Potential Italian contributions to WFI

MPE, Garching – Jan. 28, 2014Italian contribution to WFI: L. Piro

Athena, the Advanced Telescope for High Energy Astrophysics

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Potential Italian contributions toWFI

L. Piro, IAPS-Romeon behalf of the Athena Italian team



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The rationale• The primary Italian contribution to mission elements is

XIFU• Other smaller contributions include participation to

mirror and Ground Segment activities. • This approach has been consistently presented to ASI and

properly ackwnoledged by the agency• Credible approach for WFI contributions: limited and

harmonized with present commitments on XIFU. • For WFI we propose activities that are carried out by the

Italian consortium on XIFU and that can be – with a reasonable delta effort – developed for WFI



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Proposed items maximizing synergy WFI-XIFU

• On board instrument s/w for the ICU • Instrument simulations• Filters • (Part of) Digital electronics• Scientific support (instrument trade-off,

calibrations)



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• On board instrument s/w for the ICU • Instrument simulations• Filters • (Part of) Digital electronics• Scientific support (instrument trade-off,

calibrations)



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ICU in XIFU• INAF (IASF-Bo, Oss.To, IAPS) responsible for h/w and s/w)



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ICU Functions

• Set-up and control instrument subsystems• Interface to S/C for H/K and TC• Science data packaging and transfer to S/C ( I/F TBC)• Instrument health check• Failure mode management • Time signal distribution (TBC)• Filter Wheel control (I/F, motor driver and X-ray source

TBC/TBD)

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• ISO Long Wavelegth Spectrometer DPU and on board s/w (IAPS, Laben) • Herschel Instruments DPUs and instrument control software (IAPS,CGS)

- A single provider for all the three scientific instruments onboard one single interface with the S/C CDMU provider

•Euclid VIS CDPU and instrument control and data s/w (IAPS) and NISP ICU on board s/w (IASF-Bo, Oss.To, IAPS)- A single provider (INAF) for the two scientific instruments onboard one single interface

with the S/C CDMU provider

• Expertize with the main standards ICU items:– for SW design and development (UML, MISRA)– main space qualified processors ( DSP21020 (Herschel), LEON3FT (Euclid and SPICA), PowerPC

750FX (Euclid))

– SpaceWire networks (Euclid and SPICA)– ESA ECSS standards and procedures– CCSDS standard lossless compression algorithms implementation and optimisation (Euclid)

INAF team heritage on ICU

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Possibility to implement onboard Athena+ the same “effective and successful” configuration adopted for Herschel and Euclid

one single On Board Software provider (INAF) for both scientific payload instruments

one single interface between ESA, Prime and Instruments Consortia for S/C data interface matters (protocol definition, SW interface implementation and testing)

A centralised expertise for the on board science data processing

Best commonalities exploitation- design- procurement- testing

Benefit of the synergical approach

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• On board instrument s/w for the ICU • Instrument simulations• Filters: development, procurement and calibration • (Part of) Digital electronics• Scientific support (instrument trade-off,

calibrations)



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INAF (Oss.Pa) & Univ. Pa: Development and Calibration of the X-IFU Aperture Cylinder and FPA Optical/IR blocking Filters

Present baseline 5 filters for a total of Aluminum 2100 Å + Polyimide 2800 ÅSupport mesh on the two larger diameter filters.

Filters in Athena- XIFU



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HERITAGE

• HINODE XRT (USA/Japan) Calibration of the 9 focal plane filters (50 mm

diam.)

• Chandra HRC-I (USA) Development and calibration of the HRC UV/Ion shields (93 mm x 93 mm)

• Newton-XMM EPIC (Europe) Development and calibration of the Thin and Medium filters (76 mm

diam.)

Thin Al/Mesh Aluminum 1600 Å + Mesh 82 %Thin Al/Poly Aluminum 1600 Å + Polyimide 2500 ÅC/Poly Carbon 7000 Å + Polyimide 2500 ÅTi/Poly Titanium 3000 Å + Polyimide 2500 ÅThin Be Beryllium 9 μm Med Be Beryllium 30 μm Thick Be Beryllium 300 μmMed Al Aluminum 12.5 μm Thick Al Aluminum 25 μm

HRC-I Aluminum 750 Å + Polyimide 5700 Å

Thin Aluminum 400 Å + Polyimide 1800 ÅMedium Aluminum 800 Å + Polyimide 1800 Å



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Examples of filter characterization

HINODE Calibration Program

Barbera, M.,. et al., Proc SPIE, 5488, 2004.

X-Ray Astronomy Calibration and Testing facility (INAF)



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calibrations)



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Simulations of XIFU• INAF consortium (led by IAPS with IASF-Pa and

Oss.Pa, with plans to include contributions from IASF-Bo and Oss. Roma) responsible for XIFU simulations. Need to fold various effects:

• L2 environment: CR and solar protons (analysis of particle monitor from Herschel and Planck)

• Various galactic and extragalactic X-ray components

• effect of soft protons through mirrors (with optics ray tracing) driving assessment of particle diverter

• GEANT simulation of detector and its environment driving instrument design



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Advanced Telescope for High Energy Astrophysics

Particles background in L2• Cosmic Rays

• Solar protons

• Both components depend on the solar cycle.

• Analysis of Planck Particle Monitor Data undergoing

Stationaryflux

Flares



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Improvement in Background reduction

x20

x6

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σ(T) =3.3%σ(Z) =15%

Fe Ka

Cluster at the formation epoch (z=2)F=10-15 erg/cm2/s, A=0.2 arcmin2, kT=2.0 keV, Abundance 0.3, area=1m2,f/l=12m

• Extensive simulations/design and TES AC detector and suppression of secondary electrons

F(5”)=10-13 c.g.s



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Benefit

• Beneficial in terms of optimization of resources if (some of) instrument simulations activities are carried out for the WFI as well.

• E.g.: Avoid duplication of same items: various components of L2 environment, GEANT model of the spacecraft

• Similar design solutions for further reduction of the residual particle background (shields, soft particle diverter,…)



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calibrations)



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Science support• For XIFU: IAPS, IASF-Bo, Oss.Pa, Oss. Roma,

UniRoma, with contributions by Oss. Trieste, Oss. Bo, Oss. Mi, IASF-Mi). For the WFI a team drawn from the above team.

• Example: Hydrodynamical simulations of galaxies/groups/clusters/WHIM (X-IFU & WFI) FLASH/grid-based SPH cosmological simulations

(ref. INAF/OaBO & Univ.)



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• On board instrument s/w for the ICU • Instrument simulations• Filters • (Part of) Digital electronics for pre-processing• Scientific support (instrument trade-off,

calibrations)



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Digital Electronics for XIFU TESCryoAC • INAF consortium in charge of the TESCryoAC detector• Digital box (IASF-Mi):• Digitalization of analog signals from detector• Preprocessing of data



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HeritageSolar Orbiter/METIS UV detector (Intensified APS) • Testing• Development of the real

time digital processor for enabling photon counting detection (implemented in FPGA Actel RTAX 2000)

Design and development of the AntiCoincidence detector, test and measurement electronics of AGILE

Rad Hard Tests of ASICs @ Legnaro: SEU monitoring Latch-up monitoring



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Additional activities

• GSE/AIV/AIT (e.g. IASF-Bo,IAPS): • Currently not baselined for XIFU (thus of lower

priority) but with strong heritage from EPIC/XMM – PICSIT/INTEGRAL – Simbol-X and NHXM – AGILE, Herschel, …



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• On board instrument s/w for the ICU • Optical/UV blocking Filters • Instrument simulations• Scientific support (instrument trade-off, …)• (Part of) Digital electronics for pre-processor



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X-Ray Transmission Measurements and Modeling

HINODE Calibration Program

Barbera, M.,. et al., Proc SPIE, 5488, 2004.



26ATHENA+ X-IFU Italian ConsortiumLuigi Piro

Advanced Telescope for High Energy Astrophysics

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Analysis of Planck/SREM data

* Data courtesy of Dr. Paul Buehler, Andrea Zacchei and Luis Mendes** (left) each bin is 1 day averaged. The decrease is consistent with the solar cycle that is going toward the max.***(right) each bin is 50 s.

We analyzed the data from the Solar Radiation Environment Monitor onboard of Planck (SREM) in the period 2009-2013, since it is in the same orbit ATHENA+ will be placed.

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Potential Italian contributions to WFI

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