Advanced Telescope for High Energy Astrophysics
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1 Advanced Telescope for High Energy Astrophysics Etienne Pointecouteau IRAP (Toulouse, France) Member of the Athena Collaboration and of the X-IFU Science Team
2 Why does the observable universe look the way it does? Dark matter assembly of structures By 2028 Cosmology setup of the Universe Gravitational assembly of structures Euclid, erosita, SPT3G, LSST, etc Which science?
3 Why does the observable universe look the way it does? 1. How does ordinary matter assemble into the large scale structures we see today? 2. How do black holes grow and shape the Universe?
4 Key questions for observational astrophysics in How does ordinary matter assemble into the large scale structures we see today? Extended X-ray sources Athena Deep Field
5 Finding the earliest galaxy groups Testing astrophysical cosmology at the largest scales As a way to constrain models of largescale structure formation, find the first building blocks of the dark matter structure filled with hot gas. Athena will be able to detect ~ groups with mass M 500 > M sun at z>2. And measure T of ~50% of them Athena Simulation Pointecouteau, Reiprich et al., 2013 arxiv
6 The formation and evolution of clusters and groups of galaxies How and when was the energy contained in the hot intra-cluster medium generated? z=1 M=10 14 M 1000 Pointecouteau, Reiprich et al., 2013 arxiv Entropy profile Pure gravitation Entropy With AGN and supernova heating 100 Athena Simulation Radius (kpc)
7 The formation and evolution of clusters and groups of galaxies How and when was the energy contained in the hot intra-cluster medium generated? z=1 z= M=10 14 M Entropy profile M=5x10 13 M Pointecouteau, Reiprich et al., 2013 arxiv Pure Pure gravitation Entropy With With AGN AGN and and supernova heating 100 Athena Simulation Radius (kpc)
8 The formation and evolution of clusters and groups of galaxies How and when was the energy contained in the hot intra-cluster medium generated? Simulated Velocity map 100 km/s 500 Ettori, Pratt, et al., 2013 arxiv
9 The chemical evolution of hot baryons When and how were the largest baryon reservoirs in galaxy clusters chemically enriched? Ettori, Pratt, et al., 2013 arxiv
10 The chemical evolution of hot baryons When and how were the largest baryon reservoirs in galaxy clusters chemically enriched? Ettori, Pratt, et al., 2013 arxiv
11 The chemical evolution of hot baryons When and how were the largest baryon reservoirs in galaxy clusters chemically enriched? M ; z=2 cluster Ettori, Pratt, et al., 2013 arxiv
12 The Warm-Hot intergalactic medium (WHIM) Where are the missing baryons in the local Universe? What is the underlying mechanism determining the distribution of the hot phase of the cosmic web? Kaastra, Finoguenov et al., 2013 arxiv
13 The Warm-Hot intergalactic medium (WHIM) Where are the missing baryons in the local Universe? What is the underlying mechanism determining the distribution of the hot phase of the cosmic web? Kaastra, Finoguenov et al., 2013 arxiv
14 Key questions for observational astrophysics in 2028 X-ray point sources 2. How do black holes grow and shape the Universe? Athena Deep Field
15 Black hole growth in the early Universe What was the growth history of black holes in the epoch of reionization? Aird, Comastri et al arxiv
16 Black hole growth in the early Universe What was the growth history of black holes in the epoch of reionization? Aird, Comastri et al arxiv
17 Early Super-Massive Black Holes What were the seeds of the early SMBH? How did they grow in the early stages after cosmic reionisation? Determine the nature of the seeds of high redshift (z>6) SMBH, which processes dominated their early growth, and the influence of accreting SMBH on the formation of galaxies in the early Universe. Trace the first generation of stars to understand cosmic re-ionization, the formation of the first seed black holes, and the dissemination of the first metals in the Universe.
18 Cosmic feedback: black hole and galaxy co-evolution How much black hole accretion occurs in the most obscured environments? How do black holes launch winds and outflows? How much energy do they carry out to large scales? How does this relate to the evolution of the host galaxy? Disk instability Obscured BH growth Feedback phase Ceverino et al Quiescent remnant Merger Hopkins et al.2006 Georgakakis, Carrera, et al arxiv Cappi, Done et al., 2013 arxiv Dovciak, Matt et al., 2013 arxiv
19 Cosmic feedback: the impact on galaxy cluster scales How do jets from Active Galactic Nuclei dissipate their mechanical energy in the hot intracluster medium, and how does this regulate gas cooling and black hole fuelling? 5 region Croston, Sanders et al., 2013 arxiv
20 Athena/X-IFU full simulation A2146 by X-IFU within 100ks photons/cm 2 /s photons/cm 2 /s Energy [kev] Energy [kev] Courtesy of Thomas Dauser and Joern Wilms
21 Planets (interaction of solar wind with planet environment and comets) Exoplanets Stellar physics Supernovae (explosion mechanism, heavy element production) Stellar endpoints (physics of outflows and winds in X-ray binaries) Sgr A* Interstellar dust and medium High-energy transients Athena: a powerful observatory Jupiter Tycho Outflow1in1X4ray1binary,110ks Branduardi-Raymont, Sciortino, et al., 2013 arxiv ; Sciortino, Rauw et al., 2013 arxiv ; Motch, Wilms, et al., 2013 arxiv ; Decourchelle, Costantini et al., 2013 arxiv
22 By 2028: new constraints, new physics, new goals? Flux (cnts s -1 kev -1 ) 10 Ar XVII Ar XVIII Perseus Athena XIFU 150 ks kt = 6.5 kev v(baryons) = 300 km/s v(line) = 1300 km/s Ar XVII DR Ca XIX kev Line Energy (kev) Courtesy of Esra Bulbul
23 Nandra et al arxiv Athena1 Satellite mass ~ 5500 kg L2 orbit Focal length: 12 m kev Lifetime: 5 years (10 years) ESA cost cap of 1B External contributions (NASA, JAXA) Athena is our next large ESA mission Silicon Pore Optics:1 Willingale et al arxiv
24 WFI - The wide field imager Rau et al arxiv: Based on DEPFET active pixel sensor with two separate on-axis positions: 40 x40 : optimized for wide FoV applications 2.3 x2.3 : optimized for high-count rate applications European consortium lead by MPE (DE) with partners in DE, UK, PO, AU, DK, IT, FR Energy range Parameter Energy resolution Value kev kev Field of view 40 x 40 Angular resolution Detector 5 (on axis) 10 (at 20 arcmin) 4x 512x512 DEPFET chips 1x 64x64 fast chip Quantum efficiency Non-Xray background 1 kev ; 10 kev <5 E-3 count/s/cm 2 /kev
25 Barret et al arxiv: X-IFU - The X-ray integral field Unit TES micro-calorimeter detectors, cooled down at 50mK Multi-stage cryogen free mechanical coolers to guarantee a 5 year (+5) Cryogenic active anticoincidence European consortium lead by IRAP (FR) with partners in NL, IT, SP, SW, BE, PO, DE + US and Japan contributions Energy range Parameter Energy resolution (E<7 kev) Value kev 2.5 ev Field of view 5 diameter (goal 7 ) Angular resolution 5 (goal 3 ) Detector Quantum efficiency Gain error (rms) Non-Xray background 3840 TES 1 kev ; 7 kev 0.4 ev <5 E-3 count/s/cm 2 /kev
26 A Deep Universe X-ray Observatory Athena has vastly improved capabilities compared to current or planned facilities, and will provide transformational science on virtually all areas of astrophysics Line Sensitivity 1001x1ASTRO4H 10001x11 Survey Speed XMM4Newton X-ray spectroscopy at the peak of the activity of the Universe Deep survey capability into the dark ages and epoch of reionization
27 The Athena community Athena Science Study Team (ASST) SWG1 - Hot Universe SWG2 - Energetic Universe SWG3 - Observatory TWG4 -Telescope MWG5 -Mission Performances
28 Athena The next european X-ray observatory part of ESA Cosmic Vision A quantum leap forward in X-ray astronomy A powerful versatile observatory Contribution from US and Japan A large community with ~680 members to the ASST WGs Milestones Selection of the Science theme The hot and energetic Universe Selection of the Athena mission Instrument AO Technology development phase Mission adoption by ESA Instrument flight model delivery Launch Conclusions First Athena scientific conference 8-10/09/ Exploring the Hot and Energetic Universe
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