AC Fabian, M. Cappi, J Sanders. Cosmic Feedback from AGN

Transcription

1 AC Fabian, M. Cappi, J Sanders Cosmic Feedback from AGN

2 AC Fabian, M Cappi, J Sanders, S Heinz, E Churazov, B McNamara, J Croston, D Worrall, F Humphrey, F Tombesi, J Reeves, M Giustini, P O Brien, T Reiprich P Nulsen, T Ponman, N Werner, W Forman, A Young, N Brandt, G Chartas

3 Possible effect of central black hole on host galaxy E BlackHole 30 E Galaxy Energy released by growth of Black Hole Gravitational Binding Energy of Host Galaxy 2 major modes for the interaction: Kinetic (radio/jet) and Radiative (quasar)

4 KEY QUESTIONS 1) Understanding the energy flow in cool cores of clusters, groups and ellipticals: (Velocity field, bulk motions, shocks, turbulence ) 2) Understanding the energy and mass flow of AGN outflows: (Mass and energy components, velocity structure, variability, ionization structure ) X-rays are most direct probe of crucial volume-filling component

5 Cool Cores in Clusters X-ray brightest region in Clusters and Groups, with size ~100 kpc Radius of XMS FOV ~ 130 kpc at z~0.1, which is well matched to cool cores Need to map flows (velocities and line widths), Line strengths, metallicities etc Athena XMS offers order of magnitude (or more) improvement over ASTRO-H on spatial resolution and counts, and 2 on spectral resolution.

6 Chandra 1.4 Ms

7

8

9 M84 Hydra A

10 Perseus Athena XMS simulation FoV ~ counts per pixel in brightest region in 50ks observation Most of the structures are resolved with 10 PSF and much better than XMM 5 PSF is desirable, but not required

11 Perseus - simulated spectrum From Fe-K only: 38 km/s broadening (34 km/s absolute) From Fe-L only: 24 km/s broadening (24 km/s absolute) Can use soft and hard bands independently

12

13 Perseus bubble scan 250 ks Cygnus A at FeK

14 Centaurus measuring radiative cooling & metals

15 Abell 1835 more distant cluster at z = 0.25 Abell 1835: luminous x erg/s Readout XMS FoV Athena PSF is much better than XMM for removing point sources Note: the Athena images are smoothed and rebinned Chandra images

16 Abell 1835 Sim-X simulation with background 50 ks SIM-X simulation with XMS showing ct/pixel Including finite exposure time and background ICM easily visible out to several hundred kpc

17 Abell 1835 broadening comparison XMM: 260 ks RGS observation of 30 arcsec strip Athena & ASTRO-H: 50 ks observations of 7 radius region (not resolved by ASTRO-H) Thermal broadening only assumed Almost 10x better than the larger XMM region in 1/5 of the exposure time 12 km/s absolute velocity accuracy (90% level)

18 Sanders+09 v turb <274 km/s

19 Abell 1835 limits on cooling To understand AGN feedback we need to measure the gas distribution as a function of temperature What fraction successfully cools, forming stars? RGS results from Sanders et al ks Athena 2 simulations Assumes 100 Msun/yr cooling below 2.7 kev and hot component from 7 arcsec radius region

20 Cool Core Summary Athena well matched for science Background unlikely to be an issue (note surface brightness independent of z for nearby objects) WFI will carry out general cluster study simultaneously Results should enable major advances to be made

21 Outflows from AGNs and their feedback impact on galaxies/groups/clusters: Most important is to: i) Do detailed modeling and probe the outflow dynamics in brightest AGNs (to constrain geometry and location, hence energetics); ii) Characterize the outflow properties (N w,, out ) in QSOs up to z=2. Where we stand now: Theory Proga and Kallman 2004

22 PDS456 z=0.184 Reeves+09 Suzaku Kinetic power ~ erg/s XMM 2001 in red

23 Chartas et al

24

25 Absorption spectroscopy with calorimeter resolution up to 8-10 kev will revolutionize the field First probes of absorption line profiles (P-Cygni?) Probe of flow dynamics on short time-scales F. Tombesi Important to probe the geometry and location of the outflow, and therefore the total mass outflow and the kinetic power associated to AGN feedback.

26 What s s next? POPULATION STUDIES Minimum 2-10 kev flux to constrain (N W, ) within (20%, 10%) in a 100 ks observation QUANTIFY AGN FEEDBACK UP TO z~2 Margherita Margherita Giustini - Ph.D. Giustini Thesis defense, 16/05/2011 Bologna 15/04/2011

27 What s s next? INDIVIDUAL DETAILED STUDIES The ATHENA view of a mini-bal QSO PN 5 ks XMS 5 ks UNVEIL THE DYNAMICS OF THE INNER ACCRETION/EJECTION FLOW Margherita Margherita Giustini - Ph.D. Giustini, Thesis defense, 16/05/2011 Bologna 15/04/2011

28 Superwinds

29

30 M82

31

32

33 20% of massive star formation at low z in starbursts Starburst/superwind galaxies account for most star formation at 2<z<4 ULIRGS have BALS and Superwind (Mdot~1000 Msun/yr, v~1000km/s) eg Mkn 231

34 Summary Athena will give crucial information on gas velocity, metallicity, ionization and emission measure for all forms of galaxy feedback X-rays are the only probe of volume-filling component

35

36

37 Strawman for Feedback science case vs A1/2/3 Nearby cool cores Sources <F 2-10keV > # <Exp.> (ks) Tot. Exp. (Ms) Doable? A1, A2, A3? clusters few 1e A1, A2, A3 Nearby groups groups few 1e A1, A2, A3 Bad Med Best Distant (z<0.3) cool cores clusters few 1e A1, A2, A3 Outflows (dynamics) Outflows (feedback) Sey/PGs/ RGs >1e A1, A2, A3 PGs/QSOs >1e A1, A2, A3 Total N.B: Already makes use of targets and observations needed for Strong Gravity Strawman

38 Where we stand now (after Chandra and XMM-Newton): ~20 well-studied sources t=4 years t=6 months t=3 days t=10 ks Strong spectral variability, complex and variable ionized absorbers

39 The FOM for AGN feedback is the absorption line sensitivity (EW=50 ev, 100 ks, 5sigma) XMS Athena3 is preferred for outflows dynamics Athena1 is preferred for cosmological feedback

40 A2 XMS A3 XMS XMM pn Astro-H

41 Centaurus - detailed soft spectra Astro-H limits are 0.55, 0.76 and 2 Msun/yr in 50 ks

42 Absorption spectroscopy with calorimeter resolution between 2-7 kev will allow to constrain absorbers in a sample of QSOs up to z=2 Flux limits to measure (N w, ) within (10%, 5%) in 100 ks obs. Important to probe AGN feedback up to z~2