WFI Consortium Meeting

PRESENTATION OF OUR

ACTIVITIES FOR X-RAY

ASTROPHYSICS AND INTERESTS

FOR ATHENA / WFI

Garching – January 28, 2014

Aline Meuris

On behalf of the Astrophysics division

aline.meuris@cea.fr

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Institute of Research into the Fundamental Laws of the Universe

Astrophysics Division

CEA Saclay, France

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

OUTLINE

Introduction to CEA-Irfu

Science: lead programs and instrument developments and

interests for ATHENA+

Hardware: past, present, future connected to ATHENA+

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GROUPS IN CEA-IRFU CONNECTED TO ATHENA+

| PAGE 3CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

Institute of Research into the Fundamental Laws of the Universe

CEA Saclay ~800 people

Astrophysics, High Energy Physics, Nuclear Physics and associated instrumentation

Astrophysics Space instrumentation Technical services

ObservationInterpretation

SimulationInstrument lead

Front-end electronics,Mechanical engineering…

Architecture and design Detector R&D

QualityAIV

Astrophysics division (~200 people)

Scientific responsibilities in instrument developments and observation programs

Developments close to the detection systems

SCIENTIFIC INTERESTS IN X-RAY ASTRONOMY

Main fields of interest:• Compact objects: X-ray binaries, GRB, isolated pulsars, Sgr A*

• Supernovae remnants

as probe of extreme physics, e.g. particule acceleration

with XMM-Newton, INTEGRAL, RXTE, Chandra, Swift

in synergy with H.E.S.S., Fermi, radio telescopes

• Galaxy clusters

as probe of structure formation

with XMM-Newton and Planck

Intensive use of XMM-Newton since PV phase PI-ship of 7 large programs and 1 very large program

Expertise in spatially resolved and time resolved spectroscopy

| PAGE 4CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

IMPLICATION IN ATHENA

Strong involvement in next X-ray large mission since 2001

XEUSMember of the steering group and ESA Science Advisory group (M. Arnaud)

IXOMember of the ESA Science Definition Team (M. Arnaud)

Members of instrument working group (O. Limousin for WFI/HXI, C. Pigot for calorimeter)

Athena(+)Member of the Athena Study Team (A. Decourchelle)

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CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

STRONG INTEREST IN ATHENA THEMES

The Hot Universe: How does ordinary matter assemble into the large scale structures that we see today?• "The Astrophysics of galaxy groups and clusters with Athena+"

Support paper by S.Ettori, G. Pratt et al.

The Energetic Universe: how do black holes grow and influence the Universe?• The physics of accretion

• Luminous extragalactic transients

Athena+ observatory capabilities• "The astrophysics of supernova remnants and the interstellar

medium"   Support paper by A. Decourchelle, E. Costantini et al.

• "End points of stellar evolution" Support paper by C. Motch, J. Wilms et al. (J. Rodriguez)

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CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

REALIZATIONS FOR X-RAY ASTROPHYSICS

XMM-Newton (1999): 0.2-12 keV• Development of the EPIC MOS CCD Controller and Recognition Unit• Involvement in MOS CCD cameras calibration at Orsay• Contribution to the Science Survey Center

INTEGRAL / ISGRI (2001): 15-200 keV• Development of the ISGRI instrument (1024 cm2 CdTe)

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Polycell = ceramic with CdTe crystals and ASIC

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

REALIZATIONS FOR X-RAY ASTROPHYSICS

SIMBOL-X: French-Italian hard X-ray telescope (2009)

Detector R&D (2004-2012): IDeF-X 32-channel front-end ASICs

Caliste-HD hybrid with 8 ASICs, 256 pixels

MACSI with 8 Caliste-HD, 2048 pixels(2-100 keV)

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Simbol-X Focal plane

High Energy Detector (CEA/Irfu) 64 cm2 CdTe

Low Energy Detector (MPE) Si DEPFET

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

SPACE PROJECTS IN IMPLEMENTATION PHASE

Astro-H (JAXA)• Radiation damage study on CdTe detectors and ASICs

SVOM: GRB mission with China (PI institute)• MXT (0.2 – 10 keV): PI, Development of the camera • ECLAIRs (4 - 250 keV): Thermal design of the telescope,

Design and qualification of front-end ASIC IDeF-X ECLAIRs• Ground segment

Solar Orbiter (ESA M1)• Development of the X-ray spectrometers for STIX

Euclid (ESA M2)• Consortium lead (Y. Mellier IAP/CEA) and lead supports• Control electronics and AIV of the VIS focal plane

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Caliste-SO prototypes

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

SKILLS DEVELOPED ALONG 20-YEAR EXPERIENCE

• Radiation hard low power low noise front-end ASIC• (ESA) Space qualification of ASIC and hybrid components• System (thermal, mechanical, electrical) architecture and design• Instrument modeling, integration, calibration

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POSSIBLE CONTRIBUTIONS TO ATHENA+ WFI

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Microelectronics• Collaboration on very front-end electronics design• Parallel analog-to-digital conversion ASIC• Fabrication management and space qualification

Tests and qualification• Space qualification of full-custom components• Detector and electronics radiation damage studies

OWB-1 chip: R&D funded in 2012-2014 by CNES

can be the basis for a specific development

Wilkinson architecture with delay-locked loop add 4-5 bit precision with the same conversion time

Chip test: 32 channel converted in parallel in 2.7 µsto get 13-bit resolution

1.5 mW per channel

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

POSSIBLE CONTRIBUTIONS TO ATHENA+ WFI

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Hybridization• Chip and EEE assembly and ceramic hybridization, interconnects• Hybridization qualification

System and architecture• Mechanical design, thermal design and modeling of the focal plane• Background simulation

Example:

MXT detector board prototype

Collaboration with MPE

Layout by CEA, fabrication by a French space-certified company

Mounting of ASIC and pnCCD by MPE

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

POSSIBLE CONTRIBUTIONS TO ATHENA+ WFI

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Warm front-end electronics

• Real-time processing in interface with the cold front-end electronics to

guarantee system performance

Similar challenges experienced with Herschel/PACS.

Example:

MXT front-end electronics prototype

« Pixel sequencer » and « frame sequencer » based on space grade FPGA

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

CONCLUSION

CEA-Irfu highly interested in taking part in WFI consortium• Astrophysics groups defending Athena+ science case• Experience in detection system design and realization at different

levels to serve the instrument performance

THANK YOU FOR YOUR ATTENTION.

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

THANK YOU FOR YOUR ATTENTION

BACK-UP SLIDES

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CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

THE OWB-1 ADC : GLOBAL ARCHITECTURE

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Architecture Wilnkinson with DLL (delay-locked loop)

The conversion time of this N+M bits ADC is :

𝑇 𝐶=2𝑁

𝐹𝐶𝐿𝐾

=2𝑁+𝑀

𝐹𝐷𝐿𝐿

Adding conversion bits for a same time compared to a conventional 𝑴Wilkinson architecture

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

THE OWB-1 ADC : MAIN FEATURES

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FEATURE (OWB-1)

Technology CMOS AMS 0.35µm (C35B4C3)

Number of Channel 32

Resolution 12-13 bits (7-8 for the counter and 5 for the DLL)

Input voltage 2 V (from 0.8 to 2.8 typical)

Conversion time 1,5 - 2,7 µs (12-13 bits)

Output 11 bits parallel or 2 bits LVDS (Low Voltage Differential Signaling)

Consumption Typical condition : 1.5 mW per channel (see details next slides)

Clock input 100 MHz for counter

Input PADs pitch 150 µm

Channel with 50 µm

Radiation hardness SEL free : LET>110 MeV/(mg/cm²)

SEU Flag for slow control.

ASIC OWB-1 : analog to digital conversion optimized for the readout of self-triggered ASIC for CdTe detectors. Design for low count rate applications.

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

THE OWB-1 ADC : MODES OF OPERATION

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Data format : Channel (5 bits) + Code (14 bits)

Data transfer during conversion:

Two modes of DATA (code) transfer : // and serial

MODE // Serial Mode

Number of digital output PAD/ASIC 11 (CMOS) 2 (LVDS)

Reading clock [MHz] 25 300

Power Consumption per channel [mW]

Cload = 5 pF 1.4 2.1

Cload = 50 pF 1.5 2.1

WFI CENTRAL PART: PROPOSAL WITH CEA CHIPS

1) Remplacement of the MUX stage of

Veritas by 64 ‘small’ output buffers to get

parallel outputs

2) Direct bonding of Veritas outputs to

OBW-1 inputs add 1,5 W to 2 W on

central part

3) Suppression of differential output

amplifiers

Veritas*

256 256 Switcher

OBW-1-ATHENA: 128 channels, concatenation of 4 OBW-1 (50 µm pitch) | PAGE 19CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014

THE OWB-1 ADC: REDUCING THE POWER CONSUMPTION

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Design not optimized for low power but other configuration possible :• Zero suppression

Detection of a zero by the ADC

Adjusting the detection threshold above the zero signal

Reducing the power consumption• Optimisation of the output digital stage for this frequency

[V]

[t]

VCOMP

VIN OK

VRAMP

VIN ZEROVRAMP_MIN

NO EVENT NO DATA TRANSFER EVENT DATA TRANSFER

1ER JUIN 2006

ISGRI monopixel 4 x 4 mm2 (2 mm thick CdTe, 120V, 0°C)

5.60 keV FWHM

2001R&D CALISTE-HD – 256 pixels, 580 µm pitch (1 mm thick CdTe, 400V, -4°C)

0.67 keV FWHM

0.57 keV FWHM à 13.9 keV

2012

FROM INTEGRAL/ISGRI TO CALISTE

Energy (keV)0 20 40 60 80

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@ 13.9 keV