high speed cmos photon detectors and cameras
TRANSCRIPT
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High speed CMOS photon detectors and
cameras
Mark Downing, Paola Amico, Martin Brinkmann, Mark Casali, Ralf Conzelmann, Christoph
Geimer, Enrico Marchetti, Ignacio Molina-Conde, Leander Mehrgan, Javier Reyes, Matthias
Seidel, Joerg Stegmeier, Mirko Todorovic
European Southern Observatory ESO (http://www.eso.org)
1EIROforum CIS26 Jun 2018
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Outline
• Adaptive Optics Wavefront Sensing
• Camera Program
• CCD220
• LVSM CMOS Imager
• Visible Camera Design
• Summary
2EIROforum CIS26 Jun 2018
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Adaptive Optics (AO)- removing the twinkle of the stars
Wavefronts from astronomical
objects are distorted by the Earth’s
atmosphere, reducing the spatial
resolution of large telescopes to
that of a 10 cm telescope
1
Wavefront Sensor
measures deviation of
wavefront from a flat
(undistorted) wave
2Control System
computes
commands for the
deformable mirror(s)
3
Deformable mirror
compensates the
distorted wavefront,
achieving diffraction-
limited resolution 4
OFF
ON
3EIROforum CIS26 Jun 2018
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AOF GLAO
26 Jun 2018 EIROforum CIS 4
* http://www.eso.org/public/news/eso1724/
IC 4406 -> Retina Nebula
planetary nebula NGC 6563
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38 m diameter
65 m high
Deformable
Mirror
Instruments
WFS adaptor
WFS arms
(contain WFS
detectors)Some
instruments
also contain
WFS detectors
WFS adaptor
Location of Wavefront sensors
on the ELT
EIROforum CIS 526 Jun 2018
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While the Telescope is large, the volume
for cameras are modest
26 Jun 2018 EIROforum CIS 6
Space for cameras limited
Cameras
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Outline
• Adaptive Optics Wavefront Sensing
• Camera Program
• CCD220
• LVSM CMOS Imager
• Visible Camera Design
• Summary
7EIROforum CIS26 Jun 2018
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Three WFS Cameras under development
26 Jun 2018EIROforum CIS
8
Visible
Extremely low noise (0.1e-)
small format (240x240) → CCD2201)
Large format (>800x800)
modest noise (3e-) → LVSM2)
All share requirements of high speed (700-1000fps), low noise/dark current,
high QE, large 24µm pixel
NIR
Low noise (1e-)
small format (320x256) → SAPHIRA3)
n
HgCdTe
Si Multiplexer
Absorber
Gain
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Outline
• Adaptive Optics Wavefront Sensing
• Camera Program
• CCD220
• LVSM CMOS Imager
• Visible Camera Design
• Summary
9EIROforum CIS26 Jun 2018
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Existing Teledyne-e2v CCD220-DD
26 Jun 2018 EIROforum CIS 10
Store
Area
Image
Area
240x12024□µm
Store
Area
Image
Area
240x12024□µm
OP 1
OP 2 GainRegisters
OP 3
OP 4 GainRegisters
OP 8GainRegisters
OP 7
OP 6GainRegisters
OP 5
e2v CCD220: Tried and proved
240x240 24 µm pixels
8 L3Vision Electron Multiplication outputs
< 0.1 e- RoN at > 1,000 fps
Integral Peltier package to cool to -40ºC
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Outline
• Adaptive Optics Wavefront Sensing
• Camera Program
• CCD220
• LVSM CMOS Imager
• Visible Camera Design
• Summary
11EIROforum CIS26 Jun 2018
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Large Visible AO WFS Detector needed
to sample the spot elongation
12
Sodium Laser Guide Stars
• Frame rate ~1 kframe/sec
→ require bright “guide stars”
• With natural guide stars only
1% of the sky is accessible
• Sodium layer at 80-90 km
altitude can be stimulated by
Laser to produce artificial
guide stars anywhere on the
sky
LLT
Sodium
layer
Detector
plane
T ~ 10km
H ~ 80km
Distance from
launch site
Pupil
plane
Predicted spot
elongation pattern
EIROforum CIS26 Jun 2018
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¼ WFS image
EIROforum CIS 13
26 Jun 2018
• Would like 80x80 sub-apertures of 25x25
pixels to fully sample the spot elongation
2kx2k pixels,
• CCD220 not scalable → CMOS Imager
however,
• to ensure devices available on-time for first
light instruments, 80x80 sub-apertures of
10x10 pixels 800x800 pixel Large Visible
Sensor Module, LVSM, being developed as first
step
• Studies underway to develops techniques of
how to handle truncation of spot elongation or
use pixels more efficiently
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LVSMCustom Development by Teledyne-e2v
CMOS Imager with Highly integrated readout
• 800x800 continuous array of 24µm pixels
• 700fps at < 3e- read noise
• Backside illuminate for high QE: > 90% at 589nm
• All analog processing on-chip:
– correlated double sampling (CDS),
– programmable gain of x1/2/4/8 settable on the fly,
– 9/10 bit single slope ADCs,
– for total effective 12 bit data conversion
• 4 rows top + bottom processed in parallel to slow the
read out per pixel and beat down the noise
– 14us/row = 12µs to sample the analog + 2µs ADC
• 24 line at 256Mbit/sec LVDS serial interface to
outside world
– simple easy digital interface to FPGA
26 Jun 2018 EIROforum CIS 14
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Photodiode Design
• No white spots - uniform intrapixel response– high QE – good PSF – low image lag
• Photodiode - double-N implant:
1. a large square implant to guarantee uniform response and good PSF
2. a tapered finger implant, that provides a potential gradient towards the TG, to improve image lag
• At least 50% area of reflective metal to give high QE in the “red”
• Back-illuminated, high resistivity silicon >1000 ohm-cm, multi-2 AR Coating
• 12 µm thick:
– best trade between PSF and QE → validated in a previous prototype
26 Jun 2018 EIROforum CIS 15
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Highly Parallelized Readout
• At top and bottom, in the shadow of each pixel column, is a
single row of four readout channels (each 4µm wide) for total of
(4x840) 3360 channels across the device.
– Clean/simple layout with good separation and no capacitive
cross-coupling between analog and digital signals
– Good synchronicity and low latency within a 10x10 pixel
sub-aperture (< 2% of exposure time)
26 Jun 2018 EIROforum CIS 16
Read out direction
compatible for both
Shack Hartmann and
pyramid WFS
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Video Chain – single slope ADC
26 Jun 2018 EIROforum CIS 17
comparator output
Gray code
ramp
offset
0 512
Latch code
videoreset
signal
transfer
reset
Column bus
1
VRST VSF
reset
p-Si
2
transfer
4
n+
p+
3
select
4T pixel
SNPPD
x2 x4 x8
-
+
Pre-Amp
x1
LVDS Out
Parallel to Serial
mux
Ramp
VDD_SH
VSS_SH
/Ramp
shr
shs
Sample/Hold
Comparator
D Q
Clk
Gray Code
9/10
B-
+
D Q
Clk
Ping Pong Latches
A
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LVSM package - developed with ease of use in mind
• LVSM comes in a integral Peltier package to cool to < -10ºC
• Flat metal base with holes for firmly bolting to heat exchanger
• Kovar body filled with low thermal conductive Krypton gas
• Temperature sensor mounted on chip ceramic carrier
• IPGA array for electrical connections
• Mating socket soldered to flex circuit
26 Jun 2018 EIROforum CIS 18
Pump
Tube
Window
Lid
LVSM glued to
Ceramic insert
Temperature
Sensor
Peltier
Kovar
Body
Peltier pins
IPGA
Ceramic
IPGA
Bracket
Mating IPGA
Socket
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LVSM Required Performance
Pixel full well QFW > 4000 e-
Linearity to full well < 5%
Read noise including ADC < 3.0 e-RMS
Image lag < 2 %
Dark Current < 5 e-/pixel/s ; < read noise at 1fps
QE> 90% at 589nm; optimized for LGS Sodium Laser
→ BackSide Illumination (BSI)
Point Spread Function < 0.8 pixel FWHM
Cosmetics < 0.1% bad pixels
19EIROforum CIS26 Jun 2018
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Outline
• Adaptive Optics Wavefront Sensing
• Camera Program
• CCD220
• LVSM CMOS Imager
• Visible Camera Design
• Summary
20EIROforum CIS26 Jun 2018
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Heritage: AONGC - 20 deployed in VLT SPHERE,
AO Facility (MUSE & HAWK-I), and ERIS
26 Jun 2018 21EIROforum CIS
SPHERE
HAWK-I
MUSE
GRAAL
GALACI
New camera design to:
• support new detector: LVSM
• add ELT interfaces - 10GbE for data and control and 1GbE for
Precision Time Protocol, PTP
• solve obsolescence – AONGC design > 10 years old
• build on previous experience and take on board lessons learnt
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Two visible cameras
→ single camera design
• Approach is a single camera design with customisable front-ends
to support the different type of detectors:
– CCD220-DD for optical Truth/High Order NGS/Telescope Guiding:
1,000fps, ultra low noise (< 1e-), 240x240 of 24μm pixels
– LVSM CMOS imager for Shack-Hartmann LGS/Telescope WFS:
700fps, low noise (3e-), 800x800 of 24μm pixels
• Depending on the Detector installed, the camera will have a
specific name:
– CCD220-DD → ALICE (smALl vIsible CamEra)
– LVSM → LISA (Large vISble cAmera)
• Cameras will be fully integrated with minimal external support
equipment
– only an external 24VDC supply
26 Jun 2018 EIROforum CIS 22
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Camera size ~ 98x183x266 mm3
• Externals of cameras are identical except the opening of the optical window
• Front Plate – reference for all alignment of optics and mechanics
• Housing sealed to stop ingress of dust and moisture (condensation).
• Water Cooled → conductive cooling → housing external surface < 1.5ºC
26 Jun 2018 EIROforum CIS 23
Optical
Window
Front Mounting
Reference Plate
Back
Connector
Plate
Water Cooling
Re-gassing
PCB Feedthrough
with Fibre-Optic links
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Cameras are built around a
Common Backbone
26 Jun 2018 EIROforum CIS 24
Main Board
Power Board
Front
Panel
Cooling
Structure
Back
Connector
Plate
Thermal and
EMI Shield
Cover
Thermal and
EMI Shield
Cover
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Power Board designed for high efficiency
using Switch-Mode Power Supplies
• COTS components are used wherever possible and practical
– saves substantial development effort and validation time
26 Jun 2018 EIROforum CIS 25
High Efficiency
COTS DC-DC
Converters
Modules
Front
COTS
Peltier Controller
based on Switch-
Mode Supply
Filters and
Regulators
Back
Connectors
65 mm x 38 mm x 14 mm
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Low Noise of Power Board fully validated
on previous generation of camera
• Detector temperature cooled and
stabilized to high stability of ±10mK
• No structure or appreciable increase
in the very low noise of AONGC
26 Jun 2018 EIROforum CIS 26
- 40 degC
1.5 A .. 2.5 A
Noise Map
AONGC
Proto Power Board
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Main Board based on COTS FPGA
Module
Controls the read out of the Detector and handles all external communication:
• 10GbE optical fibre links to the NGC control computer and RTC (UDP)
• 1GbE optical fibre link of the Precision Time Protocol (the ELT time reference
standard) for synchronizing, scheduling, and time stamping frames.
26 Jun 2018 EIROforum CIS 27
Front
Right FE Board
IF Connector
Back
Left FE Board
IF Connector
Xilinx Zynq UltraScale+
COTS FPGA
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Customisable FE for Detector
specific support
26 Jun 2018 EIROforum CIS 28
ALICE
CCD220-DD
LVSM
LISA
Common
Cooling Rail
Left FE Board
Mount and
Heat
Exchanger
Right FE Board
Thermal and
EMI Shield
Cover
Mount and
Heat
Exchanger
Left FE Board
Right FE Board
Thermal and
EMI Shield
Cover
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Summary
• ESO has a very active Detector and Camera technology
development program to meet current and future needs of wave-
front sensing
• The new CMOS Imager, LVSM, has passed its FDR milestone and
is in manufacture with first Electrical Grade devices available later
this year for camera testing
• Cameras are at an advanced stage of design, and, manufacturing
of the first revision is under way with integration and test of the first
cameras scheduled later this year
• High confidence of success from using all lesson’s learnt from
previous developments and prototypes.
• The development phase of the cameras is expected to take
another 18 months followed by out sourcing of production to have
cameras available in time for ELT Telescope and Instrument AIV
EIROforum CIS 2926 Jun 2018
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• Larger
– LVSM at 700fps – 2k x 2k
– SAPHIRA – 512x512
• Handle Pulsed Laser:
– Shutter opens for 2-3us
– Requires 7T pixel where charge is stored inside the pixel
Future CMOS Imager
26 Jun 2018 EIROforum CIS 30
Na Layer
Pulsed
Laser Shutter open
Shutter close
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7T pixel
26 Jun 2018 EIROforum CIS 31
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END
26 Jun 2018 EIROforum CIS 32
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27/6/2008 Detectors for AO WFS 33
Na Layer
Pulsed
Laser
Pulsed laser: track spot on CCD
and move charge back and forth to
collect photons from several pulses
before reading out.
Spot contained in much
smaller number of
pixels and only these
need to be read out