ATHENA the Advanced Telescope for High ENergy Astrophysics

ATHENA : the Advanced Telescope for High ENergy Astrophysics Cryo. AC: TES & Integrated Detector F. Gatti (Uni. Ge) & C. Macculi (IAPS-INAF) ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Detector: Design, Simulation & Fabrication • Activities: • Completion of the Thermal/A-thermal signal study • Fab. of Old Anti. Co Square Design” with/without Al phonon collector • Performance Comparisons • Fix the last details of the physics of signal formation • Hexagonal Anti. Co • Design & Simulation: • Mechanics and I/F ( Simulation • Thermal (Th. Conductance tuning, Th. I/F, …) • TES-wiring Configuration vs Magnetic Field ( μT requ. ment at 1 mm) • Lowering the Tc (tuning operating temp. vs Pbias and signals shape) • Smaller TES Resistances →High Bias Current→ High Ic Wiring (Nb) • Fab Process (High Precision DRIE, …) ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics “Old Anti. Co Square Design” without Al phonon collector AC-S 7 CAD -65 100 x 100 sq um Ir TESs ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics “Old Anti. Co Square Design” without Al phonon collector AC-S 6 CAD -65 100 x 100 sq um Ir TESs -same configuration, Al fins as phonons’ collectors ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Nb wiring for High Bias Current Nb RF sputtering parmeters fixed Tc of produced Nb wires ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Process Monitoring: Alignment, Thickness, Uniformity and Contacts ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Process Monitoring: Alignment, Thickness, Uniformity and Contacts ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Hexagonal Configuration Mech/Term Design comply with Mech/Term Requirements ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Update on stress simulations Contact section (under) Scanning through G of total displacement and stress along a sample bridge. More critical situations can be observed on this particular shape, but it also depends on fixed constraints Contact section ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

Chip concept. 96 rectangular TESs laying on the Silicon chip, carved out from a 16. 8 x 16. 8 sq mm double side polished silicon wafer and suspended by 4 bridges, 100µm wide and 1000µm long. The lower wiring has double-width in respect to the upper wiring.

Chip concept. 96 rectangular TESs laying on the Silicon chip, carved out from a 16. 8 x 16. 8 sq mm double side polished silicon wafer and suspended by 4 bridges, 100µm wide and 1000µm long. The lower wiring has double-width in respect to the upper wiring.

ATHENA : the Advanced Telescope for High ENergy Astrophysics Anti-inductive TES-design TES (gray) view with Al collectors (cyan), lower (red) and upper (blue) wiring, and silicon dioxyde as insulating layer in between (yellow) Phonon Collector TES Stripline-like wires ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Single TES Magnetic Field vs height From top to bottom: -380 um silicon chip for X-ray buffer -1000 um gap -silicon buffer with Anti. Co TES and part of wiring -1 u. V applied voltage, corresponding to 160 μA ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Single TES Magnetic Field vs height 1μT 1 n. T 0 0. 5 mm 1. 0 mm 1. 4 mm ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics First Prototype Fabricated: process tested Larger TES covering: To increase signal collection with a lower thermal capacity Superposed wiring: To have anti-inductive connection and avoid magnetic cross talk with main detector ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

Processes flowchart, AC-S 6/7 ATHENA : the Advanced Telescope for High ENergy Astrophysics Processes flowchart 1. Ir, Ir/Au Ion milling/dry etching Wire deposition Lift off ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Processes flowchart 2. ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹#›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Last AC-S 5 characterization: provides the comprehension of the energy spectrum due to the ETF and the Athermals (TRL = 3 - 4) 55 Fe Photon (~ 6 ke. V) - - Athermal pulse ……. Thermal pulse ~ 1 us Rise time By doubling the area scales per 2 as expected Cu Kα + kβ ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Cryo. AC design and mechanical I/F with the TES array Work started with the SRON team, shared ideas and preliminary size of the Cryo. AC active area (silicon absorber) which will contribute to the FPA design, to be updated by GEANT 4 vs Mass Model Credits Henk van Weers (SRON) ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics About the CFEE, WFEE and WBEE, all the electronics functions from warm to cold have been well framed by the italian teams; a power budget and preliminary sizes have been also detailed. - WFEE (1 board-for-4 pixels) it biases the Cryo. AC pxl and the SQu. IDs; FLL - WBEE (2 boards: N + R) will process the analog pulses from the WFEE , and HK to the ICU; No VETO onboard. It manages the WFEE in diagnostic mode (FLL, V-PHI, test pulses. . . ). The electronics at present TRL = 3 (conservative). We are studying the solution of a single box which includes WFEE + WBEE ➢EMI towards the TES array, since the box is connected to the cryostat? ➢Power from PDU and PSU, or only PDU and the clean power is internally generated? - SQu. ID: we are in touch with Mikko. We adopt a single stage SQu. ID, Series Array, at 50 m. K - SQu. ID as single stage: 16 SSA ~ 3 n. W per chip. Implementation close to the Cryo. AC to reduce stray inductance due to long wires, 4*3 = 12 n. W @ 50 m. K - Power Supply: we are in touch with R. Cole ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics The WFEE We have in mind to develop an EQM of the WFEE. To be discussed later during the DM activity talk. ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics The WBEE Budgets: • Mass: 2. 1 kg (+50% DMM) • Volume: < 260 x 60 mm 3 (+20% DMM) • Power: 15 W (NOM boards switched on) ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics DC/DC board: • Generate ± 5 V, +3. 3 V, +2. 5 V etc. from +28 V (PDU) BEE board: • AD conversion of the 4 WFEE analog channels; • Time from PPS and 1 -MHz signals from ICU (dedicated LVDS link); • Data archiving of the signals (with a time tag) if a threshold is trepassed; • Data processing of the archived signal to generate the following values: starting time, rise time, thermal tau, athermal tau, time difference from previous event, etc. ; • Data packet creation and transmission to ICU (Space. Wire); • HK collection from WFEE (voltages, currents, temperatures, . . . ) and WBEE itself and transmission to ICU; • Sends TCs to the WFEE for setting bias voltages for SQUIDs and TESs ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Update at IAPS Roma Lab. activities: – Magnetic shielding in production (Solid. Works + Comsol) Credits: Matteo D’Andrea • S/C lead deposited on Copper • Cryophy (high magnetic permeability at cryo, test ring to be sento to SRON) • Increased the lenght of the cold finger necessary to have the optimal L/D tubes size ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›

ATHENA : the Advanced Telescope for High ENergy Astrophysics Conclusions • Produced 3 pixels to verify: – Working temperature with Tb = 50 m. K – Wide coverage for the Athermal collections – Nb wiring for high current bias • Along 2015, tests of the 3 samples to get TRL = 4 at single pixel level • Vibration mask by CNES at the FPA level • External Service for both cold and warm electronics, and therm/elect/mech interfaces • IT IS NECESSARY TO HAVE AN INTERNAL SCHEDULE BETWEEN INAF AND SRON DRIVEN BY CNES ATHENA Italian Team, X-IFU meeting with CNES/IRAP, Genova, 4 March 2015 ‹N›