2. X-IGM vs starformation Alexis Finoguenov What IGM knows about the star-formation... An X-ray perspective. A. Finoguenov (MPE) Bookkeeping of energy and metal ejection IMF+AGN-cooling Tracing the LSS Role of clusters in the chemical evolution of the Universe

3. Studying the Cosmic Galaxy and Star Formation History galaxy population Protocluster star bursts at z ~ 3 - 7 Cluster early type galaxies at z ~ 0 (with a very old stellar population) Fe Si entropy

4. Star formation rate

5. X-IGM vs starformation Alexis Finoguenov Ponman, Sanderson, Finoguenov 2003 0.65 Modified scaling: S~T

6. local groupslocal clustersClusters@z=0.3 ! !

7. X-IGM vs starformation Alexis Finoguenov

8. X-IGM vs starformation Alexis Finoguenov

9. X-IGM vs starformation Alexis Finoguenov Turbulence

10. Star-formation feedback Z=0Z=2 Borgani, AF, Kay, Ponman, Springel, Tozzi, Voit

11. X-IGM vs starformation Alexis Finoguenov AGN feedback Z=0Z=2

12. X-IGM vs starformation Alexis Finoguenov Feedback exceeding cooling threshold Z=0Z=2

13. X-IGM vs starformation Alexis Finoguenov ! ! !

14. X-IGM vs starformation Alexis Finoguenov Reproduction of scaling in simulations with galactic wind 300 km/s 800 km/s 300 km/s !

15. X-IGM vs starformation Alexis Finoguenov S R HCG 90 Trinchieri et al. 2003

16. X-IGM vs starformation Alexis Finoguenov Finding groups at high z: status report

17. X-IGM vs starformation Alexis Finoguenov eLH

18. X-IGM vs starformation Alexis Finoguenov eCDFS

19. X-IGM vs starformation Alexis Finoguenov Prob. of halo mass structures vs field size cosmos ==> > 1 deg to sample all structures

20. X-IGM vs starformation Alexis Finoguenov Cosmos Survey 2 q  degrees

21. X-IGM vs starformation Alexis Finoguenov Most of the structure shows up in XMM images in XMM images

22. Median zMedian z

23. Median zMedian z

24. XMM red -- 0.5-2 kev green -- 2-4.5 kev blue -- 4.5- 10kev 1000 sources detected

25. DiffusesourcesDiffusesources

26. Galaxies vs X-rays

27. X-IGM vs starformation Alexis Finoguenov Galaxies vs X-rays and Weak lensing

28. X-IGM vs starformation Alexis Finoguenov Z ~ 0.73 cluster : DM lensing & X-ray

29. X-IGM vs starformation Alexis Finoguenov luminous early-type ==> dense core of LSS COSMOS : environment evolution

30. X-IGM vs starformation Alexis Finoguenov Galaxy groups w/ XMM at z > 0.5 (h) and z<0.5 (l) : ACS images

31. X-IGM vs starformation Alexis Finoguenov ABC of Metals in clusters: distribution

32. X-IGM vs starformation Alexis Finoguenov Abundance Gradients (Beppo-SAX) Metallicity Gradients in non-cooling flow clusters and cooling flow clusters [DeGrandi & Molendi 2001] - these metallicity measurements refer essentially to the Fe abundance ! Clusters without cooling flows Clusters with cooling flows

33. X-IGM vs starformation Alexis Finoguenov Finoguenov et al. 2000 The central enhancement is more enriched by SN Ia than the outer parts of the ICMThe central enhancement is more enriched by SN Ia than the outer parts of the ICM In the outer regions the metals in the ICM are dominated by the contribution from SN II ! In the outer regions the metals in the ICM are dominated by the contribution from SN II ! SN Ia SN II [Si/Fe] Radial Abundance Variations of Fe and Si in Various Clusters and Groups

34. X-IGM vs starformation Alexis Finoguenov A 3667: Metallicity vs entropy

35. X-IGM vs starformation Alexis Finoguenov Metals in clusters: sources

36. XMM Observations of the X-ray Halo of M87 Böhringer et al. 2001, 2002 Matsushita et al. 2002a, b Finoguenov et al. 2002 Sakelliou et al. 2002

37. O & Si Abundance Profiles in M87 The O profile is almost flat (consistent with a flat profile within +- 10 %) The O/Si ratio increases from about 0.4 to 0.7 (from r = 2 – 50 kpc) - (using MEKAL models) Si 1-temp O Si Matsushita, Finoguenov, Böhringer 2002 2-temp

38. X-IGM vs starformation Alexis Finoguenov Metal Abundances in M87 1´ - 3´ 8´ - 16´ Radial Zones : Metals normalized to solar abundances Finoguenov, Matsushita, Böhringer, Ikebe, Arnaud 2002

39. Two types of SN as ICM Poluters SN Type II M * > 8 M sun SN Type Ia Fe- group elements dominate  - elements dominate

40. X-IGM vs starformation Alexis Finoguenov Decomposition of the Metal Abundances into Contributions from SN Ia and SN II SN IaSN II Finoguenov, Matsushita, Böhringer et al. 2002 A&A 381, 21 Inner region Outer region

41. X-IGM vs starformation Alexis Finoguenov Conclusion from the Abundance Pattern Most of the Fe in the center comes from SN Ia -- This Fe can be produced by SN Ia from M87 within the last 1 - 2 Gyr (with a Cappelaro rate of SN in early type galaxies) The abundance pattern clearly favor slow deflagration/detonation models – with incomplete burning of the  -elements Second order effect: there may be a variation in the types of SN Ia (later SN Ia show on average more  -elements -- slower explosions) The total Fe contribution by SN II falls about a factor of 1.5-2 short in explaining the wide-spread Fe abundance with classical IMF models  we can test chemical evolution parameters  we can test SN-nucleosynthesis models

42. Information on the Star Formation Rate in Cluster Early-Type Galaxies bluer brighter [Bender et al. ‘98] [Bender & Ziegler ‘97] Ellis et al. ‘97 Fundamental plane

43. Information on the Star Formation Rate in Cluster Early-Type Galaxies bluer brighter [Bender et al. ‘98] [Bender & Ziegler ‘97] Ellis et al. ‘97 Ellipticals snd S0s in distant clusters are somewhat brighter and bluer than nearby – consistent with passive evolution ! Most star formation at z>3 !! Fundamental plane

44. X-IGM vs starformation Alexis Finoguenov Galaxy Population and Environment Kodama et al. 2001 Clusters accumulate the products of early star formation

45. X-IGM vs starformation Alexis Finoguenov Observational aspects of stellar IMF mass function of stars Stellar mass-to-light ratio and ist evolution High-mass to intermediate mass star ratio Metal production per unit of remaining stellar light Weighting among massive stars

46. X-IGM vs starformation Alexis Finoguenov Mass-to-light ratios

47. X-IGM vs starformation Alexis Finoguenov Larson IMF in clusters and metal-poor stars Padoan IMF AF, Burkert, Böhringer 2003 Hernandez, Ferrara 2002 Z production weighting

48. X-IGM vs starformation Alexis Finoguenov Metal Budget @Z=0

49. X-IGM vs starformation Alexis Finoguenov Coma outskirts Finoguenov, Briel, Henry 2003

50. X-IGM vs starformation Alexis Finoguenov Summary Fossil records study consistently require both strong feedback and top heavy IMF at high-z Protoclusters are sights of missing metals at high-z, which are at high temperatures Feedback energy, released at high-z, appears to cool down by now. Observations of groups support AGNs as a dominant source of feedback. Current deep surveys are capable of finding and study groups at high-z.

51. X-IGM vs starformation Alexis Finoguenov Coauthors H.Böhringer, P.Schuecker, M.Zimer, Y.Zhang, G. Hasinger (MPE) A.Burkert (LMU) T. Ponman, J. Osmond (Bham) S. Borgani, L. Tornatore (Trieste) V. Springel (MPA) M. Voit P.Rosati (ESO)

52. Roberto Abraham Masaru Ajiki Justin Alpert Herve Aussel Josh Barnes Andrew Blain Daniela Calzetti Peter Capak John Carlstrom Chris Carilli Andrea Cimatti Andrea Comastri Marcella Corollo Emannuel Daddi Richard Ellis Martin Elvis Amr El Zant Shawn Ewald Mike Fall Alexis Finoguenov Alberto Franceschini Mauro Giavalisco Richard Griffiths Gigi Guzzo Gunther Hasinger Chris Impey Jean-Paul Kneib Karel Nel Jin Koda Anton Koekemoer Alexie Leauthaud Olivier LeFevre Ingo Lehmann Simon Lilly Thorsten Lisker Charles Liu Richard Massey Henry McCracken Yannick Mellier Satoshi Miyazaki Bahram Mobasher Takashi Murayama Colin Norman Alexandre Refregier Alvio Renzini Jason Rhodes Mike Rich Dave Sanders Shunji Sasaki Dave Schminovich Eva Schinnerer Nick Scoville Marco Scodeggio Kartik Sheth Patrick Shopbell James Taylor Dave Thompson Neil Tyson Meg Urry Yoshi Taniguchi Ludovic Van Waerbeke Paolo Vettolani Simon White Lin Yan COSMOS -- team & collaborators

53. X-IGM vs starformation Alexis Finoguenov Thank you!