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About the Chemical Evolution of dSphs (and the peculiar Globular Cluster ω Cen)

Published online by Cambridge University Press:  01 June 2008

Andrea Marcolini  and
Annibale D'Ercole
Andrea Marcolini
Affiliation:
Centre for Astrophysics, University of Central Lancashire, Preston, Lancashire, PR1 2HE, United Kingdom email: amarcolini@uclan.ac.uk
Annibale D'Ercole
Affiliation:
INAF, Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy email: annibale.dercole@bo.astro.it
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Abstract

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We present three dimensional hydrodynamical simulations aimed at studying the dynamical and chemical evolution of the interstellar medium (ISM) in isolated dwarf spheroidal galaxies (dSphs). This evolution is driven by the explosion of Type II and Type Ia supernovae, whose different contribution on both the dynamics and chemical enrichment is taken into account. Radiative losses are effective in radiating away the huge amount of energy released by SNe explosions, and the dSph is able to retain most of the gas allowing a long period (≥ 2 − 3 Gyr) of star formation, as usually observed in this kind of galaxies. We are able to reproduce the stellar metallicity distribution function (MDF) as well as the peculiar chemical properties of strongly O-depleted stars observed in several dSphs. The model also naturally predicts two different stellar populations, with an anti-correlation between [Fe/H] and velocity dispersion, similarly to what observed in the Sculptor and Fornax dSphs. These results derive from the inhomogeneous pollution of the SNe Ia, a distinctive characteristic of our model. We also applied the model to the peculiar globular cluster (GC) ω Cen in the hypothesis that it is the remnant of a formerly larger stellar system, possibly a dSph.

Keywords

hydrodynamicsmethods: numericalstars: abundancesISM: evolutionISM: abundancesgalaxies: dwarf(Galaxy:) globular clusters: individual (ω Cen)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 152 - 156
Copyright
Copyright © International Astronomical Union 2008

References

Battaglia, G. et al. , 2006, A&A, 459, 423Google Scholar
Bekki, K. & Norris, J. E., 2006, ApJL, 637, L109CrossRefGoogle Scholar
Bellazzini, M., Ferraro, F. R., Origlia, L., Pancino, E., Monaco, L., & Oliva, E., 2002, AJ, 124, 3222CrossRefGoogle Scholar
Dekel, A. & Silk, J., 1986, ApJ, 303, 39CrossRefGoogle Scholar
de Jong, et al. , 2008, astro-ph/08014027Google Scholar
Fenner, Y., Gibson, B. K., Gallino, R., & Lugaro, M., 2006, ApJ, 646, 184CrossRefGoogle Scholar
Geisler, D., Wallerstein, G., Smith, V. V., & Casetti-Dinescu, D. I., 2007, PASP, 119, 939CrossRefGoogle Scholar
Haines, C., Gargiulo, A., La Barbera, F., Mercurio, A., Merluzzi, , & Busarello, , 2007, MNRAS, 381, 7CrossRefGoogle Scholar
Ikuta, C. & Arimoto, N., 2002, A&A, 391, 55Google Scholar
Johnson, C. I., Pilachowski, C. A., Simmerer, J., & Schwenk, D., astro-ph/08042607Google Scholar
Lanfranchi, G. A. & Matteucci, F., 2004, MNRAS, 351, 1338CrossRefGoogle Scholar
Marcolini, A., D'Ercole, A., Brighenti, F., & Recchi, S., 2006, MNRAS, 371, 643CrossRefGoogle Scholar
Marcolini, A., Sollima, A., D'Ercole, A., Gibson, B. K., & Ferraro, F. R., 2007, MNRAS, 382, 443CrossRefGoogle Scholar
Marcolini, A., D'Ercole, A., Battaglia, G., & Gibson B. K, 2008, MNRAS, 386, 2173CrossRefGoogle Scholar
Mateo, M. L., 1998, ARA&A, 36, 435Google Scholar
Matteucci, F. & Recchi, S., 2001, ApJ, 558, 351CrossRefGoogle Scholar
Mayer, L., Mastropietro, C., Wadsley, J., Stadel, J., & Moore, B., 2006, MNRAS, 369, 1021CrossRefGoogle Scholar
Norris, J. E., Freeman, K. C., & Mighell, K. J., 1996, ApJ, 462, 241CrossRefGoogle Scholar
Origlia, L., Ferraro, F. R., Bellazzini, M., & Pancino, E., 2003, ApJ, 591, 916CrossRefGoogle Scholar
Pancino, E., Pasquini, L., Hill, V., Ferraro, F. R., & Bellazzini, M., 2002, ApJ, 568, L101CrossRefGoogle Scholar
Recchi, S., Theis, C., Kroupa, P., & Hensler, G, 2007, A%A 470, 5Google Scholar
Salvadori, S., Ferrara, A., & Schneider, R., 2008, MNRAS, 386, 348CrossRefGoogle Scholar
Shetrone, M. D., Côté, P., & Sargent, W. L. W., 2001, ApJ, 548, 592CrossRefGoogle Scholar
Sollima, A., Ferraro, F. R., Pancino, E., & Bellazzini, M., 2005, MNRAS, 357, 265CrossRefGoogle Scholar
Stinson, G. S., Dalcanton, J. J., Quinn, T., Kaufmann, T., & Wadsley, J., 2007, ApJ, 667, 170CrossRefGoogle Scholar
Tolstoy, E., et al. 2004, ApJ, 617, L119CrossRefGoogle Scholar
van den Bergh, S., 1994, ApJ, 428, 617CrossRefGoogle Scholar
Young, L. M., Skillman, E. D., Weisz, D. R., & Dolphin, A. E., 2007, ApJ, 659, 331CrossRefGoogle Scholar