WFI Consortium Meeting P RESENTATION OF OUR ACTIVITIES FOR X- RAY ASTROPHYSICS AND INTERESTS FOR A...
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Transcript of WFI Consortium Meeting P RESENTATION OF OUR ACTIVITIES FOR X- RAY ASTROPHYSICS AND INTERESTS FOR A...
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
| PAGE 1
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+
| PAGE 2
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)
| PAGE 5
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)
| PAGE 6
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)
| PAGE 7
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)
| PAGE 8
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
| PAGE 9
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
| PAGE 10
POSSIBLE CONTRIBUTIONS TO ATHENA+ WFI
| PAGE 11CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014
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
| PAGE 12
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
| PAGE 13
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
| PAGE 15
CEA/Irfu | WFI Consortium meeting Garching | January 28, 2014
THE OWB-1 ADC : GLOBAL ARCHITECTURE
| PAGE 16
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
| PAGE 17
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
| PAGE 18
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
| PAGE 20
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
| PAGE 21
@ 13.9 keV