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Astro WP1 (+) Status
CTA and SKA
Garret Cotter – University of Oxford
INFIERI workshop Lisbon - 13 April 2016
* Supported by the EU FP7-PEOPLE-2012-ITN project nr. 317446, INFIERI, “Intelligent Fast Interconnected and Efficient Devices for Frontier Exploitation in Research and Industry“. ESR9
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CTAGarret Cotter, Oxford for WP1 Astro (+WP4)
ESR’s Andrea De Franco, Laurel KayeJason Watson (STFC)
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Cherenkov Telescope Array SciNeGHE 2014
Schwarzschild- Couder MST Extension
• 9.6- m primary, 8 deg FOV
• Pixel scale allows SiPM
camera
• Potentially could extend
MST array from 25 to 49
telescopes
Two-Mirror Atmospheric Cherenkov Telescope:
The Schwarzschild-Couder Telescope (SCT)
• Innovative U.S. design key to boosting
CTA performance
• Corrects aberrations providing higher
resolution, wider field
• Small plate scale enables SiPM camera
• Deep analog memory waveform
samplers to minimize dead-time and
allow flexible triggering
• High level of integration into ASICs
allows dramatic cost savings (
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Cherenkov Telescope Array SciNeGHE 2014
Schwarzschild- Couder MST Extension
• 9.6- m primary, 8 deg FOV
• Pixel scale allows SiPM
camera
• Potentially could extend
MST array from 25 to 49
telescopes
Two-Mirror Atmospheric Cherenkov Telescope:
The Schwarzschild-Couder Telescope (SCT)
• Innovative U.S. design key to boosting
CTA performance
• Corrects aberrations providing higher
resolution, wider field
• Small plate scale enables SiPM camera
• Deep analog memory waveform
samplers to minimize dead-time and
allow flexible triggering
• High level of integration into ASICs
allows dramatic cost savings (
-
The CTA Observatory
Cherenkov Telescope Array SciNeGHE 2014
Schwarzschild- Couder MST Extension
• 9.6- m primary, 8 deg FOV
• Pixel scale allows SiPM
camera
• Potentially could extend
MST array from 25 to 49
telescopes
Two-Mirror Atmospheric Cherenkov Telescope:
The Schwarzschild-Couder Telescope (SCT)
• Innovative U.S. design key to boosting
CTA performance
• Corrects aberrations providing higher
resolution, wider field
• Small plate scale enables SiPM camera
• Deep analog memory waveform
samplers to minimize dead-time and
allow flexible triggering
• High level of integration into ASICs
allows dramatic cost savings (
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CTA site selection
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6 mm pixel
2048 pixels
INFIERI participation in CTA
CHEC camera
MAPMT (prototype) SiPM (under consideration for production)
GCT (Gamma Cherenkov Telescope)
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High Voltage connection to the
MAPM (cable secured and pins insulated
during normal operation)
Individual amplifier
circuit
TARGET ASIC
providing 16 channels
of digitisation and
triggering
High Voltage
supply (12 V in,
0 – 1200 V out,
12 bit resolution)
Mechanical
standoff with
threaded hole for
securing the
TARGET module
to the backplane
Samtec 40 pin connector to the backplane carrying raw
data, trigger and sync signals and power
Xilinx Spartan 6
FPGA (on reverse of PCB)
Samtec individually
shielded coaxial ribbon
cables for analogue
signals and preamplifier
power
Front-end buffer
module consisting of 4
x 16 channel
preamplifier boards
Front-most front-end
buffer PCB forming
the interface to the
focal plane plate
CHEC-M Camera Module
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9
DACQ
boards
Backplane
WP1 – camera lab testing completed last meeting
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Dec 2016 – camera and telescope integrated and commissioned, Observatoire de Paris, Meudon
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Andrea – Update on front end
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Photosenso
r modules
TARGET
Module
Preamplifier
Module
MAPM
BackplaneSafety Board
DACQ
Boards4 x 1 Gbps
I/O
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Jason – update on camera integration & commissioning
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Laurel – update on advanced processing algorithms
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SKA
Steve Torchinsky, Nancay, WP1 Astro
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SKA Frontend Developments for Band 450 – 1450MHz
EMBRACE– Electronic MultiBeam Radio Astronomy ConcEpt– Results accepted for publication in “Astronomy &
Astrophysics”– http://dx.doi.org/10.1051/0004-6361/201526706
Steve Torchinsky, WP1 Astro
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SKA Frontend Developments for Band 450 – 1450MHz
Future development towards a large prototype
– To be built on the SKA site in South Africa
(seeking funding)
– Various frontends proposed
• Vivaldi array (EMBRACE)
• Octogonal Ring Array
– collaboration: Manchester/Nancay
– LNA, beamformer chips, provided
by Nancay
– INFIERI ESR to work on ORA
testing at Nancay beginning in June
2016
Steve Torchinsky, WP1 Astro
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Astro Summary
• WP1 and WP4 deliverables from Annexe 1 are all now achieved
• WP1 further investigations into SiPM’s for detectors in production cameras – Andrea, Jason
• Expansion of original astro activities into SKA- ESR at Nancay
• Expansion of CTA activities – advanced algorithms - Laurel on neural nets for CTA