SNe heating and the chemical evolution of the intra-cluster medium

Pipino, A.; Matteuccí, F.; Borgani, S.; Biviano, A.

doi:10.1016/s1384-1076(02)00136-7

Cited by 78 publications

(137 citation statements)

References 74 publications

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“…These results suggest that so far the enrichment of the ICM is mainly due to SN II. We note that Pipino et al (2002) using different chemical evolution models for galaxies, showed that SN II dominate the chemical enrichment inside the galaxies, while Ia supernovae play a predominant role in the ICM, that is not in agreement with the observational results.…”

Section: Sn Enrichmentcontrasting

confidence: 87%

Metallicity map of the galaxy cluster A3667

Lovisari¹,

Kapferer²,

Schindler³

et al. 2009

A&A

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We use XMM-Newtondata of the merging cluster Abell 3667 to analyze its metallicity distribution. A detailed abundance map of the central 1.1 × 1.1 Mpc region indicates that metals are inhomogeneously distributed in the cluster showing a non-uniform and very complex metal pattern. The highest peak in the map corresponds to a cold region, slightly offset South of the X-ray center. This could be interpreted as stripped gas due to a merger between a group moving from NW towards the SE and the main cluster. We note several clumps of high metallicity also in the opposite direction with respect to the X-ray peak. Furthermore we determined abundances for 5 elements (O, Si, S, Ar, Fe) in four different regions of the cluster. Comparisons between these observed abundances and theoretical supernovae yields allow to get constraints on the relative number of SN Ia and II contributing to the enrichment of the intra-cluster medium. To reproduce the observed abundances of the best determined elements (Fe, O and Si) in a region of 7 around the X-ray center, 65-80% of SN II are needed. The comparison between the metal map, a galaxy density map obtained using 550 spectroscopically confirmed cluster members and, our simulations suggest a recent merger between the main cluster and the group in the SE.

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Section: Sn Enrichmentcontrasting

confidence: 87%

Metallicity map of the galaxy cluster A3667

Lovisari¹,

Kapferer²,

Schindler³

et al. 2009

A&A

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“…This model is an updated version of the multizone model of Martinelli et al (1998) and Pipino et al (2002). In the model the ellipticals form by fast accretion of gas at high redshift, and the infall law is calibrated to obtain, in the absence of galactic winds, a luminous mass of roughly 10 11 M (1.32 × 10 11 in Table 1).…”

Section: Chemical Evolutionmentioning

confidence: 99%

Cosmological formation and chemical evolution of an elliptical galaxy

Colavitti

Pipino

Matteuccí

2009

A&A

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Aims. We aim to study the effect of a cosmologically motivated gas infall law for the formation of a massive elliptical galaxy in order to understand its impact on the formation of spheroids. Methods. We replace the empirical infall law of the model by Pipino & Matteucci with a cosmologically derived infall law for the formation of an elliptical galaxy. We compare our predictions with observations. We also compare the obtained results with those of Pipino & Matteucci.Results. We computed models with and without galactic winds; we found that models without wind predict a too large current SNIa rate. In particular, the cosmological model produces a current SNIa value which is about ten times higher than the observed values. Moreover models without wind predict a high current SNII rate, too large even if compared with the recent GALEX data. The predicted SNII rate for the model with wind, on the other hand, is too low if compared with the star formation histories given by GALEX. The mean value for the [Mg/Fe] ratio in the dominant stellar population of the simulated galaxy, as predicted by the cosmological model, is too low if compared to observations. This is a very important result indicating that the cosmological infall law is in contradiction to the chemical evolution. Conclusions. A cosmologically derived infall law for an elliptical galaxy cannot reproduce all the chemical constraints given by observations. The problem resides in the fact that the cosmologically derived infall law implies a slow gas accretion with a consequent star formation rate active for a long period. In this situation low [Mg/Fe] ratios are produced for the dominant stellar population in a typical elliptical, at variance with observations.

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“…This occurs because the degree of α-enhancement depends on the timescale of the Fe released by type Ia SNe relative to the timescale of star formation (see Matteucci & Recchi 2001). Good models of chemical evolution for elliptical galaxies predict that the star formation timescale was shorter in more massive objects, in order to reproduce the observed increase of the [α/Fe] ratio in the dominant stellar population as a function of galactic mass (Matteucci 1994;Pipino et al 2002;Pipino & Matteucci 2004;Romano et al 2003). This implies that galactic winds should occur first in massive objects, thus interrupting the star formation process.…”

Section: Abundances In the Icmmentioning

confidence: 99%

Interpretation of Abundance Ratios

Matteuccí¹,

Chiappini

2005

Publ. Astron. Soc. Aust

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Abstract:In this paper we discuss abundance ratios and their relation to stellar nucleosynthesis and other parameters of chemical evolution models, reviewing and clarifying the correct use of the observed abundance ratios in several astrophysical contexts. In particular, we start from the well-known fact that abundance ratios depend on stellar yields, initial mass function, and stellar lifetimes, and we show, by means of specific examples, that in some cases it is not correct to infer constraints on the contributions from different supernovae types (Ia, II), and particularly on different sets of yields, in the absence of a complete chemical evolution model taking into account stellar lifetimes. In spite of the fact that some of these results should be well known, we believe that it is useful to discuss the meaning of abundance ratios in the light of several recent claims based upon an incorrect interpretation of observed abundance ratios. In particular, the procedure, often used in the recent literature, of directly deriving conclusions about stellar nucleosynthesis just by relating abundance ratios to yield ratios implicitly assumes the instantaneous recycling approximation. This approximation is clearly not correct when one analyses the contributions of supernovae type Ia relative to supernovae type II as functions of cosmic time. In this paper we show that the uncertainty which arises from adopting this oversimplified procedure in a variety of astrophysical objects, such as elliptical galaxies, the intracluster medium, and high redshift objects, does not allow us to draw any firm conclusion, and that the differences between abundance ratios predicted by models with the instantaneous recycling approximation and models with detailed stellar lifetimes is of the same order as the differences between different sets of yields. On the other hand, if one is interested only in establishing the global metal production (e.g. galaxies plus intracluster medium) over the lifetime of the Universe, then the adoption of simplified arguments can be justified.

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SNe heating and the chemical evolution of the intra-cluster medium

Cited by 78 publications

References 74 publications

Metallicity map of the galaxy cluster A3667

Metallicity map of the galaxy cluster A3667

Cosmological formation and chemical evolution of an elliptical galaxy

Interpretation of Abundance Ratios

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