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. .. , 218 Acronyms AC: Alternative Current ACIS: Advanced CCD Imaging Spectrometer ADC: Analogue-to-Digital Converter ADR: Adiabatic Demagnetisation Refrigerator AGB: Asymptotic Giant Branch AGN: Active Galactic Nucleus APC: Astrophysique et Cosmologie ARF: Ancillary Response File ASIC: Application Specific Integrated Circuits ATHENA: Advanced Telescope for High-Energy Astrophysics BBFB: Base-Band Feedback BCG: Brightest Cluster Galaxy BH: Black Hole CAD: Computer-Aided Design CC/NCC: Cool-Core/Non-cool-core cluster CCCM: Channel-Cut Crystal Monochromator CCD: Charged-Coupled Device CDM: Cold Dark Matter (also Code Domain Multiplexing) CFEE: Cold Front-End Electronics CFRP: Carbon-Fibre Reinforced Polymer CMB: Cosmic Microwave Background CNES: Centre National d'Études Spatiales CPU: Central Processing Unit CREME: Cosmic

, CryoAC: Cryogenic Anti-Coincidence detector CXB: Cosmic X-ray Background DAC: Digital-to-Analogue Converter DC: Direct Current DCS: Detector Cooling System DDS: Direct Digital Synthesiser DEPFET: Depleted p-channel Field-Effect Transistor DM: Dark Matter DRE: Digital Readout Electronics E2E: End-To-End EBIT: Electron-Beam Ion Trap ECAP: Erlangen Centre for Astroparticle Physics EM: Emission-Measure EMW: Emission-Measure-Weighted EPIC: European Photon Imaging Camera ERB: Energy Resolution Budget ESA: European Space Agency ETF: Electro-Thermal Feedback EW: Emission-Weighted FAA: Ferric Ammonium Alum FB: FeedBack FE: Front End FoV: Field-of-View FDM: Frequency Domain Multiplexing FPA: Focal Plane Assembly FPGA: Field-Programmable Gate Arrays FW: Filter Wheel FWHM: Full Width at Half Maximum GCR: Galactic Cosmic Ray GGG: Gadolinium-Gallium Garnet GPU: Graphic Processing Unit GRB: Gamma-Ray Burst GSE: Ground Support Equipment GFSC: Goddard Space Flight Center (NASA) GW: Gravitational Wave HETG: High-Energy Transmission Grating HEW: Half-Energy Width HFI: High Frequency Instrument HWHM: Half Width at Half Maximum ICM: Intra-Cluster Medium ICS: Inner Cryogenic Shield ICU: Instrument Control Unit IPCS: Inner Passive Cryogenic Shield IFCA: Istituto de Fisica de Cantabria IFU: Integral Field Unit IGM: Intergalactic Medium IRAP: Institut de Recherche en Astrophysique et Planétologie ISM: Interstellar Medium ITFN: Internal Thermal Fluctuation Noise IXO: International X-ray Observatory JT: Joule-Thomson

, Line Spread Function LUT: Look-Up Table MAM: Mirror Assembly Module MC: Monte Carlo MM: Mirror Module MOSFET: Metal-Oxyde Semiconductor Field-Effect Transistor MW: Mass-Weighted MXS: Modulated X-ray Source NEP: Noise Equivalent Power NS: Neutron Star NXB: Non-X-ray Background OCS: Outer Cryogenic Shield OV: Outer Vessel PAMELA: Payload for Antimatter/Matter Exploration and Light-nuclei Astrophysics PCB: Printed Circuit Board PDU: Power Distribution Unit PHA: Pulse Height or Pulse Height Amplitude PSF: Point Spread Function PT: Pulse Tube (cooler) QE: Quantum Efficiency RGS: Reflection Grating Spectrometer RK: Runge-Kutta RMF: Redistribution Matrix File RMS: Root Mean Squared RSJ: Resistively Shunted Johnson (model) RSS: Root Sum Squared RTU: Remote Terminal Unit S/N: Signal-to-Noise ratio SIM: Science Instrument Module SIMPUT: Simulation input

, SIXTE: Simulator for X-ray Telescopes SMBH: Supermassive Black Hole SNe Supernovae SNR: Supernova Remnant (also Signal-to-Noise Ratio) SNRD: Signal-to-Noise Ratio Density SOHO: Solar and Heliospheric Observatory SPH: Smoothed Particle Hydrodynamics SPO: Silicon Pore Optics SQUID: Superconducting Quantum Interference Device SRG: Spectrum Roentgen-Gamma SREM: Standard Radiation and Environment Monitor SVOM: Space Variable Objects Monitor SXI: Soft X-ray Imager SXS: Soft X-ray Spectrometer SZ: Sunayev Zel'dovich (effect) TDM: Time Domain Multiplexing TES: Transition Edge Sensor TFN: Thermal Fluctuation Noise TTR: Transformer Turns Ratio ToO: Target of Opportunity UFO: Ultra-Fast Outflow UV: Ultra-Violet WD: White Dwarf WFEE: Warm Front-End Electronics WHIM: Warm Hot Intergalactic Medium WFI: Wide Field Imager XCaT: X-IFU Calibration Team XIS: X-ray Imaging Spectrometer X-IFU: X-ray Integral Field Unit XMS: X-Ray Micro-calorimeter Spectrometer XRB: X-Ray Binary XRISM: X-Ray Imaging Spectroscopy Mission

, /> <readout mode="event"/> "x-ifu" pixeltype="LPA_75_AR0.5" npix="3832" xoff="124.5e-6" yoff="124.5e-6"> <samplefreq value="156.25e+3"/> <grading num="1" name="high" pre="494" post="8192" rmf="athena_xifu_rmf_highres_v20150609.rmf"/> <grading num="2" name=", /> <rmf filename="athena_xifu_sixte_v20150402.rmf"/> <phabackground filename="xifu_nxb_20170926.pha"/> <threshold_readout_lo_keV value="200.e-3"/> <threshold_event_lo_keV value=

&. Model=, BBFBSquid" filename="pars_8.fits" hduname="BBSquid"/> <DRE model="BBFB_DRE" filename="pars_8.fits" hduname="BBDRE"/> <ADC model="Adc" filename="pars_8.fits" hduname="ADC_16_LPA75um"/> <Trigger model=

, Zinit = 3 Z 500-5-c3 13 2D del.-det., ?9 = 5.0, centred ignit

, Merger 09_09 15 3D violent WD merger (double-degen.), 0.9+0.9 M 11_09 16 3D violent WD merger (double-degen.), 1.1+0.9 M Merger2 09_076 17 3D violent WD merger (double-degen.), 0.9+0.76 M , Zinit = 1 Z 09_076_Z0.01 17 3D violent WD merger (double-degen.), 0.9+0.76 M , Zinit = 0.01 Z 6D Sh18_Ma_b_Zc_d 18 3D dynamically-driven double-degenerate double detonation, 159 models in total for different WD masses

;. Sn-ia and . Iwamoto, , 1999.

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. Nomoto, Heger & Woosley (2002) (f) Heger & Woosley (2010) (g) Sukhbold et al. (2016) AGB: (?) Karakas, 2004.

, MXS configurations and line centroid uncertainties

, After discussion with SRON, and following the results presented in de Vries, 2018.

, Two-line configuration (so-called "Hitomi-like") obtained with a layer of 250 nm of Cu on top of 150 nm of Cr. The fluorescence yields per line are: 45% Cr K ? / 5% Cr K ? / 45% Cu K ? / 5% for Cu K ? III. Three-line configuration obtained with a 250 nm of Cu, above a 150 nm of Cr, on top of 150 nm of Ti. The fluorescence yields per line are, The fluorescence yields per line are: 90% Cu K ? / 10% Cu K ? II

. Cr-k-?-/-4%-cr-k-?-/-36%-cu-k-?-/-4%-cu-k-?-iv, Four-line configuration obtained with 250 nm of Cu, above 150 nm of Cr, above 150 nm of Ti, on top of 700 nm of Si. The yields per line are

K. Si-k-?-/-20%-ti-k-?-/-2%-ti, 30% Cr K ? / 3% Cr K ? / 31% Cu K ? / 3% Cu K ? An additional 55 Fe source was also considered for line studies (which creates a Mn K ? doublet through Auger electron loss)

T. Si, . Mn, . Cr, and ). Cu, we summarise in Table iv the number of counts required to get a 0.2 eV (FWHM) uncertainty on the line centroid, as per the current X-IFU requirements on the energy scale

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