Advanced Telescope for High Energy Astrophysics Etienne Pointecouteau IRAP (Toulouse, France) Member of the Athena Collaboration and of the X-IFU Science Team
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?
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?
Key questions for observational astrophysics in 2028 1. How does ordinary matter assemble into the large scale structures we see today? Extended X-ray sources Athena Deep Field
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 > 5 10 13 M sun at z>2. And measure T of ~50% of them Athena Simulation Pointecouteau, Reiprich et al., 2013 arxiv1306.2319
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 arxiv1306.2319 Entropy profile Pure gravitation Entropy With AGN and supernova heating 100 Athena Simulation 10 100 1000 Radius (kpc)
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=2 1000 M=10 14 M Entropy profile M=5x10 13 M Pointecouteau, Reiprich et al., 2013 arxiv1306.2319 Pure Pure gravitation Entropy With With AGN AGN and and supernova heating 100 Athena Simulation 10 100 1000 Radius (kpc)
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 arxiv1306.2322
The chemical evolution of hot baryons When and how were the largest baryon reservoirs in galaxy clusters chemically enriched? Ettori, Pratt, et al., 2013 arxiv1306.2322
The chemical evolution of hot baryons When and how were the largest baryon reservoirs in galaxy clusters chemically enriched? Ettori, Pratt, et al., 2013 arxiv1306.2322
The chemical evolution of hot baryons When and how were the largest baryon reservoirs in galaxy clusters chemically enriched? 10 14 M ; z=2 cluster Ettori, Pratt, et al., 2013 arxiv1306.2322
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 arxiv1306.2324
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 arxiv1306.2324
Key questions for observational astrophysics in 2028 X-ray point sources 2. How do black holes grow and shape the Universe? Athena Deep Field
Black hole growth in the early Universe What was the growth history of black holes in the epoch of reionization? Aird, Comastri et al. 2013 arxiv1306.2325
Black hole growth in the early Universe What was the growth history of black holes in the epoch of reionization? Aird, Comastri et al. 2013 arxiv1306.2325
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.
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. 2010 Quiescent remnant Merger Hopkins et al.2006 Georgakakis, Carrera, et al. 2013 arxiv1306.2328 Cappi, Done et al., 2013 arxiv1306.2330 Dovciak, Matt et al., 2013 arxiv1306.2331
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 arxiv1306.2323
Athena/X-IFU full simulation A2146 by X-IFU within 100ks 10-4 10-4 10-5 10-5 10-3 0.8 0.9 0.8 0.9 10-3 10-4 10-4 photons/cm 2 /s 10-5 10-6 10-5 10-6 photons/cm 2 /s 10-7 1 10-7 0.5 1 2 5 10 Energy [kev] 0.5 1 2 5 10 Energy [kev] Courtesy of Thomas Dauser and Joern Wilms
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 1306.2332; Sciortino, Rauw et al., 2013 arxiv1306.2333; Motch, Wilms, et al., 2013 arxiv1306.2334; Decourchelle, Costantini et al., 2013 arxiv1306.2335
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 5 3.55 kev Line 3 3.2 3.4 3.6 3.8 4 Energy (kev) Courtesy of Esra Bulbul
Nandra et al. 2013 arxiv1306.2307 Athena1 Satellite mass ~ 5500 kg L2 orbit Focal length: 12 m 2m2 @1keV 0.26 m2 @ 6 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. 2013 arxiv1308.6785
WFI - The wide field imager Rau et al. 2013 arxiv:1308.6785 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 0.1-15 kev 150 ev @ 6 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 87% @ 1 kev ; 96% @ 10 kev <5 E-3 count/s/cm 2 /kev
Barret et al. 2013 arxiv:1308.6784 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 0.2-12 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 >60% @ 1 kev ; >70% @ 7 kev 0.4 ev <5 E-3 count/s/cm 2 /kev
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
The Athena community Athena Science Study Team (ASST) SWG1 - Hot Universe SWG2 - Energetic Universe SWG3 - Observatory TWG4 -Telescope MWG5 -Mission Performances
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 2013 - Selection of the Science theme The hot and energetic Universe 2014 - Selection of the Athena mission 2016 - Instrument AO 2014-2018 - Technology development phase 2019 - Mission adoption by ESA 2025 - Instrument flight model delivery 2028 - Launch Conclusions First Athena scientific conference 8-10/09/2015 - Exploring the Hot and Energetic Universe http://www.sciops.esa.int/index.php?project=conf2015&page=athena2015