Semi conductor detectors for soft gamma-ray astrophysics

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1 Semi conductor detectors for soft gamma-ray astrophysics François Lebrun APC (UMR 7164), CEA-Saclay ISGRI PI IWORID 2005 Grenoble

2 High-energy astronomy specific telescopes X-rays and gamma rays radio, IR, visible, UV F. Lebrun IWORID 2005 Grenoble 2

3 Atmospheric absorption space experiments Atmospheric Opacity γ-rays Wavelength F. Lebrun IWORID 2005 Grenoble 3

4 internal background minimization of the detector and surrounding material mass F. Lebrun IWORID 2005 Grenoble 4

5 The SIGMA gamma camera problem Anger camera: NaI + PMTs Detector: NaI 1.2 cm thick 1 GeV P + energy loss: ~ 10 MeV saturation Area: 3200 cm 2 a proton every 300 µs (eccentric orbit) Recovery time > 300 µs Performance degradation (imaging) Solutions: several smaller cameras unacceptable dead zone increase Pixellated camera F. Lebrun IWORID 2005 Grenoble 5

6 INTEGRAL: an ESA gamma-ray observatory IBIS The gamma-ray Imager onboard the INTEGRAL satellite. Excellent Imaging, good spectra ISGRI the IBIS low energy camera (CdTe) Launch: October 2002 Perigee: 10,000 km, Apogee: 150,000 km Operations funded till end 2008 SPI The gamma-ray Spectrometer of INTEGRAL. Excellent spectra, good images F. Lebrun IWORID 2005 Grenoble 6

7 16 CdTe planar detectors ASIC (LETI/DSM) FEE Polycell ISGRI Modular Detection Unit F. Lebrun IWORID 2005 Grenoble 7

8 From SIGMA to IBIS/ISGRI SIGMA IBIS/ISGRI Energy range (kev) Angular resolution Spectral resolution E/E (100 kev) 13% 8% Field of view (FWHM) 9.4 x x 19 Timing accuracy 4 s 64 µs Broad-band sensitivity (100 kev) E=E, 3σ, 10 6 s (cm -2 s -1 kev -1 ) F. Lebrun IWORID 2005 Grenoble 8

9 Noisy pixels (CdTe detectors) Testing thousands of detectors hundreds of them sometime noisy A noisy pixel can trigger continuously blind camera! What can be done? Switch off the noisy pixel Switch on again the off-pixel after a while Raise its low threshold The Noisy Pixel Handling System (NPHS) implemented on board does all that F. Lebrun IWORID 2005 Grenoble 9

10 ISGRI in flight behaviour: unexpected effects Many pixels automatically disabled Likely origin: preamp overload multiple triggers detected as noisy Problem solved after tuning the Noisy Pixel Handling system Events with zero rise-time (10%) preamp saturation (E>5 MeV) Capacitive coupling Trigger of neighbouring detectors Easy correction F. Lebrun IWORID 2005 Grenoble 10

11 ISGRI in flight behaviour: detector stability F. Lebrun IWORID 2005 Grenoble 11

12 ISGRI in flight behaviour: background F. Lebrun IWORID 2005 Grenoble 12

13 ISGRI in flight behaviour: degradation -2.6% / year -0.7% November 2003 Solar flare F. Lebrun IWORID 2005 Grenoble 13

14 The ISGRI Milky Way F. Lebrun IWORID 2005 Grenoble 14

15 SPI: in-flight annealings 3.58 Resolution in kev 1778,96 kev line K 85 K 85 K 85 K A N N E A L I N G - 1 A N N E A L I N G - 2 A N N E A L I N G H 36 H 126 H Revolution number F. Lebrun IWORID 2005 Grenoble 15

16 Soft gamma-ray astrophysics scientific needs for the future sensitivity imaging Energy range Energy resolution Field of view X-ray binaries X XX X X X AGNs XX X pulsars X X X Supernovae XXX X XX SNRs XX XXX XX GRBs X X X e + e - X X CR interactions XX XX XX ISM radioactivity XX XX XX XX XX XX XX XXX XX XX XX Fast timing XX XX F. Lebrun IWORID 2005 Grenoble 16

17 Compton Telescopes F. Lebrun IWORID 2005 Grenoble 17

18 Compton telescope A basic Compton telescope features two layers of position sensitive detectors Layer 1: made of scattering material to scatter the incident gamma ray Layer 2: made of absorbing material to absorb the scattered photon θ E 1 E Both incoming photon energy E 0 and the scatter angle θ can be derived from the Energy deposits E 1 and E 2 E 0 = E 1 + E 2 cos θ = 1 + m e c 2 (1/E 0-1/E 2 ) In addition Compton telescopes allows for polarization studies F. Lebrun IWORID 2005 Grenoble 18

19 Detectors for Compton telescopes Scattering layer: low Z material (e.g. Si) Maximum scattering efficiency Minimum absorbing efficiency Minimum doppler broadening Possibility to measure the electron recoil Absorbing layer: High Z material (e.g. CsI, CdTe, CdZnTe) For both layers, the best energy resolution is mandatory to achieve a good angular resolution (e.g. Ge) The sensitivity depends on the angular resolution In fine the energy resolution is the key parameter F. Lebrun IWORID 2005 Grenoble 19

20 MEGA Records both Compton scattering and pair creation Electron recoil measurement Tracker (scattering layer): Si Calorimeter (absorbing layer): CsI F. Lebrun IWORID 2005 Grenoble 20

21 The advanced Compton telescope Si(Li) at -40 C or Ge at -180 C Wide field Compton instrument dedicated to nuclear astrophysics Goal: sensitivity < 10-7 cm - 2 s -1 F. Lebrun IWORID 2005 Grenoble 21

22 Steps toward a Compton telescope for the NEXT mission Stacks of shottky CdTe diodes Angular resolution T. Tanaka et al. 2004, SPIE Glasgow F. Lebrun IWORID 2005 Grenoble 22

23 Coded Mask Telescopes F. Lebrun IWORID 2005 Grenoble 23

24 Telescope Telescope PSF SWIFT Catching GRBs Coded aperture 17 FWHM Position accuracy 1 4 Detector Energy resolution Timing resolution 100 µs FOV Energy range 32k CZT pixels 7 kev FWHM 2 sr kev Sensitive area 5200 cm 2 Max. trigger rate s -1 Barthelmy et al. 2005, AAS BAT BA T XR T XRT UVO T UVOT Spacecraf t F. Lebrun IWORID 2005 Grenoble 24

25 Study of GRB prompt emission with ECLAIRs Space gamma-ray telescope coupled to ground based optical telescopes Wide field coded mask camera Energy range: kev Field of view: ~ 2 sr 1024 cm2 shottky CdTe 4x4 mm Advanced readout electronics kev Counts CNES microsatellite (2009) Energy (kev) F. Lebrun IWORID 2005 Grenoble 25

26 Ultra deep X-ray X survey with EXIST HET: 5.6 square meters of pixel CZT detectors (1.25 mm pitch) F. Lebrun IWORID 2005 Grenoble 26

27 Detectors for coded-mask soft gamma-ray telescopes GRANAT/SIGMA: single large NaI disk + PMTs INTEGRAL/ISGRI: planar CdTe INTEGRAL/PICsIT: CsI+PIN-diodes INTEGRAL/SPI: Cooled HPGe detectors SWIFT/BAT: planar CZT ECLAIRS: planar CZT EXIST: pixel CZT F. Lebrun IWORID 2005 Grenoble 27

28 Gamma-ray Lenses F. Lebrun IWORID 2005 Grenoble 28

29 Towards a gamma-ray lens d diffracted beam transmitted beam A plane parallel crystal intercepting a beam of very short wavelength radiation λ act as a 3-D 3 Diffraction array. When entering such a crystal under an angle θ a beam of high-energy photons is therefore diffracted under the same angle θ defined by the Bragg condition: 2 d sin(θ) = n λ A gamma-ray concentrator (gamma-ray lens ) could then be build in mounting hundreds of such crystals onto concentric rings Detectors at the focus could be Ge,, CdTe or CZT Because of their long focal distance (>( > 10 m) m gamma-ray concentrators would require two satellites in close formation as in the MAX mission under investigation in France F. Lebrun IWORID 2005 Grenoble 29

30 The ISGRI Milky Way Confusion! F. Lebrun IWORID 2005 Grenoble 30

31 Grazing Incidence Telescopes: extending the mirror domain F. Lebrun IWORID 2005 Grenoble 31

32 The Galactic Nucleus IBIS ISGRI G XMM EPIC As As will seen be with seen INTEGRAL with SIMBOL BOL-X in the in kev band F. Lebrun IWORID 2005 Grenoble 32

33 SIMBOL-X (CNES-ASI 1-60 kev) 250 T=22 o C 200 counts / ADC chanel FWHM = 71.5 ev ENC = 8.43 el r.m.s FWHM =151.1 ev DEPFET : 8x8 «macro pixel» 1mm² matrix energy (ev) 256 pixels CdTe Schottky arrays, 0.5 mm thick (ACRORAD) Spectrum with IDeF-X V0 ASIC F. Lebrun IWORID 2005 Grenoble 33

34 SIMBOL-X X Sensitivity Minimum detectable flux (photons cm -2 s -1 kev -1 ) XMM SIMBOL-X INTEGRAL Energy (kev) F. Lebrun IWORID 2005 Grenoble 34

35 HEFT (balloon) - NuSTAR (SMEX 6-80 kev) Detector: pixel CZT Pixel size: 500m Thickness: 2 mm Unit dimension: 1.3 x 1.3 cm Units/focal plane: 4 E/E = 1.4% (FWHM, 70 kev) Elect. noise (rms, leakage incl.) 40 e - F. Lebrun IWORID 2005 Grenoble 35

36 Focusing telescope for the NEXT mission (1-80 kev) Caltech ISAS collaboration Detector: pixel CdTe Pixel size: 500µm Thickness: 0.5 mm Unit dimension: 2.4 x 1.3 cm F. Lebrun IWORID 2005 Grenoble 36

37 Conclusions Planar Semiconductor detectors such as CdTe, CZT, Ge are currently observing the soft gamma-ray sky from space Thanks to their satisfactory in-orbit behaviour (stability, background, degradation) it is now established that they can be safely operated and that they can maintain their performance over long periods of time in space More and more projects plan to use semiconductor detectors Both focusing and Compton telescope will take advantage of pixel detectors (CdTe, CZT) with their Fine imaging capability Enhanced spectral performance F. Lebrun IWORID 2005 Grenoble 37

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