope Design
Carl Budtz-Jørgensen et. al
Multilayer Mirrors: NuSTAR
CZT Detectors: ASIM

2. TEM image of 1.5 nm-period ML

8. Achieving High Position Resolution Using CZT Drift Strip Detectors
I. Kuvvetli1, C. B. Jørgensen1, A. Zappettini2, G. Benassi2, E. Caroli3, L. Marchini2, N. Zambelli2, J. B. Stephen3, N. Auricchio3
1)DTU Space, Technical University of Denmark, Copenhagen, Denmark
2)IMEM-CNR, Parma, Italy
3)INAF/IASF, Bologna, Italy

9. 3D CZT Detectors
General requirements for the high energy astrophysics instrumentation sensors are :
high efficiency, good spatial resolution, good spectroscopic resolution
ESA development project:“3D CZT High Resolution Detectors /11/NL/CBi”.
This prototype detector technology is based on CZT Drift Strip Detector.
Astrophysical applications:
Focal instrument for Laue Lens (uni. of Ferrara)
Focal Instrument for High Energy (up to 500keV) focussing optics (ESA funded development project on-going at DTU)
Polarimeter ( keV) (INAF Bologna)
Compton Telescope
(Homeland Security)

10. CZT Drift Strip Detector
1D CZT drift strip detectors
0.70% FWHM @ 356 keV X Y
CZT DSD design:
8 drift strips and one collecting anode readout strip
All strips are 10 mm long, 100 um wide, 100 um gab
Drift detector cell pitch (between A and B) s 1.6 mm
CZT crystal: 10 mm ×10 mm ×2.5 mm
Small anodes  better energy resolution at high energies
Drift strips  screening the anodes from holes and provides effective large sensitive area by focusing electrons on anodes
Cathode/anode signal  provides DOI
The energy resolution can further be enhanced using DOI
The DTU Space CZT drift detector
Van Pamalen, Budtz-Jørgensen NIM A 441(1998), 197

11. TEST AT ESRF 100-600 keV monochromatic beam. 50x50 µm
3DCZT prototype (CZT detector: 20 mm x 20 mm x 5 mm).

12. ESRF 400 keV XY Scanning
400 µm
400 µm

13. ESRF 400 keV Z Scanning
Y (mm)
Z-scan (mm)

14. Polarization 4 mm CZT ø scatter detector. Efficiency: 19%@ 511 keV 5040
2550 40

15. Challenge at DTU Space Design of a soft gamma ray focussing telescope using these technologies 0.1 to 0.6 MeV Polarimetry Your input and ideas are most welcome

16. CZT Drift Strip Detector
1D CZT drift strip detectors
0.70% FWHM @ 356 keV X Y
CZT DSD design:
8 drift strips and one collecting anode readout strip
All strips are 10 mm long, 100 um wide, 100 um gab
Drift detector cell pitch (between A and B) s 1.6 mm
CZT crystal: 10 mm ×10 mm ×2.5 mm
Small anodes  better energy resolution at high energies
Drift strips  screening the anodes from holes and provides effective large sensitive area by focusing electrons on anodes
Cathode/anode signal  provides DOI
The energy resolution can further be enhanced using DOI
The DTU Space CZT drift detector
Van Pamalen, Budtz-Jørgensen NIM A 441(1998), 197

17. Measured 1D Position Resolution
The measured position resolutions depend on non-correlated electronic noise and the size and shape of the charge distribution generated by the photo and Compton electrons.
The charge distributions generated by photo or Compton electrons were calculated using the Casino Monte Carlo code
The calculated position resolutions were obtained without adjustable parameters and describe the measurements quite well.

18. 2D Position Capability Y X 57Co source 1us shaping
Planar bias:Vp=-400V
Drift biases:
V1=-60V
V2=-120V
Beam size= Ø350um collimator
X-step= 200 um
Y-step= 400 um

19. n d i  W/B4C Multilayer B4C W Γ B4C = 0.6 for all bilayers
SiOx
d i n
Γ B4C = 0.6
for all bilayers
e.g. d5 = 12 nm
B4C layer = (0.6 x 12) nm
W layer = (0.4 x 12) nm
Desiree Della Monica Ferreira
Postdoc, DTU Space - Astrophysics
Multilayer Coatings for ATHENA