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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 Centaurus Metallicity maps Sersic 159-03 Lovisari et al., subm. A496 A2029 Hydra A A2319 red – high metallicity blue - low metallicity Centaurus Metallicity maps A496 Lovisari et al., subm. A2029 Even for relaxed clusters the metal distribution is non-spherical very inhomogeneous Sersic 159-03 Hydra A A2319 red – high metallicity blue - low metallicity Centaurus Metallicity maps A496 Lovisari et al., subm. A2029 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 Hydra A (see predictions by simulations, Kapferer et al. 2007) Sersic 159-03 A2319 Radial profiles of different elements • Contribution SNII / SNIa decreases towards centre • Fraction SNII/ SNIa ~ 65-80% Lovisari et al., subm. O/Fe Si/Fe Where do the metals come from? What processes are responsible? Complex mixture of processes Simulations required Stefanie Unterguggenberger Markus Heider Wolfgang Kapferer Sabine Schindler Thomas Kronberger Eelco van Kampen Lorenzo Lovisari Thomas Kronberger Magda Mair Chiara Ferrari Emanuela Orrú Martin Pančišin Julia Weratschnig Sabine Schindler Magda Mair Josef Stoeckl Wolfgang Kapferer Julia Weratschnig http://astro.uibk.ac.at/astroneu/hydroskiteam/index.htm Simulation Metal enrichment Many different scales involved Simulations on galaxy scales on cluster scales Galaxy scales… Ram-pressure stripping is an important process in clusters • More and more observational evidence for ram-pressure stripping…. Crowl et al. 2006 Film1 Kronberger et al. 2008 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. 2008 Kapferer et al. 2008 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 Sun et al. 2007 A3627: ESO137-001 Hester et al. 2010 Tail of star formation trailing IC3418 in Virgo Ram pressure stripping is also important in collisions within clusters…. Film2 Kapferer et al. 2008 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 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 simulated observations Kapferer et al. 2009 Simulations on cluster scales… Density and temperature Density and metalliticy Ram-pressure stripping – galactic winds Ram-pressure stripping – galactic winds (X-ray) Results: simulation inhomogeneous metal distribution enriched gas is not mixed immediately with the ICM observed metallicity map Lovisari et al. 2009 Comparison of ram-pressure stripping and galactic winds Kapferer et al. 2007 Movie1 mass loss redshift Movie2 profile 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 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.