Garching – January 28, 2014

WFI Consortium MeetingPRESENTATION OF OUR ACTIVITIES FOR X-RAY ASTROPHYSICS AND INTERESTS FOR ATHENA / WFI

Garching – January 28, 2014

Aline MeurisOn behalf of the

Astrophysics division

[email protected]

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Institute of Research into the Fundamental Laws of the UniverseAstrophysics DivisionCEA 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 UniverseCEA Saclay ~800 peopleAstrophysics, 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 accelerationwith XMM-Newton, INTEGRAL, RXTE, Chandra, Swift

in synergy with H.E.S.S., Fermi, radio telescopes• Galaxy clusters

as probe of structure formationwith 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



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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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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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


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 ASICsCaliste-HD hybrid with 8 ASICs, 256 pixelsMACSI 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


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


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


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 CNEScan be the basis for a specific developmentWilkinson architecture with delay-locked loop add 4-5 bit precision with the same conversion timeChip test: 32 channel converted in parallel in 2.7 µsto get 13-bit resolution1.5 mW per channel



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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 companyMounting of ASIC and pnCCD by MPE



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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


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.


THANK YOU FOR YOUR ATTENTION

BACK-UP SLIDES

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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


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.


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 serialMODE // 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


THE OWB-1 ADC: REDUCING THE POWER CONSUMPTION

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Design not optimized for low power but other configuration possible :• Zero suppressionDetection of a zero by the ADCAdjusting 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

Garching – January 28, 2014

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