Metal enrichment processes in the intra-cluster medium

Schindler, S.; Kapferer, W.; Domainko, W.; Mair, M.; Kampen, E. van; Kronberger, T.; Kimeswenger, S.; Ruffert, M.; Mangete, O M; Breitschwerdt, D.

doi:10.1051/0004-6361:200500107

Cited by 82 publications

(93 citation statements)

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These maps show clearly a non-uniform and nonspherical distribution of the metals, which agrees with the results of simulations (e.g. Schindler et al 2005). Recent observations also shed some light on the redshift evolution of the metallicity.…”

Section: Introductionsupporting

confidence: 90%

Metal enrichment of the intra-cluster medium by thermally and cosmic-ray driven galactic winds

Kapferer¹,

Kronberger²,

Breitschwerdt

et al. 2009

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We investigate the efficiency and time-dependence of thermally and cosmic ray driven galactic winds for the metal enrichment of the intra-cluster medium (ICM) using a new analytical approximation for the mass outflow. The spatial distribution of the metals are studied using radial metallicity profiles and 2D metallicity maps of the model clusters as they would be observed by X-ray telescopes like XMM-Newton. Methods. Analytical approximations for the mass loss by galactic winds driven by thermal and cosmic ray pressure are derived from the Bernoulli equation and implemented in combined N-body/hydrodynamic cosmological simulations with a semi-analytical galaxy formation model. Observable quantities like the mean metallicity, metallicity profiles, and 2D metal maps of the model clusters are derived from the simulations. Results. We find that galactic winds alone cannot account for the observed metallicity of the ICM. At redshift z = 0 the model clusters have metallicities originating from galactic winds which are almost a factor of 10 lower than the observed values. For massive, relaxed clusters we find, as in previous studies, a central drop in the metallicity due to a suppression of the galactic winds by the pressure of the ambient ICM. Combining ram-pressure stripping and galactic winds we find radial metallicity profiles of the model clusters which agree qualitatively with observed profiles. Only in the inner parts of massive clusters the observed profiles are steeper than in the simulations. Also the combination of galactic winds and ram-pressure stripping yields too low values for the ICM metallicities. The slope of the redshift evolution of the mean metallicity in the simulations agrees reasonably well with recent observations.

show abstract

Section: Introductionsupporting

confidence: 90%

Metal enrichment of the intra-cluster medium by thermally and cosmic-ray driven galactic winds

Kapferer¹,

Kronberger²,

Breitschwerdt

et al. 2009

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…In Table 3 ICM of galaxy clusters, which is of the order of 10 10−12 M iron mass (Arnaud et al 1992). Taking all model assumptions into account we can conclude that SN Ia events in the ICSP are a less important enrichment mechanism compared to outflows by galactic winds and ram-pressure stripping (Domainko et al 2007;Kapferer et al 2007Schindler et al 2005;Tornatore et al 2007). …”

Section: The Sn Ia Rate In the Icsp/igspmentioning

confidence: 97%

The evolution of an intra-cluster and intra-group stellar population

Kapferer¹,

Schindler²,

Knollmann

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We investigate the properties of an intra-cluster stellar population (ICSP) and an intra-group stellar population (IGSP) as a function of time. We apply different criteria to separate between the stellar components residing in the galaxies and in the intergalactic spaces. In addition we investigate the rate of SNIa events in the ICSP/IGSP and the amount of 56 Fe produced by these events. Finally we compare the dynamics of the ICSP/IGSP with the stellar component residing in the galaxies. Methods. By applying a combined N-body/hydrodynamic description (GADGET-2) with radiative cooling and a recipe for star formation and stellar feedback two different sized systems were calculated, i.e. galaxy cluster and galaxy groups. From these simulations extended halo catalogues were extracted with AHF: Amiga's Halo Finder. Together with the full information of all particles in the simulation several separation criteria between the ICSP/IGSP and the stellar component in the galaxies were investigated in detail. Results. Applying different criteria to distinguish the stellar components inside and outside clusters/groups reveals different amounts of stellar mass present in the ICSP. We find that 7% to 40% of all stars belong to the ICSP in the galaxy cluster simulation depending on the applied separation criteria at redshift z = 0. The same separation criteria applied on a group simulation results in a 3% to 30% IGSP component compared to the total stellar mass in the system at redshift z = 0. Our investigation reveals a major difference between the gradient in the evolution of the ICSP and IGSP; the stellar mass present in the ICSP is increasing, whereas the fraction of stellar mass in the IGSP is decreasing in the same redshift regime. Applying simple SNIa rate estimates yields SNIa rates for the ICSP/IGSP of the order of 0.05 SNIa events per year in the ICSP and one order of magnitude lower for the IGSP, reflecting the different stellar masses in the ICSP/IGSP. The amount of 56 Fe-mass produced by the ICSP/IGSP SNIa is nearly two orders of magnitudes lower than observed values. The mean age of the stellar component populating the ICSP/IGSP is younger than the mean age of the stellar component in the galaxies. The maximum in the velocity distribution of the ICSP is shifted to lower velocities compared to the maximum in the velocity distribution of the stellar component in the galaxy cluster simulation. This reflects the high galaxy interaction rate present in the galaxy clusters. The difference gives us a measure for the dynamical state of the galaxy cluster/group.

show abstract

“…In our model this translates into a combined pressure of gas, cosmic rays and MHD waves, which is lower at the sonic point than the external ICM pressure. In addition to the quiescent winds, calculated in Schindler et al (2005), we take into account starbursts caused by galaxy-galaxy interactions in this simulation. These interactions enhance the SFRs of the systems very strongly over short times (several 10 to 100 Myr, Kapferer et al 2005) and therefore lead to short, strong outflows of matter.…”

Section: X-ray Metal Mapsmentioning

confidence: 99%

“…Gnedin (1998) did combined softened lagrangian hydrodynamic (SLH) particle-particle/particle-mesh (P 3 M) simulations to investigate the contribution of galaxy-interactions on the enrichment of the ICM. A comparison of the efficiency between rampressure stripping and quiet galactic winds was recently done by Schindler et al (2005).…”

Section: Introductionmentioning

confidence: 99%

Simulations of galactic winds and starbursts in galaxy clusters

Kapferer¹,

Ferrari²,

Domainko³

et al. 2006

A&A

Self Cite

View full text Add to dashboard Cite

We present an investigation of the metal enrichment of the intra-cluster medium (ICM) by galactic winds and merger-driven starbursts. We use combined N-body/hydrodynamic simulations with a semi-numerical galaxy formation model. The mass loss by galactic winds is obtained by calculating transonic solutions of steady state outflows, driven by thermal, cosmic ray and MHD wave pressure. The inhomogeneities in the metal distribution caused by these processes are an ideal tool to reveal the dynamical state of a galaxy cluster. We present surface brightness, X-ray emission weighted temperature and metal maps of our model clusters as they would be observed by X-ray telescopes like XMM-Newton. We show that X-ray weighted metal maps distinguish between pre-or post-merger galaxy clusters by comparing the metallicity distribution with the galaxy-density distribution: pre-mergers have a metallicity gap between the subclusters, post-mergers a high metallicity between subclusters. We apply our approach to two observed galaxy clusters, Abell 3528 and Abell 3921, to show whether they are pre-or post-merging systems. The survival time of the inhomogeneities in the metallicity distribution found in our simulations is up to several Gyr. We show that galactic winds and merger-driven starbursts enrich the ICM very efficiently after z = 1 in the central (∼3 Mpc radius) region of a galaxy cluster.

show abstract

Metal enrichment processes in the intra-cluster medium

Cited by 82 publications

References 25 publications

Metal enrichment of the intra-cluster medium by thermally and cosmic-ray driven galactic winds

Metal enrichment of the intra-cluster medium by thermally and cosmic-ray driven galactic winds

The evolution of an intra-cluster and intra-group stellar population

Simulations of galactic winds and starbursts in galaxy clusters

Contact Info

Product

Resources

About