Company profile & Space Science Detector Capabilities

www.photek.co.uk page 1

Company profile & Space Science Detector Capabilities

- Ian Cox


Company Profile

• Specialist manufacturers of vacuum based detectors

and camera systems for photon detection. Photek

manufacture Image Intensifiers, PMT’s, Streak

Tubes, open faced detectors and a range of

associated electronics and camera systems

• Located in St Leonards-on-Sea – South East England

• Established September 1991


Company Profile

• 36 Employees

– 10 sales/administrative

– 7 R&D

– 19 production/test

• 5 employees educated to PHD level

• Further 8 employees educated to degree level


Detector Products

• MCP image intensifier

• Ultra fast MCP photomultipliers

• Streak tubes

• Magnetic focus image intensifiers

• De-magnifying gen 1 image intensifiers

• Vacuum compatible detectors


Camera Products

• Photon counting

• Nanosecond ICCD

• Intensified CCD

• Fluorescence

• X-ray

• Particle imaging


Electronic Products

• HT power supplies

• Nanosecond gating control

• Laser pulse generator

• Preamplifier

• Image intensifier cooling


Applications

• Early warning Missile systems

• Wafer silicon inspection

• Astronomy including orbital space science

experiments

• Ultra-high speed cameras

• Nuclear & high energy physics research

• Life-science research

• Industrial processing

• Security


Facilities

• 1,500m2 factory space

• Class 100 assembly area

• Class 10,000 clean room

• Electro-mechanical vibration table

• Ultra-high vacuum processing equipment

• High speed (50 ps) laser pulsing equipment

• Wet and dry hydrogen stoving capability

• Inventor 3-D CAD software


Facilities – Continued

• Protel Electronic Design Software

• Agilent 18 GHz sampling scope

• LeCroy 5 GHz digital scope

• Spectrometer

• Photometer

• Optical table and dark room facilities

• Environmental test chamber

• Phosphor screen production and inspection facilities

• Optical coating plant


Quality

• Photek operates a company wide quality system based on ISO9000 and TQM principles

• Currently working towards ISO9000 accreditation with successful implementation expected in 2008

• We operate a strict stock control and inspection policy with all items batch controlled and tracked

• All detectors and systems are fully characterised in out photometry laboratory

• Each device has a serial number that is used throughout the entire manufacturing process


Test and Support

• Excellent support and test facilities

• Rigorous testing of all products is completed before

release

• Support question always answered by a technical

member of staff. Typically educated to PHD level

• 12 month warranty on all products

• Technical support for lifetime of product


Space Science Projects

• ACE Advanced Composition Explorer

• XMM UV Optical Monitor

• MSX UVISI Detector

• GUVI Global Ultraviolet Imager

• SSUSISpecial Sensor Ultra-violet

Spectrographic Imager

• UVIT Ultra-Violet Imaging Telescope


Advance Composition Explorer

• CRIS Detector (Cosmic Ray Isotope Spectrometer)

– 40 mm Image Intensifier with 2 MCP

– UV Fibre Optic Input Window

– Blue Enhance Cathode to Match Scintillating Fibre

Optics

– 100,000 Gain

• Uses scintillating fibre optic

structure. The detector is to measure

direction and energy of cosmic rays


UV Optical Monitor

• Photon Imaging 170 nm to 550 nm region

• Aligned with X-Ray Telescope

• Provides Simultaneous Visible, UV and X-ray

Images


The XMM Detector

• 25 mm Photon Counting

• High Sensitivity in the 170 nm to 550 nm Region

• Built in Fibre Optic Taper

• Concave Input Window


Mid Course Space Experiment

• Johns Hopkins University

• Launched 24 April 96

• Part of the spectrograph on the UVISI Instrument

• Diffuse and Discrete Aurora

• Low Earth Atmosphere Phenomena


MSX-UVISI Detector

• 40 mm Photon Counting Image Intensifier

• MgF2 Input Window

• CsI Photocathode

• 100 nm – 250 nm Response


Global Ultra Violet Imager

• Johns Hopkins University Applied Physics Laboratory

• Launched on the TIMED Spacecraft during 2001

• TIMED is used to study the energetics and dynamics

of the Mesosphere and lower Thermosphere between

an altitude of approximately 60 to 180 kilometers.

• GUVI is a far-ultraviolet (115 to 180 nm), scanning

imaging spectrograph that provides horizon-to-

horizon images in five selectable wavelength intervals


GUVI Detector

• 25 mm UV Photon Counting

• MgF2 Input Window

• CsI Photocathode

• Wedge and Strip Anode

• 106 cps

• 3x106 Gain


Ultra-Violet Imaging Telescope

• Indian Space Research Organisation (ISRO)

• Due to launch on the ASTROSAT spacecraft during

2008 – now delayed until 2012.

• ASTROSAT aims are to investigate the origin and

mechanism of radiation emissions in active galactic

nuclei.

• UVIT aims to provide flux calibrated images of the

sky in the far-UV, near-UV and visible spectral

regions


Summary

• World leading space science vacuum detector

manufacturer

• Photek have the experience and knowledge to

produce detectors to the most stringent space

science requirements

• Quality systems in place to ensure repeatability of

detector manufacture

• Test and support facilities give first class support for

the lifetime of our detectors


• Three 40 mm photon counting detectors

• Far UV (120-180 nm)

• Near UV (180-300 nm)

• Visible (180-550 nm)

• Integrated fibre optic taper with bonded

FillFactory Star 250 CMOS sensor

UVIT Detectors


UVIT Detectors

Photek have supplied 7 detectors for the UVIT project

• NUV EM

• NUV FM and FS

• FUV FM and FS

• VIS FM and FS


UVIT Detector


Outline SpecificationFUV Detector 120-180nm• MgF2 Input Window•CsI Solar Blind Photocathode•2x 60:1 40mm MCP’s•P46 Phosphor•Fibre taper output•Star250 Sensor

NUV Detector 180-300nm•Fused Silica Input Window•CsTe Solar Blind Photocathode

VIS Detector 180-550nm•Fused Silica Input Window•Low Noise S20 Photocathode


Spectral Response

Wavelength Specification QE Measured QE

120nm >5.8% 6.8%

130nm 7.3%

140nm >6.2% 6.2%

150nm 5.3%

160nm >4.2% 4.3%

170nm 3.5%

180nm >1.2% 1.2%

190nm 0.5%

200nm 0.2%


Cathode RecessPosition Recess (mm)

A 2.067mm

B 2.056mm

C 2.047mm

Centre 2.050mm

The cathode recess is measured from the front of the DM mounting ring and the front of the input window.

A

B

C View from front of detector


Window ThicknessPosition Optical Thickness (mm)

A 3.6mm

B 3.6mm

C 3.6mm

Centre 3.6mm

The window thickness is an optical measurement from the photocathode surface to the outside surface of the window.

A

B



Cathode to MCP GapPosition Gap (mm)

A 0.11mm

B 0.11mm

C 0.10mm

Centre 0.11mm

The cathode gap is measured from the photocathode surface of the input window to the front of the MCP

A

B



Electrical – Operating VoltagesOptimal Maximum O/V Test

Cathode -270V -270V -300V

MCP 2350V 2600V 2860V

Anode 5000V 5500V 6000V

• Cathode and MCP voltage WRT ground (MCP Input).• Anode voltage WRT MCP output. • Optimal voltages are voltages as tested at Photek • The maximum specified voltages should not be exceeded• Each electrode has been over voltage (O/V) tested to the stated value


ResolutionWavelength Cathode Voltage Resolution

185nm -300 20 microns FWHM


FUV FM Gain Calibration

-100V -50V +50V +100VNominal

Cathode -270VMCP 2580VAnode 3500V

Cathode -270V MCP 2480VAnode 4000V




Nominal


Event SizeCathode MCP Anode -100V -50V Nominal +50V +100V

-270 2580 3500 1.9 1.9 2 2.1* 2.2*

-270 2480 4000 1.8 1.8 1.9 1.9 2

-270 2400 4500 1.7 1.7 1.8 1.8 1.9

-270 2350 5000 1.6 1.7 1.7 1.8 1.8

-270 2300 5500 1.6 1.6 1.7 1.7 1.8

Note: The approximate FWHM of the event footprints has been measured and the results shown above for a range of operating voltages.


Dark Noise

2 Hour Dark Noise Image @22CNo bright defects detectable Average rate 5cps

Count rate graph shows variation of count rate on a 1 second timescale.


Image Alignment

A B

C

View from front of detector

D

Star250 Readout


Uniformity

Horizontal / vertical cathode uniformity

Average uniformity SD/Mean=4.5%


Environmental Testing

1. Encapsulation of detector2. 24 Hour / 40C Bake to cure Arathane3. Qualification level thermal cycle4. Bond Star250 sensor5. Vacuum Test6. Acceptance level thermal cycle7. Acceptance level vibration tests8. Final acceptance tests

Note: Detector is tested after each stage of environmental testing


Vacuum Test

Photek do not have full thermal vacuum test facilities. The following compromise test was agreed:

1.Place detector in a vacuum chamber 2.Leave for 24 hours @20C3.Increase the room temperature to 30C and leave for 48 hours4.Reduce room temperature back to 20C and leave for 24 hours


Thermal Cycle

Qualification Level Thermal Cycle

Acceptance Level Thermal Cycle

Note: Short cycles 2hrs, long cycles 24 hrs

+35˚C -15˚ C+45˚C -25˚C Peaks

+30˚C -10˚C+40˚C -20˚C Peaks


5.0 10.0 100.0100.0m

1.0

10.0

100.0

Frequency, Hz

LogM

ag, g

Sine Vibration

Frequency (Hz) Acceptance level

5 – 20 8.3mm (0-Peak)

20 – 50 13.3g

50 – 70 10g

70 –100 5.3 g

Sweep rate 4 oct. / min.


Random Vibration

Frequency (Hz) Acceptance Level PSD (g2 / Hz)

20 – 100 + 3 dB / oct.

100 – 700 0.09

700 – 2000 - 6 dB / oct.

Overall RMS 9.9 g

20.0 2.0K100.0 1.0K1.0m

10.0m

100.0m

1.0

Hz

Lo

gM

ag

, g

²/H

z


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Company profile & Space Science Detector Capabilities

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