Potential Italian contributions to WFI

PotentialItaliancontributions toWFI L. Piro, IAPS-Rome on behalf of the AthenaItalian team

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

Proposeditemsmaximizingsynergy WFI-XIFU • On board instrument s/w for the ICU • Instrument simulations • Filters • (Part of) Digital electronics • Scientificsupport(instrumenttrade-off, calibrations)

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

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)

INAF team heritage on ICU • ISO Long WavelegthSpectrometer DPU and on boards/w (IAPS, Laben) • Herschel Instruments DPUsand 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 boards/w (IASF-Bo, Oss.To, IAPS) • A single provider (INAF) for the twoscientificinstrumentsonboard one single interface with the S/C CDMU provider • Expertize with the mainstandards ICU items: • for SW design and development(UML, MISRA) • mainspacequalified processors ( DSP21020 (Herschel), LEON3FT (Euclid and SPICA), PowerPC 750FX (Euclid)) • SpaceWirenetworks (Euclid and SPICA) • ESA ECSS standards and procedures • CCSDS standard losslesscompressionalgorithmsimplementation and optimisation (Euclid)

Benefit of the synergicalapproach 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 commonalitiesexploitation • design • procurement • testing

Proposeditemsmaximizingsynergy WFI-XIFU • On board instrument s/w for the ICU • Instrument simulations • Filters: development, procurement and calibration • (Part of) Digital electronics • Scientificsupport(instrumenttrade-off, calibrations)

Filters in Athena- XIFU • INAF (Oss.Pa) & Univ. Pa: Development and Calibration of the X-IFU Aperture Cylinder and FPA Optical/IR blockingFilters Presentbaseline 5 filters for a total of Aluminum2100 Å + Polyimide 2800 Å Supportmeshon the twolargerdiameterfilters.

HERITAGE • ChandraHRC-I (USA) • Development and calibration of the HRC UV/Ionshields (93 mm x 93 mm) HRC-I Aluminum 750 Å + Polyimide 5700 Å • Newton-XMM EPIC (Europe) • Development and calibration of the Thinand Medium filters (76 mm diam.) Thin Aluminum 400 Å + Polyimide 1800 Å MediumAluminum 800 Å + Polyimide 1800 Å • HINODE XRT (USA/Japan) • Calibration of the 9 focalplanefilters(50 mm diam.) Thin Al/Mesh Aluminum 1600 Å + Mesh 82 % Thin Al/Poly Aluminum 1600 Å + Polyimide 2500 Å C/PolyCarbon 7000 Å + Polyimide 2500 Å Ti/Poly Titanium 3000 Å + Polyimide 2500 Å Thin Be Beryllium 9 μm Med Be Beryllium 30 μm Thick Be Beryllium 300 μm Med Al Aluminum 12.5 μm Thick Al Aluminum 25 μm

Examples of filtercharacterization X-RayAstronomyCalibration and Testingfacility (INAF) Barbera, M.,. et al.,Proc SPIE, 5488, 2004. HINODE CalibrationProgram

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 environmentdriving instrument design

Stationary flux Flares 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

Improvement in Background reduction • Extensive simulations/design and TES AC detector and suppressionof secondary electrons F(5”)=10-13 c.g.s x20 x6 Fe Ka σ(T) =3.3% σ(Z) =15% 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 16 σ(T) =2.4% σ(Z) =12%

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,…)

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.)

Proposeditemsmaximizingsynergy WFI-XIFU • On board instrument s/w for the ICU • Instrument simulations • Filters • (Part of) Digital electronics for pre-processing • Scientificsupport(instrumenttrade-off, calibrations)

Digital Electronics for XIFU TESCryoAC • INAF consortium in charge of the TESCryoAC detector • Digital box (IASF-Mi): • Digitalizationof analogsignals from detector • Preprocessingof data

Heritage • Solar 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 AntiCoincidencedetector, test and measurementelectronics of AGILE • Rad Hard Tests of ASICs @ Legnaro: SEU monitoring • Latch-up monitoring

Additionalactivities • GSE/AIV/AIT (e.g. IASF-Bo,IAPS): • Currentlynotbaselined for XIFU (thus of lowerpriority) but with strong heritagefrom EPIC/XMM – PICSIT/INTEGRAL – Simbol-X and NHXM – AGILE, Herschel, …

Proposeditemsmaximizingsynergy WFI-XIFU • On board instrument s/w for the ICU • Optical/UV blocking Filters • Instrument simulations • Scientificsupport (instrumenttrade-off, …) • (Part of) Digital electronics for pre-processor

X-RayTransmissionMeasurementsandModeling HINODE CalibrationProgram Barbera, M.,. et al.,Proc SPIE, 5488, 2004.

Advanced Telescope for High Energy Astrophysics Analysis of Planck/SREM data 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. * 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. 26 Luigi Piro ATHENA+ X-IFU Italian Consortium

Potential Italian contributions to WFI