MPE's views on SDDs as focal plane detectors for SFA - Overview: - - PowerPoint PPT Presentation

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mpe s views on sdds as focal plane detectors for sfa
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MPE's views on SDDs as focal plane detectors for SFA - Overview: - - PowerPoint PPT Presentation

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eXTP meeting (eXTP: enhanced X-ray Timing and Polarization mission) Shanghai, 30th March 1st April 2016 MPE's views on SDDs as focal plane detectors for SFA - Overview: MPE HEG space projects XMM-Newton EPIC-PN, eROSITA, Athena WFI - Our

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SLIDE 1

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

MPE's views on SDDs as focal plane detectors for SFA

  • Overview: MPE HEG space projects

XMM-Newton EPIC-PN, eROSITA, Athena WFI

  • Our concepts for spectroscopic detectors
  • Our SDDs as focal plane detectors
  • principle – features – details – examples

eXTP meeting

(eXTP: enhanced X-ray Timing and Polarization mission) Shanghai, 30th March – 1st April 2016

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SLIDE 2

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE
  • First generation of PNCCDs:
  • developed for X-ray astronomy: XMM-Newton
  • Satellite launch: 1999
  • Pixel size: 150µm x 150µm (4.1 arcsec)
  • 12 CCDs: 64 x 200 pixels
  • Long term stability of pnCCD detector

(EPIC-PN camera) aboard XMM-Newton:

  • all 12 CCDs are still operating
  • same operating parameters (T = -90°C)
  • quantum efficiency unchanged
  • slight radiation damage as expected: CTI

MPE HEG space projects

ESA XMM-Newton with PNCCD camera (1999 – today)

∆FHHM/FWHM < 2eV/155eV/y≈ 1%/y

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SLIDE 3

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

MPE HEG space projects

XMM-Newton PNCCD camera

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SLIDE 4

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

f=1600 mm eROSITA

eROSITA (extended Roentgen survey with an imaging telescope array)

  • all-sky survey: 4 y (/7.5y)
  • soft band: 30 x sensitivity of ROSAT
  • hard band (>2keV): first all-sky survey
  • test of cosmological model (Dark Energy)
  • eROSITA telescope developed unter

responsibility of MPE

  • Wolter-I mirror system: 54 shells
  • PSF: 15‘‘ resolution (HEW) on-axis
  • FoV: 1.0° diam.
  • Russian SRG satellite → L2 orbit (2017)

4

MPE HEG space projects

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SLIDE 5

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

advanced type of XMM-Newton PNCCD back-illuminated frame-transfer CCD chip thickness (= 450 µm) fully sensitive image: 384 x 384 pixels of 75 x 75 µm2 size column-parallel: 384 independent channels frame transfer: 0.12 ms CAMEX: analog signal processor readout time: 9 ms time resolution: 50 ms

  • on-board event processing
  • minimiz. heat dissipation (≈ 80% standby) → 0.7 W

OOT events ≈ 0.2% excellent low energy response

eROSITA PNCCD Detector

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SLIDE 6

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

eROSITA detector:

  • PNCCD
  • eROSITA CAMEX
  • Multi-layer detector board
  • Flexible lead as I/F to CE

Detector housing:

  • Mech. + thermal I/F
  • Graded Z-shield: Be/B4C - Al - Cu
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SLIDE 7

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Filter wheel

Camera Head Camera Electronics Array of 7 PNCCD focal plane cameras:

MPE HEG space projects

eROSITA with 7 PNCCD cameras on SRG satellite

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SLIDE 8

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Energy resolution

55Fe spectrum: FWHM(5.9keV) = 131 eV Mn-Kα Mn-Kβ Mn-Kα Mn-Kβ Al-K Si escape peaks

Signal spread over up to 4 pixels

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SLIDE 9

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Intensity distribution over image area Al-K of X-ray tube (QM_140123_06)

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SLIDE 10

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Sensor PNCCD Illumination type back-illumination Image area 384 x 384 pixels Pixel size 75 µm x 75 µm (< 10 arcsec) Readout ASIC 128-channel eROSITA CAMEX (3 ASICs per PNCCD) Read noise 2.4 electrons ENC rms Energy resolution FWHM(0.53 keV) ≈ 62 eV FWHM(5.9 keV) ≈ 140 eV Operating temperature

  • 95°C (best wrt radiation damage)

Quantum efficiency E = 1 keV: 89% (on-chip-filter) E = 5 keV: 99% (on-chip filter) Readout time 9.2 ms Time resolution 50 ms

eROSITA PNCCD detector characteristics

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SLIDE 11

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

11

Wide Field Imager:

  • unprecedented survey power (FoV = 40`x40`)
  • high count-rate capability (1 Crab)
  • E=[0.2 keV – 15 keV] state-of-the-art energy resolution
  • focal plane detectors: DEPFET APS

(enhanced type of DEPFET MIXS detector for BepiColombo)

  • WFI consortium with MPE as lead institute

Mirror system: f = 12 m Aeff ≈ 2 m² at 1 keV X-IFU: X-ray micro- Calorimeter ∆E=2.5eV T=50mK

MPE HEG space projects

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SLIDE 12

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

MPE HEG space projects

Wide field imager (WFI) for ESA‘s Athena

Heritage: MIXS on BepiColombo

DEPFET APS Detectors for WFI on Athena

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SLIDE 13

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

13

Focal plane layout

Pointing on large or fast WFI detector Large FoV detector

  • 40` x 40` by 1024 x 1024 pixel

↔ Size ≈ 14 x 14 cm2

  • 4 independent + identical quadrants
  • requirement: <5ms/frame

→ <10µs/row

  • 2-side buttable DEPFETs

High count-rate capable detector

  • FoV = 143`` x 143``

↔ Size ≈ 8.3 x 8.3 mm2

  • 64 x 64 pixels subdivided in 2 halves
  • requirement: 80µs/frame

→ 2.5µs/row

  • mounted defocussed
  • Pixel: 130 µm x 130 µm (↔ 2.23``)

⇒ accurate source position reconstruction (splits!) for PSF = 5ʾʾ HEW

  • Control ASIC: 3-port Switcher-A
  • Readout ASIC: VERITAS-2
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SLIDE 14

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

14

Parameter Value Energy Range 0.2-15 keV Field of View 40’ x 40’ Angular Resolution Pixel Size PSF=5`` (on-axis) 130 x 130 µm2 (2.2``) Large DEPFET detector 1024 x 1024 pixel (4 quadrants) =14cmx14cm Fast DEPFET detector 64 x 64 pixel (split full frame mode - 2 halves readout) Operating mode Rolling shutter Operating time Nonstop possible Quantum efficiency (on-chip + ext. filter w. mesh) 20% @ 277 eV 80% @ 1 keV 90% @ 10 keV Energy Resolution FWHM(1 keV) ≤ 80 eV (end of life) FWHM(7 keV) ≤ 170 eV (end of life) Time Resolution full frame Fast detector Large detector 80 μs <5 ms Count Rate Capability Fast DEPFET (defocused) 1 Crab: >80% throughput, <1% pile-up Particle Background (L2 orbit) < 5 × 10-3 cts cm-2 s-1 keV-1 Lifetime 5 y + extension (launch 2028)

Main WFI Requirements / Characteristics

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SLIDE 15

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE
  • SDD detectors produced at MPI HLL

NASA Mars Rovers:

  • SPIRIT and OPPORTUNITY (01/2004)
  • CURIOSITY (08/2012)
  • ESA's Rosetta (67P/Tschurjumow-Gerasimenko)
  • µRosi on Max Vallier satellite

Space projects with SDD detectors produced at MPI HLL

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SLIDE 16

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Our concepts for spectroscopic detectors

Features:

  • Ultrapure FZ silicon wafers (∅ = 150 mm)
  • Double-sided processing permits full depletion of 450 µm Si

→ high QE at high X-ray energies

  • First stage of signal amplification (transistor) integrated on-chip

→ low readout noise

  • Back-illuminated detectors → uniform QE over detector area
  • Shallow p-implant of photon entrance window

→ high QE at low energies + high p/b ratio

  • Deposition of on-chip light filter (Al) → "no" signal by visual light
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SLIDE 17

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Fe-Kα

Quantum efficiency

450 µm Si 300 µm Si

no on-chip light filter

Our concepts for spectroscopic detectors

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SLIDE 18

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Mn-Kα Mn-Kβ

Energy resolution

55Fe spectrum:

FWHM(5.9keV) = 130 eV

E = 200eV

BESSY synchrotron:

FWHM(200eV) = 52 eV

Gaussian shape !

(measured with eROSITA PNCCD but similar for the other detectors)

Our concepts for spectroscopic detectors

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SLIDE 19

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Our concepts for spectroscopic detectors

  • Concept requires adequate

process technology →developed at MPI HLL

  • Basic spectroscopic detector concepts:
  • Silicon drift detectors

readout node / cell time resolution: µs → fastest spectroscopic detector spatial resolution possible by array of SDD cells

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SLIDE 20

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Our concepts for spectroscopic detectors

  • PNCCD

full-column-parallel CCD: readout node / ch. time resolution: ms → spectroscopic + imaging detector

  • DEPFET active pixel sensor

readout node / pixel CCD-like but even faster + more radiation hard → window mode (readout of selected sensor rows)

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SLIDE 21

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

SDD principle & development

  • riginal concept

by Gatti & Rehak, 1983  depleted volume  transverse electric field  particle tracking

  • n-chip transistor

HLL, 1993  integration of first amplification stage

spectroscopy adaptation

by Kemmer & Lutz, 1984  uniform back contact = entrance window

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SLIDE 22

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE
  • SDDs developed and produced at MPI HLL (MPE & MPP + Ketek + PNSensor)
  • Drift rings with nJFET in "center"
  • Integration of first transistor on-chip

→ robustness wrt microphonic noise + electrical pickup

  • Small capacitance 35fF → low noise level + high count rate capability
  • Depletion voltage ≈ -100 V
  • Cell area: 5 mm2 … cm2
  • good peak-to-valley ratio

≈ 15.000:1 (for SD3 with int. collimator)

Our SDD features

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SLIDE 23

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE
  • Example: 10 mm2 SDD, T=-17°C, 1 µs shaping, pulsed reset 1kHz:

FWHM(5.9keV) ≈ 134 eV @ 105 photons / s

  • Array of SDD cells, e.g. 7, 19 or 31 cells

SDD 19 x 5 mm² XTRA on XEUS

SDD features

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SLIDE 24

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Concept for HTRS on IXO

  • International X-ray Observatory (IXO) proposal/studies:

High Time Resolution Spectrometer (HTRS)

  • 31 SDD cells
  • Time resolution: 10 µs
  • Energy resolution: FWHM(5.9 keV) = 150 eV (T=-40°C, beginning of mission)
  • Detector size: 24 mm diameter, 4.5 cm2 area
  • Cell size: 14.6 mm2

Spider web baffle:

  • for suppression of split events
  • area coverage: 10%
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SLIDE 25

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

SDD very radiation tolerant

 min. contribution of dark curr. (no signal storage like CCD or DEPFET)  JFET rad hard

  • X-rays up to 1013 absorbed photons (Mo-K, 18 keV)

→ w/o degradation of energy resolution

  • protons → increase of dark current

Extreme example: HTRS/IXO (15mm Al): equiv. 5·109 10-MeV proton/cm² in 10 y Model based on exp. results: → FHWM(5.9 keV) ≤ 250 eV @ T=-40°C end of mission (spec. 300 eV) for Acell=14.6 mm2

SDD radiation hardness

Don‘t forget: shielding + cooling (depends on orbit eXTP: LEO 550km, incl. 14°  Mission duration: 5 y) HTRS/IXO

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SLIDE 26

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Silicon Drift Detectors in Space produced at MPI HLL

→ analysis of chemical composition of surface APXS (Alpha-Particle X-ray Spectrometer)

  • n NASA’s Mars Exploration

Rovers Spirit and Opportunity

landed Jan 04, Opportunity still active (in 2014) APXS "sniffer" by MPCh, Mainz SDD 10 mm² & Cu244 α-sources

APXS on ROSETTA Lander

rendezvous with comet 67P/ C-G (Churyumov-Gerasimenko) Mar04, orbit Sept14, Lander philae 12Nov14

  • nly short period of operation

Mars Exploration Rover APXS system (MPCh)

APXS

  • n NASA Mars Science Laboratory

Rover Curiosity

landed August 2012 with Peltier cooler

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SLIDE 27

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

µrosi on Max Valier satellite

Miniature X-ray telescope

  • Eff. area: 4.1cm2 @ 1.25keV

SDD @ T=-15°C

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SLIDE 28

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE
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SLIDE 29

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

µrosi detector calibration in PUMA @ MPE

T=-15.5°C SDD specs:

  • 450 µm thickness
  • 20 mm2 active area
  • collimator
  • FWHM(5.9keV) = 128eV @ T=-20°C
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SLIDE 30

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

SFA requirements:

E = [0.5keV; 20keV]  FWHM(6keV) < 180eV end of life → shielding + cooling (depends on orbit)  Timing resolution: 10µs  11 SFA units  How many SDD cells are necessary per SFA unit?

  • Inner cell(s) for source photons and
  • uter ring for diffuse+instrumental background

(large number requires multi-ch. ASIC for readout inst. of discrete compon.)

Which cell size is optimum?

  • depends on PSF of mirrors (→ cell size tailored to SFA)

Technical budgets for SFA camera incl. shielding + electronics? Mass, power, volume, radiator area, …

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SLIDE 31

eXTP meeting, Shanghai 30 March – 1 April 2016

  • N. Meidinger, MPE

Small SDD cell arrays

Gravitas proposal 1 + 4 cells Source photons + background 1 + 6 cells (core of 31 cells for HTRS/IXO) 7 instead of 19 cells (XTRA/XEUS)