The Athena X-ray Observatory (and its X-ray Integral Field Unit) Didier Barret Ins=tut de Recherche en Astrophysique et Planétologie

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1 The Athena X-ray Observatory (and its X-ray Integral Field Unit) Ins=tut de Recherche en Astrophysique et Planétologie Many thanks to the Athena Science Study Team: D. Lumb, K. Nandra, X. Barcons, J.W. den Herder, A. Decourchelle, A.C. Fabian, H. Matsumoto, L. Piro, R. Smith, R. Willingale, the Athena working groups and topical panels, the X-IFU Science Advisory Team, and the X-IFU Consor=um

2 Outline - Athena science - The Hot and Energe=c Universe - Athena science payload - X-ray Integral Field Unit (X-IFU) performance op=miza=on - relevant probing super-eddington accre=on - Athena current status - Conclusions 2

3 Athena science - Scien=fic theme: The Hot and Energe=c Universe - How does ordinary ma]er assemble in the large-scale structures? - Tool: X-ray emi_ng hot gas in clusters - How do black holes grow and shape galaxies? - Tool: Accre=on powered X-rays onto compact objects - Together with: - Observatory science from planets, stars, supernova remnants, interstellar medium - Discovery science enabled in par=cular through a fast ToO capability to study the transient sky Need to combine a large aperture X-ray telescope, wide field imaging, highresolu=on spectroscopy and an agile spacecrac 3

4 Athena in a nutshell - Second Large (L) mission of the ESA Cosmic Vision Launch year: end of with the newly developed Ariane 6 (64) - A 7 ton spacecrac to be placed in a L2(L1) orbit - Unprecedented collec=ng area in X-rays: - 2 m 2 at 1 kev and 0.17 m 2 at 7 kev - 5 angular resolu=on - Two focal plane instruments with a movable mirror assembly - The Wide Field Imager (WFI) op=mized for fine imaging and bright sources - The X-ray Integral Field Unit (X-IFU) op=mized for high-resolu=on spectroscopy 4

5 The Hot Universe - key ques=ons - How do baryons in groups and clusters accrete and dynamically evolve in the dark ma]er haloes? - What drives the chemical and thermodynamic evolu=on of the Universe largest structures? - What is the interplay of galaxy, supermassive black hole, and intergalac=c gas evolu=on in groups and clusters? - Where are the missing baryons at low redshic and what is their physical state? 5

6 Hot Universe Accre=on in dark ma]er haloes Map gas mo=ons and turbulence to understand how baryons accrete and evolve in the largest dark ma]er poten=al wells of groups and clusters. Chemical enrichment Synthesize the abundances using yields of various SN types and AGB stars to determine when the largest baryon reservoirs in galaxy clusters were chemically enriched 1 O Fe L Mg Si S Ar Ca 10 1 Fe-K Counts/s/keV Athena X-IFU XMM-Newton EPIC PN Hitomi SXS Simulated velocity maps (courtesy of Ph. Peille et al.). E9ori, Pra9 et al. (2013) arxiv Energy (kev) High resolucon X-ray spectrum of a z=1 cluster. Pointecouteau, Reiprich et al (2013), arxiv:

7 Hot Universe Cluster feedback Measure hot gas bulk mo=ons and energy stored in turbulence directly associated with the expanding radio lobes to understand how jets from AGN dissipate their mechanical energy in the intracluster medium, and how this affects the hot gas distribu=on Missing baryons Measure the chemical composi=on, density, size, temperature, ioniza=on and turbulence of the missing 50% of baryons at z<2 and reveal the underlying mechanisms driving their distribu=on on various scales, from galaxies to galaxy clusters, as well as metal circula=on and feedback processes Residuals (σ) OVIII Kα 8 10 OVII Kα OVII Kα OVII Kα OVII Kβ NeIX Kα SpaCally revolved high resolucon spectroscopy of the Perseus cluster- Hitomi collaboracon (2016) Energy (kev) MulC-filament WHIM absorpcon X-ray spectrum using GRB arerglow. Barret et al. (2016), Courtesy of F. Nicastro 7

8 The Energe=c Universe - key ques=ons - How do early supermassive black holes form, evolve and shape the Universe? - What is the role of (obscured) black hole growth in the evolu=on of galaxies? - How do accre=on-powered oumlows affect larger scales via feedback? - How do accre=on and ejec=on processes operate in the near environment of black holes? 8

9 Energe=c Universe Black hole growth Determine the nature of the seeds of high redshic (z>6) SMBH, which processes dominated their early growth, and the influence of accre=ng SMBH on the forma=on of galaxies in the early Universe. Obscured accre=on Find the physical condi=ons under which SMBH grew at the epoch when most of the accre=on and star forma=on in the Universe occurred (z~1-4) Flux distribucon of AGNs in comparison with model prediccons. Aird, Comastri et al. (2013) arxiv Compton thick AGN spectrum. Georgakakis, Carrera et al., (2013 ) arxiv

10 Energe=c Universe AGN oumlows Characterize ejecta, by measuring ioniza=on state, density, temperature, abundances, veloci=es and geometry of absorp=on and emission features of the winds and oumlows and determine how much energy these carry. Black hole winds Probe oumlow proper=es and disk magne=c fields in galac=c binaries and in the same systems determine the rela=onship between the accre=on disk and its hot electron plasma. Understand the interplay of the disk/corona system with ma]er ejected in the form of winds and oumlows. Counts/s/keV FeXXV (v=0.25c) FeXXV (v=0.25c) FeXXV (v=0.3c) logξ=4.2 (high state) logξ=3.9 (low state) FeXXVI (v=0.3c) Normalized counts/s/kev/cm Fe XXV Heα Energy (kev) Simulated ultra-fast ou\low spectrum - Cappi, Done et al 2013, arxiv: Fe XXVI Hα Fe XXV Heβ Fe XXVI Hβ Energy (kev) Disk wind spectrum of the stellar mass black hole GRS Barret et al (courtesy J. Miller) 10

11 Athena performance requirements Parameter Value Driving science goals Op=cs Effec=ve area at 1 kev 2 m 2 Early groups, cluster entropy and metal evolu=on, WHIM, high redshic AGN, census of AGN, first genera=on of stars Effec=ve area at 7 kev 0.17 m 2 Cluster energe=cs (gas bulk mo=ons & turbulence), AGN winds & oumlows, SMBH & GBH spins PSF HEW (< 8 kev) 5 on axis, 10 off axis High z AGN, census of AGN, early groups, AGN feedback on cluster scales X-IFU X-IFU spectral resolu=on 2.5 ev WHIM, cluster hot gas energe=cs and AGN feedback on cluster scales, energe=cs of AGN oumlows at z~1-4 X-IFU field of view 5 diameter Metal produc=on & dispersal, cluster energe=cs, WHIM X-IFU background < counts/s/cm 2 /kev Cluster energe=cs & AGN feedback on cluster scales, metal produc=on & dispersal X-IFU count rate capability WFI 1 mcrab 80% high-res events WHIM using GRB acerglows WFI spectral resolu=on 150 ev GBH spin, reverbera=on mapping WFI field of view 40 x 40 High-z AGN, census AGN, early groups, cluster entropy evolu=on, jet-induced ripples WFI count rate capability 80% throughput at 1 Crab GBH spin, reverbera=on mapping, accre=on physics WFI background < counts/s/cm 2 /kev Cluster entropy, cluster feedback, census AGN at z~1-4 Recons. astrometric error 1 (3 sigmas) High z AGNs Satellite ToO trigger efficiency 40% in less than 4 hours WHIM, first genera=on of stars 11

12 Observatory and discovery science - Solar system bodies: sun interac=on - Exoplanets: magne=c interplay - Star forma=on: brown dwarfs - Massive stars: stellar winds - Supernovae: explosion mechanisms - Supernovae remnants: shock physics - Interstellar medium: composi=on - Stellar endpoints: dense ma]er at supra nuclear densi=es - Discovery science: unknowns Normalized counts/s/ang Solar scattered Fe and Ne Fe XVII OVIII Ly α Broad OVIII Ly α Fe XVIII OVIII Ly β Jupiter X-IFU Charge exchange Broad OVII CVI SXII SXI Wavelength (Ang) 12

13 Payload OpCcs Wide Field Imager X-ray Integral Field Unit Light-weight Si-pore opccs AcCve Pixel Sensors based on DEPFETs Cryogenic imaging spectrometer, based on a large format of TransiCon Edge Sensors cooled at 50 mk with an accve background shielding ESA & industry ConsorCum led by MPE (K. Nandra), with other European partners and NASA ConsorCum led by IRAP/CNES-F (D. Barret), with SRON-NL (J.W. den Herder), INAF/IAPS-IT (L. Piro) and other European partners, NASA and JAXA. Breaking the limits, September 21st 2016, Arbatax, Italy Didier Barret 13

14 X-IFU performance op=miza=on - Poten=al for improvements: count rate & spectral resolu=on (1.5 ev) & PSF oversampling TES array baseline configura=on - single size pixels Addi=on of a Small Pixel Array 5 equivalent diameter field of view Barret et al. (SPIE 2016) 14

15 X-IFU count rate capability Frac=on of high resolu=on events (2.5 ev) Throughput for high and mid resolu=on events (<3-4 ev) Fraction of high resolution events 1,0 0,9 0,8 0,7 0,6 0,5 0,4 0,3 0,2 0,1 LPA 1 (in focus) LPA 2 (15 mm out of focus) LPA 2 (35 mm out of focus) SPA (in focus) Req. Goal Intensity (mcrab) Throughput (High+Medium resolution events) LPA 1 (in focus) LPA 2 (15 mm out of focus) LPA 2 (35 mm out of focus) SPA (in focus) Bright sources Intensity (mcrab) 1 mcrab = 95 cps/s (over the whole detector array) Barret et al. (SPIE 2016) Breaking the limits, September 21st 2016, Arbatax, 15

16 Effec=ve area = spectroscopic capabili=es Effec=ve area comparison between X-IFU and other facili=es 10 4 x 15 Effective area (cm 2 ) x 100 x X-IFU EPIC PN SXS NuSTAR 1 10 Energy (kev) 16

17 Effec=ve area = spectroscopic capabili=es Figure of merit for spectroscopy measurements 25 Athena X-IFU Hitomi SXS Gratings Figure of merit (m kev -1/2 ) Energy (kev) 17

18 Spectroscopic capabili=es 8.8 kev absorp=on line in NGC1313 X-1 seen by XMM-Newton and NuSTAR - Rela=vis=c oumlow Fe XXV (6.67 kev, 0.25 c) or Fe XXVI Kα (6.97 kev, 0.2 c) Broad band spectroscopic capability of X-IFU NGC 1313 X-1 X-IFU s Walton et al.(2016) Photons/s/keV/cm X-IFU simulated spectrum XSTAR based model of NuSTAR data Energy (kev) 2.0 Photons/s/keV/cm2 NGC 1313 X-1 X-IFU s X-IFU simulated spectrum XSTAR based model of NuSTAR data Energy (kev) Breaking the limits, September 21st 2016, Arbatax, Italy Didier Barret 18

19 Current status of Athena - Mission Consolida=on Review (May 2016) concluded that: - The two missions concepts studied (small and large mirrors) are sound - The instrument switching mechanism is through a movable mirror assembly - Offers also defocussing to increase the X-IFU count rate capability - The instrument resources are challenging: all being addressed or fixed - The mass lic capacity of Ariane 64 up to 7 tons - Consolida=on of the cost at comple=on is required (transfer of focal plane module to the instrument consor=a, firming up interna=onal contribu=on to the mission and some payload elements, industrial costs, ) - Mission concept to be carried over considers the large mirror 19

20 Conclusions - Athena will provide breakthrough capabili=es in wide field imaging and high resolu=on X-ray spectroscopy - Athena feasibility studies are progressing well - The large mirror configura=on is the baseline for the upcoming study phase - Instrument baseline designs are being consolidated with no degrada=on of performance up to now - Join the Athena community and support the mission - X-IFU will be a powerful tool to study super-eddington accre=on: - disk coronae, winds, rela=vis=c oumlows, surrounding materials thus enabling to connect accre=on physics to feedback process across the broad mass scale of compact objects - See more from C. Pinto, M. Middelton 20

21 Hold on and thank you for your support The wealth of informa=on provided by such a spectrum, that will be measured on sub-arc minute scales enables in depth studies of the physical proper=es of the hot cluster gas (e.g. temperature, density, turbulence, bulk mo=on, abundance,... ) High-z GRB acerglows probing the ISM composi=on at z>7-10 and tracing the first genera=on of stars to understand cosmic reioniza=on, the forma=on of the first seed black holes, and the dissemina=on of the first metals X-IFU - Perseus core Photons m -2 s -1 kev νf ν Fe complex Al, Si, S Energy (kev) Perseus core X-IFU simulated spectrum based on Hitomi - Model courtesy of C. Pinto and A. Fabian Energy (kev) Barret et al. (2016) - Courtesy of L. Piro Breaking the limits, September 21st 2016, Arbatax, 21