,
,
, Basic reminders of spectroscopy
, Soft and hard X-ray all-sky surveys
, 7 A1689 and Bullet cluster X-ray + optical observations, p.11
, Eagle cosmological simulation cube
, Historical first use of the ?-model
Normalised temperature profiles of clusters of galaxies, p.15 ,
Cavities and bubbles. The interplay between the ICM and the, p.16 ,
Perseus cluster spectral observations: from Ariel V to XMM, vol.18 ,
, Examples of supernovae remnants
,
Metallicity and abundance ratios in clusters of galaxies, p.23 ,
, Effective area of the Athena mirror
, Mirror design for the Athena telescope
,
,
, , p.37
,
,
, The CryoAC and effect on the NXB
, , vol.46
48 3.1 Steps of an E2E simulation ,
78 3.14 Exposure time penalty for degradations in the energy resolution, 103 4.8 Reconstructed radial metallicity profiles for Z ,
148 5.8 Systematic errors introduced by changes in absorber thickness, 139 5.4 Possible solutions in (f , M ), vol.146 ,
, Results of NXB monitoring using the CryoAC
Mechanical and thermal design of the test bench, p.163 ,
, Set up of the test bench
,
, Degradation of the energy resolution as a function of the current noise, p.167
, Design of the radioactive source
, Heat load tests set-up
, Magnetic field measurements set-up
, 177 II Observational strategies to measure the ICM turbulence, p.178
, 206 v Count rate capability of the X-IFU for extended sources under TDM, p.207
, , p.35
, , p.55
Models of the sources used for count rate studies, p.68 ,
, Scaling laws for line sensitivity
, Cluster toy model used for NXB studies
Effect of systematic errors in the NXB knowledge, p.86 ,
, Properties of the cluster data set
Systematic error estimation in the recovered parameters, p.100 ,
,
, Comparison of energy scale correction techniques
, Hold time measurements
, Magnetic shielding measurements
213 iv Counts needed in each MXS line, iii List of lines used for atomic studies ,
, 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=
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
, , 1999.
, , 2010.
, , 2018.
, 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
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 ,
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) ,
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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