Feedback and enrichment from SNR to LSS

1. Feedback and enrichment from SNR to LSS Jelle S. Kaastra SRON

2. The importance of feedback in astrophysics

3. Earth versus solar system Earth Solar system

4. Which elements can we see? K-shell

5. Which elements will we see?(IXO) K-shell

6. First step feedback: Nucleosynthesis

7. Intermediate mass stars • Stars < 8 Msun in late stages produce much C and N through nuclear fusion • strong winds blow elements away • Finally, core collapses to white dwarf and planetary nebula is ejected

8. X-ray spectrum planetary nebula(Yu et al. 2009) Ne O C

9. Type Ia supernova remnants • Metals are ejected into the interstellar medium • Mainly heavier elements (Si, Fe, Ni) • Example: Cassiopeia B (better known as Tycho, remnant of SN that exploded 1572)

10. Core collapse remnants • Metals are ejected into the interstellar medium • Mainly lighter elements (O, Ne, Si) • During explosion also nucleosynthesis of heavier metals (up to U) • Example: Cassiopeia A (remnant of SN that exploded ca. 1680) All X-rays Si Ca Fe

11. Enrichment in clusters of galaxies

12. Importance clusters of galaxies for abundance studies • Largest bound structures • Fair samples of the Universe • Deep potential wells, retains most of the gas • Hot gas: no significant “hiding” of metals in dust (& more gas than stars) • Spatial extent allows mapping

15. Cr, Mn(cf. Badenes et al. 2008)

16. Simulations • Sample: extended HIFLUCS sample 106 clusters (Reiprich & Böhringer) • Use T & n profiles • Fit multi-T model • Spectra r<0.2R500

17. Simulations: 10 best cases • Sample: 10th best in 100 ks • WFI: errorsdominatedbysystematics, equalto XMM/EPIC! • NEED High-res! • XMS: unambiguousdetectionall C-Zn (inc. Scandium) • Maps: 0.01 solar in coreforall elements nowdetectedwith XMM

18. Circulation of the elements in clusters of galaxies

19. How to get metals in custers?Ram pressure stripping • Ram pressure stripping mostly in cluster cores

20. Galactic winds • Massive stars born in groups • Sometimes many SN explosions in relatively short time • Combined power may blow gas out of galaxies M 82, optical M 82, X-ray

21. Galaxy-Galaxy interactions • Close encounters may cause tidal tails • Stars and gas torn away from galaxies • Enriched gas enters intergalactic space Antennae (Sky & Telescope)

22. Sloshing central galaxy: cosmic mixer(de Plaa et al. 2010)

23. Giant outflows from active galaxies • In compact clusters like M87, radio lobes show cool, enriched material levitated by the AGN outflow X-ray Radio

24. Uplift of enrichedmaterial in M87/Virgo(Simionescu et al. 2008) • Currently only maps in Fe • Need mapping in more elements to reconstruct the source of the metals

25. Need for mapping different elements • White contours: ram-pressure stripping • Black contours: galactic winds • (after Schindler & Diaferio 2008)

26. AGN outflows

27. Importance of AGN outflows(adapted from talk Jerry Kriss @ Utrecht conference) • May affect dispersal heavy elements into IGM & ICM (e.g. Cavaliere et al. 2002; Scannapieco & Oh 2004) • Influence ionisation structure IGM (Kriss et al. 1997) • Intertwined with evolution host galaxy (e.g. Silk & Rees 1998; Wyithe & Loeb 2003) • Not sure about how outflows created, their structure, mass & energy: key question: do outflows escape confines of host galaxy? • Crucial to understand working central engine: central engine, energy budget • Low-z AGN are the nearest & brightest, so best objects to study

28. Complex velocity structure • Example: STIS spectra NGC 5548 (Crenshaw & Kraemer 1999) show 5 velocity components: • Nr 1 high -1040 km/s • Nr 2 med -667 km/s • Nr 3 med -530 km/s • Nr 4 med -336 km/s • Nr 5 low -160 km/s Radial velocity (km/s)

29. Complex ionisation structure • Gas at multiple ionisation parameters • Hot debate: continuous distribution, or multiple (2 or 3) discrete components in pressure equilibrium? Steenbrugge et al. 2005

30. Mass loss through the wind

31. Mrk 509 campaign • 600 ks RGS+EPIC+OM XMM-Newton = 10 x 60 ks, 4 days spacing • Simultaneous Integral, 1.2 Ms • Chandra LETGS 170 ks + HST/COS spectra • Swift monitoring in between & before • Optical/IR coverage WHT & Pairitel • One of biggest campaigns on AGN ever

32. 600 ks RGS (= 6 ks IXO)

33. Discrete versus continuous absorption measure distribution? • Column densities well approximated by sum 5 components • Higher column for higher ionisation parameter • But what about a continuous model?

34. Continuous model(Detmers et al. 2011) • Fitted columns with continuous (spline) model • Surprise comps C & D pop-up as discrete components! • Upper limits FWHM 35 & 80 % • Component B (& A) too poor statistics to prove if continuous • Component E also poorer determined: correlation ξ and NH. D E C B

35. Ionisation equilibrium E D C B A

36. Abundances AGN • AGN outflows have chemical composition core galaxy (modified by AGN environment, star formation?) • Hard to measure in emission (systematics, multi-region, etc.) • Mrk 509 results (Steenbrugge et al. 2011): accurate (down to 5 %) abundances of C, N, O, Ne, Mg, Fe

37. Prospects IXO • Gratings: area & resolution 10 x RGS •  600 ks RGS is 6 ks IXO for weak lines •  time-resolved spectroscopy, excellent velocity separation (100 km/s) • XMS: area 100 x RGS, resolution ~ RGS •  600 ks RGS is 6 ks IXO for weak lines •  time-resolved spectroscopy

38. Conclusions • Feedback & chemical enrichment can be studied on all scales with IXO • High-resolution X-ray spectroscopy is the key to all the answers • Let's make that key!