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Metal Enrichment Processes

Metal Enrichment Processes. Sabine Schindler University of Innsbruck. With XMM observations it is now possible to determine not only the metallicity (Fe abundance) of a cluster or the metallicity profile, but a 2D metallicity map. red – high metallicity blue - low metallicity.

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Metal Enrichment Processes

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  1. Metal Enrichment Processes Sabine Schindler University of Innsbruck

  2. With XMM observations it is now possible to determine not only the metallicity (Fe abundance) of a cluster or the metallicity profile, but a2D metallicity map

  3. red – high metallicity blue - low metallicity Metallicity mapsLovisari et al., subm. A496 A2029 Centaurus Hydra A A2319 Sersic 159-03

  4. red – high metallicity blue - low metallicity Metallicity mapsLovisari et al., subm. A496 A2029 Centaurus Even for relaxed clusters the metal distribution is non-spherical very inhomogeneous Hydra A A2319 Sersic 159-03

  5. red – high metallicity blue - low metallicity Metallicity mapsLovisari et al., subm. A496 A2029 Centaurus Metal mass:determined with the 2D metal maps the metal mass is up to a factor 2 higher than determined by a single metallicity value so far metal masses have been underestimated (see predictions by simulations, Kapferer et al. 2007) Hydra A A2319 Sersic 159-03

  6. Radial profiles of different elements • Contribution SNII / SNIa decreases towards centre • Fraction SNII/ SNIa ~ 65-80% Lovisari et al., subm. O/Fe Si/Fe

  7. Where do the metals come from?What processes are responsible? Complex mixture of processes Simulations required

  8. http://astro.uibk.ac.at/astroneu/hydroskiteam/index.htm Simulation

  9. Metal enrichment Many different scales involved Simulations • on galaxy scales • on cluster scales

  10. Galaxy scales…

  11. Ram-pressure stripping is an important process in clusters • More and more observational evidence for ram-pressure stripping…. Crowl et al. 2006

  12. Film1 Kronberger et al. 2008

  13. Results • star formation is increased significantly by ram-pressure stripping (up to a factor of 10) • stars form in the central compressed region and in the stripped gas behind the galaxy  intra-cluster stellar population • stars fall back onto and through disc  different morphology Kronberger et al. 2008Kapferer et al. 2008

  14. Evidence for star formation in stripped gas Blue knots behind a galaxy in the Coma cluster Star formation in the wake of ESO137-001 in A3627 Yoshida et al. 2008 red: CHANDRA contours blue & cyan: star forming regions Tail of star formation trailing IC3418 in Virgo Sun et al. 2007 A3627: ESO137-001 Hester et al. 2010

  15. Ram pressure stripping is also important in collisions within clusters…. Film2 Kapferer et al. 2008

  16. Systematic study of ram-pressure stripping varying • surrounding gas density • relative velocity gas density stellar surface brightness log scale v = 500 km/s ρ = 5 10-27 g/cm3 t = 500 Myrs Kapferer et al. 2009

  17. Results • even ram-pressure in the outskirts of clusters is sufficient to strip gas and form new stars • up to 95% of newly formed stars can be in the wake Kapferer et al. 2009

  18. simulated observations Kapferer et al. 2009

  19. Simulations on cluster scales… Density and temperature Density and metalliticy Ram-pressure stripping – galactic winds Ram-pressure stripping – galactic winds (X-ray)

  20. Results: • inhomogeneous metal distribution • enriched gas is not mixed immediately with the ICM simulation observed metallicity map Lovisari et al. 2009

  21. Comparison of ram-pressure stripping and galactic winds Kapferer et al. 2007 Movie1 Movie2 mass loss profile redshift

  22. Comparison Winds – Ram-Pressure Stripping • Distribution of Metals Galactic winds extended distribution Ram-pressure stripping centrally concentrated distribution • Efficiency Galactic winds are more efficient in earlier epochs Ram-pressure stripping is more efficient after z=1-2 • Amount of Metals Ram-pressure stripping can produce considerably more metals than galactic winds (depending on cluster mass and other cluster properties) Schindler et al. 2005, Kapferer et al. 2007, 2009

  23. Summary • different processes contribute to the metallicity (not just a single process, but ram-pressure stripping is very important), they yield different metal distributions and have different time scales • ram-pressure in the outskirts of clusters is sufficient to strip gas and form new stars • inhomogeneous metallicity distribution, enriched material is not mixed immediately with ICM • metal mass from X-ray observations is considerably underestimated due to inhomogeneous metal distribution • ram-pressure stripping leads to enhanced star formation, star formation also behind the galaxy  intra-cluster stars Schindler et al. 2005, Kapferer et al. 2005, Kapferer et al. 2006, Domainko et al. 2006, Kapferer et al. 2007a,b, Kronberger et al.2008, Kapferer et al. 2008, 2009, 2010, Lovisari et al. 2009, Lovisari et al., subm.

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