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X-ray imaging spectrometers in present and future satellite missions. Peter Lechner MPI Halbleiterlabor & PNSensor GmbH. 1. X-ray imaging spectrometers in present and future satellite missions. MPI Semiconductor Lab X-ray Astronomy pnCCD XMM-Newton Framestore pnCCD ROSITA - PowerPoint PPT Presentation
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P. LechnerIWORID 2002
Peter Lechner
MPI Halbleiterlabor & PNSensor GmbH
1
X-ray imaging spectrometers in X-ray imaging spectrometers in present and future satellite missionspresent and future satellite missions
P. LechnerIWORID 2002
• MPI Semiconductor Lab
• X-ray Astronomy
• pnCCD XMM-Newton
• Framestore pnCCD ROSITA
• Active Pixel Sensor XEUS
• Conclusion
100 % personally biased
apologies!
1
X-ray imaging spectrometers in X-ray imaging spectrometers in present and future satellite missionspresent and future satellite missions
P. LechnerIWORID 2002
MPI semiconductor laboratory• common institution of the Max-Planck-Institutes for
Physics and for Extraterrestrial Physics
• founded in 1992
• 35 scientists, engineers, technicians, students
strip detectors for ALEPH/CERN
• development of novel detectors
high energy physics
ALEPH, ATLAS @ CERN
HERA-B, TESLA @ DESY
astrophysics
XMM-Newton, XEUS, ROSITA, MEGA, SVOM
related fieldssynchrotron radiation experiments
technology transferSilicon Drift Detectors for X-ray spectroscopy
industrial applications 2
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
pnCCD camera for XMM-Newton
• development of novel detectors
high energy physics
ALEPH, ATLAS @ CERN
HERA-B, TESLA @ DESY
astrophysics
XMM-Newton, XEUS, ROSITA, MEGA, SVOM
related fieldssynchrotron radiation experiments
technology transferSilicon Drift Detectors for X-ray spectroscopy
industrial applications 2
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
MPI semiconductor laboratory• common institution of the Max-Planck-Institutes for
Physics and for Extraterrestrial Physics
• founded in 1992
• 35 scientists, engineers, technicians, students
P. LechnerIWORID 2002
Silicon Drift Detector Array for EXAFS, X-ray holography
• development of novel detectors
high energy physics
ALEPH, ATLAS @ CERN
HERA-B, TESLA @ DESY
astrophysics
XMM-Newton, XEUS, ROSITA, MEGA, SVOM
related fieldssynchrotron radiation experiments
technology transferSilicon Drift Detectors for X-ray spectroscopy
industrial applications 2
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
MPI semiconductor laboratory• common institution of the Max-Planck-Institutes for
Physics and for Extraterrestrial Physics
• founded in 1992
• 35 scientists, engineers, technicians, students
P. LechnerIWORID 2002
Silicon Drift Detector modules for X-ray fluorescence analysis
and electron microprobe analysis
• development of novel detectors
high energy physics
ALEPH, ATLAS @ CERN
HERA-B, TESLA @ DESY
astrophysics
XMM-Newton, XEUS, ROSITA, MEGA, SVOM
related fieldssynchrotron radiation experiments
technology transferSilicon Drift Detectors for X-ray spectroscopy
industrial applications
KETEK GmbH
2
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
MPI semiconductor laboratory• common institution of the Max-Planck-Institutes for
Physics and for Extraterrestrial Physics
• founded in 1992
• 35 scientists, engineers, technicians, students
P. LechnerIWORID 2002
MPI semiconductor laboratory
... with modern, custom made facilities ...... for a full 6-inch silicon process line 800 m² cleanroom up to class 1 ...
mounting & bonding test & qualification simulation, layout & data analysis
3
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
X-ray astronomy
4
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
access to hot matter and energetic processes
supernovae
X-ray bursters
neutron stars
X-ray binaries
pulsars
black holes
quasars
P. LechnerIWORID 2002
X-ray astronomy - instrumentation
5
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
telescope
• collimator, coded mask
• mirror telescope ´Wolter-I´
grazing angle reflection
• (microchannel plate)
XMM mirrors
P. LechnerIWORID 2002
X-ray astronomy - instrumentation
5
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
telescope
• collimator, coded mask
• mirror telescope ´Wolter-I´
grazing angle reflection
• (microchannel plate)
focal plane
• proportional counter
• CCD
ASCA, Chandra, XMM-Newton
• APS
XEUS
• (high-Z semiconductors, cryogenic detectors)
XMM-Newton
Chandra
P. LechnerIWORID 2002
pnCCD principle
MOS-CCD (´video CCD´)
• MOS transfer gates
• buried channel
• partial depletion
• frontside illumination
• serial readout
6
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
pnCCD principle
MOS-CCD (´video CCD´)
• MOS transfer gates
implanted pn-junctions
• buried channel
deep transfer
• partial depletion
full depletion
• frontside illumination
back entrance window
• serial readout
1 preamp / channel
pnCCD6
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
pnCCD performance
• largest monolithic CCD
6 x 6 cm²
384 x 400 pixel
150 µm pixel
• fast readout
5 msec full frame
• low noise
4 el. rms
• high quantum efficiency
90 %
• radiation hard
400 Mp/cm²
7
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
pnCCD performance
7
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
• largest monolithic CCD
6 x 6 cm²
384 x 400 pixel
150 µm pixel
• fast readout
5 msec full frame
• low noise
4 el. rms
• high quantum efficiency
90 %
• radiation hard
400 Mp/cm²
P. LechnerIWORID 2002
pnCCD performance
7
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
• largest monolithic CCD
6 x 6 cm²
384 x 400 pixel
150 µm pixel
• fast readout
5 msec full frame
• low noise
4 el. rms
• high quantum efficiency
90 %
• radiation hard
400 Mp/cm²
P. LechnerIWORID 2002
pnCCD performance
7
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
• largest monolithic CCD
6 x 6 cm²
384 x 400 pixel
150 µm pixel
• fast readout
5 msec full frame
• low noise
4 el. rms
• high quantum efficiency
90 %
• radiation hard
400 Mp/cm²
P. LechnerIWORID 2002
pnCCD vs. MOS-CCDs
typereadout
time[msec]
pixel cell size[µm²]
detector size[cm²]
MIT/LL-FI 60 130 3 20 500 24 x 24 2.5 x 2.5MIT/LL-BI 125 200 50 10 500 24 x 24 2.5 x 2.5
Leicester 80 130 25 30 500 40 x 40 2.4 x 2.4SRON 100 145 65 15 500 27 x 27 2.8 x 2.8
pnCCD 70 130 90 90 4,6 150 x150 6 x 6
XMM
energy resolution@ 272 eV & 5.9 keV
FWHM [eV]
quantum efficiency@ 272 eV & 10 keV
[%]
CHANDRA(original)
backside illumination
full depletion
large pixels, parallel readout
8
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
XMM-Newton – the satellite
• 3 imagers
2 MOS-CCD + RGS
1 pnCCD
pointing at one source
• energy range
0.1 ... 15 keV
• Wolter-I telescopes
58 nested mirror shells
eff. area 0,5 m² (1 keV)
focal length 7,5 m
FOV 30 arcmin
resolution 15 arcsec
• highly excentric orbit
48 h
perigee: 7.000 km
apogee: 114.000 km
9
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
XMM-Newton – integration & launch
10
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
• mounting of pnCCD camera
• satellite integration
• mirror system
P. LechnerIWORID 2002
10
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
• launch by ARIANE-V from Kourou
10–Dec–1999
• XMM-Newton in orbit
XMM-Newton – integration & launch
P. LechnerIWORID 2002
XMM-Newton – first light
large Magellanic cloud
supernova remnant
1987A
11
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
XMM-Newton - observations
remnant of supernova
observed by Tycho Brahe
in 1572
energy [keV]
rela
tive
inte
nsity
element distribution
12
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
XMM-Newton - observations
Lockman hole:
a look into deep space
first observation of
´green´ and ´blue´
hard x-ray sources
no diffuse background?
12
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
pnCCD – performance in space
• perfect imaging since launch
• 500 revolutions
> 1000 observations
• no significant change of
energy resolution and
charge transfer efficiency
• few pixels lost in rev. 156
impact of micro-meteorite?
• effect reproduced on ground
using a dust accelerator 13
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
pnCCD - limitation
charge transfer speed limited
by the time needed for readout
´out of time´ events
pnCCD: ~ 6 %
14
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
framestore pnCCD
• frame store area
separation transfer / readout
reduction of out-of-time events
6 % (XMM) 0.4 %
• prototypes under test
smaller pixels (75 µm)
improved performance
15
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
ROSITA - ROROentgen SSurvey with an IImaging TTelescope AArray
point sources
diffuse background
16
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
XEUS – X-ray Evolving Universe Spectroscopy
17
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
• X-ray telescope with large aperture
energy range 100 eV ... 30 keV
• scientific aim:
investigation of the universe
at an early evolution stage
• two spacecrafts
- mirror spacecraft
Wolter-I telescope
effective area: 6 m² (30 m²) @ 1keV
- detector spacecraft
• focal plane instrumentation
- 2 narrow field imagers
- 1 wide field imager
P. LechnerIWORID 2002
XEUS WFI vs. XMM-Newton
XMMXMM XEUS WFIXEUS WFI
energy range 0.1 ... 15 keV 0.1 ... 20 keV thickness 300 µm 500 µm
focal length 7.5 m 50 m
angular resolution 15 arcsec 2 arcsec
focal plane res. 36 µm / arcsec 250 µm / arcsec pixel size 150 µm 75 µm
field of view 30 arcmin 5 arcmin detector area 6 x 6 cm² 7.6 x 7.6 cm²
collection area 1keV 0.5 m² 6 m² (30 m²) readout speed
time resolution 70 msec 1 ... 5 msec readout speed
operating temp. 130 K > 180 K
Active Pixel Sensor
1 integrated preamp / pixel
random accessible pixels
no charge transfer within
silicon18
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
DEPFET – DEDEpleted PP-channel FField EEffect TTransistor
19
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
• p-FET (JFET or MOSFET) on depleted n-Si bulk
• local potential minimum for electrons ‘internal gate‘
• current change prop. to number of charges in the ‘internal gate‘I > 200 pA / electron
• nondestructive readout
• charge integration and storagein ON and OFF state
• reset through clear contact, supported by clear gate
• backside illuminated
P. LechnerIWORID 2002
DEPFET – simulation
20
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
DEPFET – active pixel sensor
21
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
DEPFET – active pixel sensor
22
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
DEPFET – active pixel sensor
BioScope for autoradiography (University Bonn)
23
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
DEPFET – status
• test of isolated pixel
JFET-based DEPFET
L = 5 µm, W = 50 µm
time-continuous filter
______________________
• production of APS
prototypes 64 x 64
• new readout chip
under test
• new control chip
submitted24
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
P. LechnerIWORID 2002
Conclusion
25
MPI laboratory
X-ray astronomy
pnCCD
framestore pnCCD
active pixel sensor
conclusion
X-ray astronomy
driving force in semiconductor detector development
novel detectors
new view to the X-ray sky
... no end in sight ...
P. LechnerIWORID 2002
ThanksL. Andricek, D. Hauff, P. Klein*, G.Lutz, R.H. Richter, M. Schnecke, P. Solc*
Max-Planck-Institut für Physik, Munich, Germany
H. Bräuninger, S. Bonerz, U. Briel, K. Dennerl, J. Englhauser, G. Hartner, G. Hasinger, T. Johannes*, S. Kemmer*, J. Kollmer,
N. Krause*, N. Meidinger, E. Pfeffermann, E. Ruttkowski, G. Schaller, F. Schopper, D. Stötter*, L. Strüder, J. Treis, J. Trümper
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany
R. Eckard, R. Hartmann, K. Heinzinger, P. Holl, P. Lechner, H. Soltau, U. Weichert
PNSensor GmbH, Munich, Germany
N. Findeis*, J. Kemmer, S. Krisch*, R. Stötter, U. Weber*
KETEK GmbH, Munich, Germany
E. Kendziorra, K. Kramer, R. Staubert
Astronomisches Institut Tübingen, Tübingen, Germany
P. Fischer, W. Neeser*, I. Peric, M. Trimpl, J. Ulrici, N. Wermes
University of Bonn, Bonn, Germany
W. Buttler
Ingenieurbüro Buttler, Essen, Germany
E. Gatti, A. Longoni, M. Sampietro
Politecnico di Milano, Milan, Italy
P. Rehak
Brookhaven National Laboratory, Upton, NY, USA
26