CANDELA, a setup to study a stacked detector configuration and the way to ASTRO-H , Daniel Maier, P.160
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1 CANDELA, a setup to study a stacked detector configuration and the way to ASTRO-H , Daniel Maier, P.160
2 Overview CANDELA setup Statistics on polarization measurements Perspective: ASTRO-H 2 Daniel Maier
3 CANDELA setup sources 3 Daniel Maier optics detector onboard electronics data analysis
4 CANDELA setup sources optics detector onboard electronics 1 Fe-55 Am Daniel Maier L E D H E D SpaceWire 1 SpaceWire data analysis
5 CANDELA setup 5 Daniel Maier
6 Low energy detector (LED) HV filter SW1 0/0 SW2 CMX 63/0 y SW1 SW2 0/63 CMX silicon based (Z = 14) active pixel matrix 64 x 64 Same technology as for ATHENA WFI 6 Daniel Maier x 63/63
7 LED pixel structure + p back contact -5 V -10 V -20 V -30 V -40 V -50 V -80 V silicon based (Z = 14) active pixel matrix 64 x 64 DePFET pixel: - sideward depletion - internal gate - additional CLEAR FET macro pixel 7 Daniel Maier
8 LED matrix structure SWITCHER CHIP 1 common DRAIN column row SWITCHER CHIP 2 38 μs GATE CLEAR CLEAR GATE 1.47 μs 1.37 μs SOURCE DRAIN CG off CG on G on G off C on C off CAMEX SWITCHER controller chips - switch gate, clear gate, and clear potentials 8 Daniel Maier ADC CAMEX readout chip (same as for SVOM MXT) signal amplification - correlated double sampling - multiplexing to ADC -
9 CAMEX 9 Daniel Maier D3C SEQ SPI DEPFET matrix SWITCHER SWITCHER LED electronics IFC receiver scd_control ech_control sender CMX+ CMX- ADJ AD 8130 AD V ADC RAM offset map bad map 14 bit PAGU pixel address generator unit 32 bit PCU RAM EPP pixel correction unit energy map neighbor map 33 bit CMCU common mode correction unit 33 bit ETAU energy threshold analyzer unit 32 bit PTAU pattern & trace analyzer unit 32 bit PPFU programable pixel filter unit 64 bit cmd_control Space Wire core SpaceWire PC
10 LED electronics: EPP ADC 14 bit PAGU pixel address generator unit input: frame based 10 Daniel Maier 32 bit RAM RAM offset map bad map energy-threshold map neighbor-threshold map PCU pixel correction unit 33 bit EPP CMCU common mode correction unit 33 bit ETAU energy threshold analyzer unit 32 bit PTAU pattern & trace analyzer unit event building - pixel individual energy tresholds 32 bit PPFU programable pixel filter unit 64 bit IFC output: event based - position - pulse height - time
11 LED energy calibration pixel individual calibration via cubic spline interpolation smooth transition functional description E(PHA) 11 Daniel Maier
12 LED energy calibration -1 F [(s kev cm²) ] 3000 gcmx = 100 % gcmx = 62 % gcmx = 33 % gcmx = 21 % Emin 10 low energy background noise Daniel Maier E [ev] 0
13 LED spectra photon flux F [1/(s * kev * cm 2)] 6 gcmx = 100 % total singles doubles triples quadruples ) Np-Lβ 1 1,2 3) Te-Lα 1,2 18) Np Lγ 1 4) Mn-Kα,esc 19) end-d 5) Ti-Kα 1,2 7) Mn-Kβ 1, ) Np-Lβ 2 2) Cd-Lα 6) Mn-Kα 1, ) Al-Kα 1,2 8) Cu-Kα 1,2 9) Cu-Kβ 1,3 10) Mn-Kα, Mn-Kα, esc 19 11) end-s 12) Mn-Kα, Mn-Kα 13) Mn-Kα, Mn-Kβ ) Mn-Kβ, Mn-Kβ 15) Np-Lα 1, Daniel Maier E [kev]
14 photon flux F [1/(s * kev * cm 2)] LED spectra 4 gcmx = 62 % total singles doubles triples quadruples ) Al-Kα 1,2 16) Np-Lβ 2 2) Mn-Kα,esc 17) Np-Lβ 1 3) Ti-Kα 1,2 18) end-s 4) Mn-Kα 1,2 19) Am-26 5) Mn-Kβ 1,3 20) Te-Kβ 1,3 6) Cu-Kα 1,2 21) Te-Kβ 2 7) Cu-Kβ 1,3 22) not id. 8) Mn-Kα, Mn-Kα, esc 23) not id. 13 9) Mn-Kα, Mn-Kα 19 10) Mn-Kα, Mn-Kβ ) Mn-Kβ, Mn-Kβ 24 12) Np-Lα 1, ) Nb-Kα 1,2 14) Np-Lη 15) Np-Lβ Daniel Maier E [kev] 24) end-d
15 photon flux F [1/(s * kev * cm 2)] LED spectra gcmx = 33 % total singles doubles triples quadruples Daniel Maier ) Nb-Kβ 1,2,3 2) Mn-Kα,esc 17) not id. 3) Ti-Kα 1,2 18) Np Lγ 1 4) Mn-Kα 1,2 19) Np Lγ 3,6 5) Mn-Kβ 1,3 20) Ag Kα 1 6) Cu-Kα 1,2 21) Cd Kα 1,2 7) Cu-Kβ 1,3 22) Sn Kα 1,2 8) Mn-Kα, Mn-Kα, esc 23) Am ) Al-Kα 1, ) Mn-Kα, Mn-Kα 24) Te Kα 1,2 10) Mn-Kα, Mn-Kβ 25) Sn Kβ 1,3 11) Mn-Kβ, Mn-Kβ 26) Te-Kβ 1,3 12) Np-Lα 1,2 27) Te-Kβ 2 13) Np-Lη,β 6 28) Am-33 14) Np-Lβ 2 29) end-s 15) Np-Lβ 1 30) Am-59 E [kev]
16 photon flux F [1/(s * kev * cm 2)] LED spectra gcmx = 21 % total singles doubles triples quadruples ) Al-Kα 1,2 16) Np-Lγ 1,2 2) Mn-Kα,esc 17) Np-Lγ 3,6 3) Ti-Kα 1,2 18) Ag-Kα 1,2 4) Mn-Kα 1,2 19) Cd-Kα 1,2 5) Mn-Kβ 1,3 20) Sn-Kα 1,2 6) Cu-Kα 1,2 21) Am-26 7) Cu-Kβ 1,3 22) Te-Kα 1,2 8) Mn-Kα, Mn-Kα, esc 23) Sn-Kβ 1, ) Mn-Kα, Mn-Kα ) Am-33 11) Np-Lα 1,2 26) Am-59 12) Np-Lη,β ) Np-Lβ 2 14) Np-Lβ 1 15) Nb-Kβ 1,2, Daniel Maier ) Te-Kβ 1,2,3 10) Mn-Kα, Mn-Kβ E [kev]
17 High energy detector (HED) cooling cables connection PT-100 temperature sensors HED: CdTe based (Z = 48 & 52) 8 x 8 Schottky diodes triggered readout mode polarization effect 17 Daniel Maier side view top view Pt guard ring CdTe ASIC 1 Al Al Al Al Al Al Al Al ASIC 2 ASIC 3 Caliste-64 body ASIC 4 IO-ports 10 mm
18 High energy detector (HED) Rbias RF CF differentiator other channels integrator 2 1 Rpz Rint Cdiff Cdet 15 pulse shaper Rdiff Cint peak detection analogue memory 0 other IDeF-X ASICs output side view top view Pt guard ring CdTe ASIC 1 Al Al Al Al Al Al Al Al ASIC 2 ASIC 3 18 Daniel Maier Caliste-64 body ASIC 4 IO-ports 10 mm multiplexer Ubias preamp. multiplexer detector output to ADC
19 HED: energy calibration energy calibration via correlation (ECC) build a synthetic energy spectrum - assume a transformation ev ADU: - E = g*pha + Eoff build several synthetic pulse-height spectra - compare the observed with the synthetic spectra via correlation - I I 1 emission line spectrum synthetic energy spectrum synthetic pulse-height spectra 1 * E [ev] I OPHA,1 g1 1 OPHA,2 g1 I OPHA,1 g2 I 1 1 PHA [ADU] 19 Daniel Maier E [ev] PHA [ADU] PHA [ADU]
20 HED: energy calibration energy calibration via correlation (ECC) build a synthetic energy spectrum - assume a transformation ev ADU: - E = g*pha + Eoff build several synthetic pulse-height spectra - compare the observed with the synthetic spectra via correlation - 59 ev/adu 167 ADU 20 Daniel Maier
21 HED: energy calibration energy calibration via correlation (ECC) build a synthetic energy spectrum - assume a transformation ev ADU: - E = g*pha + Eoff build several synthetic pulse-height spectra - compare the observed with the synthetic spectra via correlation - 59 ev/adu 167 ADU 21 Daniel Maier
22 _144120_pixspec_lin.fits(value_1-512) HED: energy calibration non-linear ECC 1 pixel (2/4) relative flux flux observed spectrum linear linearsynthetic syntheticspectrum spectrum non-linear synthetic spectrum PHA 22 Daniel Maier [ADU]
23 HED spectra photon flux F [1/(s * kev * cm 2)] linear ECC 3 1) Np-L l total singles doubles triples quadruples (100.0%) (90.1%) (9.4%) 2073 (0.2%) 1025 (0.1%) 2) Np-Lα 3) Np-Lβ 4) Np-Lγ 5) Am-26 6) Am-59, Te-Kα,esc 7) Am-59, Cd-Kα,esc 0.1 8) Compton reprocessing of 9 9) Am Daniel Maier E [kev]
24 HED spectra 100 photon flux F [1/(s * kev * cm 2)] ) E th non-linear ECC 3 1) Np-L 5 total singles doubles triples quadruples l 2) Np-Lα (100.0%) (90.1%) (9.4%) 2073 (0.2%) 1025 (0.1%) 3) Np-Lβ 4) Np-Lγ 5) Am-26 6) Sn-Kβ 7) Am-59, Te-Kα,esc 10 8) Am ) Am-59, Cd-Kα,esc 10) Am ) Compton reprocessing of ) Am-59 13) Np-Kα 1, Daniel Maier E [kev]
25 HED spectra photon flux F [1/(s * kev * cm 2)] cubic splines interpolation ) Np-L total singles doubles triples quadruples l 2) Np-Lα ) E th (100.0%) (90.1%) (9.4%) 2073 (0.2%) 1025 (0.1%) 3) Np-Lβ 4) Np-Lγ 5) Am-26 6) Sn-Kβ 7) Am-59, Te-Kα,esc 8) Am ) Am-59, Cd-Kα,esc 10) Am ) Compton reprocessing of ) Am-59 13) Np-Kα 1, Daniel Maier E [kev]
26 CANDELA: a stacked setup x 0/0 63/0 y 7/7 7/0 x 0/7 y 0/0 63/63 0/63 LED HED HED LED heating HED + LED absorption mutual influences? electrical crosstalk 26 Daniel Maier fluorescence
27 LED-HED mutual influences electrical cross talk heating absorption fluorescence 27 Daniel Maier S. Pürckhauer, 2015
28 LED-HED mutual influences electrical cross talk heating absorption fluorescence 28 Daniel Maier S. Pürckhauer, 2015
29 LED-HED mutual influences fluorescence: - no Si fluorescence in the HED fluorescence yield photon flux F [1/(s * kev * cm 2)] - Cd and Te fluorescence in the LED total singles doubles triples quadruples gcmx = 33 % Cd Kα1, Te Kα 1, Daniel Maier E [kev]
30 LED-HED (positive) interactions time coincident events - LED fluorescence HED escape canceling the fluorescence peaks in the LED - reducing the escape peaks in the HED by 25.4 % - reducing the low energetic background in the LED caused by compton forward scattering - CANDELA: Δt = 3.0 ms S. Pürckhauer, Daniel Maier
31 Compton forward scattering Compton scattering in the LED θmin = 0 31 Daniel Maier sc. photon escapes the LED sc. photon is directed to the HED sc. photon is detected by the HED
32 Compton forward scattering Compton scattering in the LED 32 Daniel Maier sc. photon escapes the LED sc. photon is directed to the HED sc. photon is detected by the HED
33 Compton forward scattering Compton scattering in the LED 33 Daniel Maier sc. photon escapes the LED sc. photon is directed to the HED sc. photon is detected by the HED
34 Compton forward scattering Compton scattering in the LED 34 Daniel Maier sc. photon escapes the LED sc. photon is directed to the HED sc. photon is detected by the HED
35 Compton forward scattering Compton scattering in the LED θmin = 0 35 Daniel Maier sc. photon escapes the LED sc. photon is directed to the HED sc. photon is detected by the HED
36 Compton camera 36 Daniel Maier
37 Compton polarimeter 37 Daniel Maier
38 Compton polarimeter 38 Daniel Maier
39 Statistics & polarimetry instrument degree of polarization angle of polarization source point estimations 39 Daniel Maier observation interval estimations
40 Statistics & polarimetry instrument degree of polarization angle of polarization interval estimations source observation Maier et al. 2014: Point and interval estimations for the degree and the angle of polarization. A Bayesian approach. 40 Daniel Maier
41 Perspective: ASTRO-H soft X-ray imager SXI soft X-ray spectrometer SXS hard X-ray imager HXI soft gamma ray detector SGD supported by ESA & CNES launch km LEO m = 2.4 t L = 14 m 41 Daniel Maier
42 Comparison CANDELA setup Si + CdTe pixelized detectors timing: 3 ms 42 Daniel Maier ASTRO-H setup CdTe + CdTe strip detectors timing: ~ 1 μs to do (hardware): - adding the 2nd detector - test long term operation
43 To do: (Science) HXI & SGD proposals AGN & CXB polarization 43 Daniel Maier
44 Thank you. Contact: Daniel Maier room: P Daniel Maier
45 Astrophysical X-ray sources active galactic nuclei (AGN) - X-ray sources: - soft X-ray emission of the disc inv. Compton scattering in the corona fluorescence emission of the disc ~6.4 kev Compton reflection hump ~30 kev fields of research accretion on SMBH galaxy evolution feedback on the interstellar & intracluster medium 45 Daniel Maier Centaurus A, Chandra observation NASA/CXC/CfA/R. Kraft et al.
46 LED configuration dark-frame measurement update EPP (normal mode) flat-field measurement bad1 map offset map energy-threshold map neighbor-threshold map offset map 46 Daniel Maier update EPP source measurement bad2 map noise map bad map
47 LED analysis: bad pixel A B C D E F accepted legal event accepted but possibly illegal pattern rejected legal event rejected but possibly legal event rejected (possible split event) rejected (possible illegal pattern) 47 Daniel Maier
48 LED data analysis: bad pixel A B C D E F accepted legal event accepted but possibly illegal pattern rejected legal event rejected but possibly legal event rejected (possible split event) rejected (possible illegal pattern) A+B+C 48 Daniel Maier A+B
49 LED spectra 49 Daniel Maier
50 LED Am spectrum 50 Daniel Maier
51 HED: polarization effect CdTe: many mid-gap levels band bending due to Schottky contact increased nion rearrangement of the electric field inside the crystal 51 Daniel Maier
52 HED: polarization effect spectroscopic effect - reduced charge collection efficiency - reduced quantum efficiency 52 Daniel Maier
53 LED: Geant4 simulation credit: S. Pürckhauer, Daniel Maier
54 CANDELA: Compton kinematics 54 Daniel Maier
55 LED energy calibration Eoff = -50 ev Eoff = +60 ev Eoff = +100 ev photon flux F [(s kev cm ² ) ] 1000 Eoff = 0 ev total singles doubles triples quadruples Daniel Maier E [ev] E [ev] E [ev] E [ev]
56 Compton forward scattering photoelectric absorption detection of time coincident events Compton electron must be detected by the LED CAMEX gain 56 Daniel Maier
57 Compton polarimeter modulation factor: C max C min max+c min μ=c 57 Daniel Maier
58 Compton polarimeter (Muleri & Campana, 2012) 58 Daniel Maier
59 Summary and outlook LED 64x64 - energy range: 150 ev 15keV ΔE = kev ΔE = kev systematic error < 100 ev for 6 kev < E < 28 kev Δt = 2.44 ms window mode HED 8x8 energy range: kev - ΔE = 1 60 kev - systematic error < 100 ev for 14 kev < E < 60 kev - Δt < 7 μs - broad band energy range: 150 ev < E < 150 kev status: time coincident events can be measured - next: Compton camera test the 3d source positioning study the imaging accuracy interval estimations? - next, next: Compton polarimeter validate the predicted modulation factor check the predicted point and interval estimations 59 Daniel Maier
arxiv: v1 [physics.ins-det] 11 Dec 2015
Energy calibration via correlation Originally published in Nuclear nstruments and Methods in Physics Research Section A, 206 (DO: 0.06/j.nima.205..49) Daniel Maier, Olivier Limousin CEA Saclay, DSM/rfu/Service
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