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

CTAGarret Cotter, Oxford for WP1 Astro (+WP4)

ESR’s Andrea De Franco, Laurel KayeJason Watson (STFC)

++

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 (

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 (

CTA site selection

6 mm pixel

2048 pixels

INFIERI participation in CTA

CHEC camera

MAPMT (prototype) SiPM (under consideration for production)

GCT (Gamma Cherenkov Telescope)

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

9

DACQ

boards

Backplane

WP1 – camera lab testing completed last meeting

Dec 2016 – camera and telescope integrated and commissioned, Observatoire de Paris, Meudon

Andrea – Update on front end

32

Photosenso

r modules

TARGET

Module

Preamplifier

Module

MAPM

BackplaneSafety Board

DACQ

Boards4 x 1 Gbps

I/O

Jason – update on camera integration & commissioning

Laurel – update on advanced processing algorithms

SKA

Steve Torchinsky, Nancay, WP1 Astro

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

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

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