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Chemodynamics of the Galaxies: From Cuspy to Dark Matter DensityProfiles and Metallicity Gradients

Published online by Cambridge University Press:  11 July 2011

M. Koleva ,
Ph. Prugniel ,
I. Vauglin ,
S. Pasetto ,
E.K. Grebel ,
P. Berczik ,
C. Chiosi ,
R. Spurzem  and
W. Dehnen
S. Pasetto
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Germany and Max-Planck-Institut für Astronomie, Heidelberg, Germany Max-Planck-Institut für Astronomie, Heidelberg, Germany
E.K. Grebel
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Germany
P. Berczik
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Germany; National Astronomical Observatories of China (NAOC), Chinese Academy of Sciences (CAS), Datun Lu 20A, Chaoyang District, Beijing 100012, China Main Astronomical Observatory (MAO), National Academy of Sciences of Ukraine (NASU), Akademika Zabolotnoho 27, 03680 Kyiv, Ukraine; Kavli Institute of Astronomy and Astrophysics, Peking University, Beijing, China
C. Chiosi
Affiliation:
Astronomic Department of the University of Padova, Vicolo dell’Osservatorio 32, Padova, Italy
R. Spurzem
Affiliation:
National Astronomical Observatories of China (NAOC), Chinese Academy of Sciences (CAS), Datun Lu 20A, Chaoyang District, Beijing 100012, China Kavli Institute of Astronomy and Astrophysics, Peking University, Beijing, China; Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Germany; Max-Planck-Institut für Astronomie, Heidelberg, Germany
W. Dehnen
Affiliation:
Department of Physics & Astronomy, University of Leicester, Leicester, LE1 7RH, UK
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Abstract

We follow the dynamical and chemical evolution of isolated systems tuned in their properties on selfgravitating spherical three component (gas+stars+dark matter) dwarf spheroidal galaxies (dSph). The system starts as a strongly dark matter dominated cuspy density profile. It is shown that after few Gyr of evolution the star formation processes are naturally able to reshape the cuspy dark matter profile into a flatter one. The same family of models is then evolved by orbiting in a Milky Way external potential in order to investigate the history of the Carina dwarf galaxy. Structural parameters and the star formation history of Carina are self-consistently determined in good agreement with the observations.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 48: CRAL-2010 A Universe of Dwarf Galaxies , 2011 , pp. 461 - 462
Copyright
© EAS, EDP Sciences, 2011

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References

Pasetto, S., Grebel, E.K., Berczik, P., Spurzem, R., & Dehnen, W., 2010, A&A, 514A, 47
Pasetto, S., Grebel, E.K., Berczik, P., Chiosi, C., & Spurzem, R., A&A, accepted
Rizzi, L., Held, E.V., Bertelli, G., & Saviane, I., 2003, ApJ, 589, L85CrossRef