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What IGM knows about the star-formation... An X-ray perspective.

What IGM knows about the star-formation... An X-ray perspective. Bookkeeping of energy and metal ejection IMF+AGN-cooling Tracing the LSS Role of clusters in the chemical evolution of the Universe. A. Finoguenov (MPE). Studying the Cosmic Galaxy and Star Formation History. Protocluster

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What IGM knows about the star-formation... An X-ray perspective.

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

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

  3. Star formation rate

  4. Ponman, Sanderson, Finoguenov 2003 Modified scaling: S~T 0.65 Alexis Finoguenov

  5. local groups local clusters Clusters@z=0.3 ! !

  6. Alexis Finoguenov

  7. Alexis Finoguenov

  8. Turbulence Alexis Finoguenov

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

  10. AGN feedback Z=0 Z=2 Alexis Finoguenov

  11. Feedback exceeding cooling threshold Z=0 Z=2 Alexis Finoguenov

  12. ! ! ! Alexis Finoguenov

  13. Reproduction of scaling in simulations with galactic wind ! 800 km/s 300 km/s 800 km/s 300 km/s Alexis Finoguenov

  14. HCG 90 S Alexis Finoguenov Trinchieri et al. 2003 R

  15. Finding groups at high z: status report Alexis Finoguenov

  16. eLH Alexis Finoguenov

  17. eCDFS Alexis Finoguenov

  18. Prob. of halo mass structures vs field size cosmos ==> > 1 deg to sample all structures Alexis Finoguenov

  19. Cosmos Survey 2qdegrees Alexis Finoguenov

  20. Most of the structure shows up in XMM images Alexis Finoguenov

  21. Median z

  22. Median z

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

  24. Diffusesources

  25. GalaxiesvsX-rays

  26. GalaxiesvsX-rays and Weak lensing Alexis Finoguenov

  27. Z ~ 0.73 cluster : DM lensing & X-ray Alexis Finoguenov

  28. COSMOS : environment <==> evolution luminous early-type ==> dense core of LSS Alexis Finoguenov

  29. Galaxy groups w/ XMM at z > 0.5 (h) and z<0.5 (l) : ACS images Alexis Finoguenov

  30. ABC of Metals in clusters: distribution Alexis Finoguenov

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

  32. Radial Abundance Variations of Fe and Si in Various Clusters and Groups • The 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 ! SN II [Si/Fe] SN Ia Finoguenov et al. 2000 Alexis Finoguenov

  33. A 3667:Metallicity vs entropy Alexis Finoguenov

  34. Metals in clusters:sources Alexis Finoguenov

  35. 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

  36. O & Si Abundance Profiles in M87 O Si Si 2-temp 1-temp 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) Matsushita, Finoguenov, Böhringer 2002

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

  38. Two types of SN as ICM Poluters SN Type II M* > 8 Msun SN Type Ia Fe- group elements dominate a- elements dominate

  39. Decomposition of the Metal Abundances into Contributions from SN Ia and SN II SN Ia SN II Inner region Outer region Finoguenov, Matsushita, Böhringer et al. 2002 A&A 381, 21 Alexis Finoguenov

  40. 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 a-elements • Second order effect: there may be a variation in the types of SN Ia (later SN Ia show on average more a-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 Alexis Finoguenov

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

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

  43. Galaxy Population and Environment Clusters accumulate the products of early star formation Kodama et al. 2001 Alexis Finoguenov

  44. 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 Alexis Finoguenov

  45. Mass-to-light ratios Alexis Finoguenov

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

  47. Metal Budget @Z=0 Alexis Finoguenov

  48. Coma outskirts Finoguenov, Briel, Henry 2003 Alexis Finoguenov

  49. 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. Alexis Finoguenov

  50. 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) Alexis Finoguenov

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