Hostname: page-component-8448b6f56d-jr42d Total loading time: 0 Render date: 2024-04-19T13:29:52.240Z Has data issue: false hasContentIssue false
  • English
  • Français

Reconstructing the spatial distribution of the Galactic stellar halo

Published online by Cambridge University Press:  01 December 2006

M. Cignoni ,
V. Ripepi ,
M. Marconi ,
J. M. Alcalá ,
M. Capaccioli ,
M. Pannella  and
R. Silvotti
M. Cignoni
Affiliation:
Osservatorio Astronomico Di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy email: cignoni@df.unipi.it Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, I-40127 Bologna, Italy
V. Ripepi
Affiliation:
Osservatorio Astronomico Di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy email: cignoni@df.unipi.it
M. Marconi
Affiliation:
Osservatorio Astronomico Di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy email: cignoni@df.unipi.it
J. M. Alcalá
Affiliation:
Osservatorio Astronomico Di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy email: cignoni@df.unipi.it
M. Capaccioli
Affiliation:
Osservatorio Astronomico Di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy email: cignoni@df.unipi.it
M. Pannella
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, Postfach 1312, D-85741 Garching, Germany
R. Silvotti
Affiliation:
Osservatorio Astronomico Di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy email: cignoni@df.unipi.it
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The VLT Survey Telescope (VST) is going to offer a unique chance to collect deep and wide field photometry in multi-directions, opening the door to a definitive mapping of the Galactic halo. In this shortcoming scenario, we present a pilot study aimed at recovering the halo stellar density using the Capodimonte Deep Field (OACDF, Alcalá et al. 2004). Turn-off stars are isolated and the relative color-magnitude diagram (CMD) is compared with synthetic CMDs. Our result is consistent with a power law exponent n≈ 3 over a range of Galactocentric distances from 8 to 40 kpc.

Keywords

Galaxy: haloGalaxy: structureGalaxy: stellar contentStars: Hertzsprung-Russell diagramMethods: statistical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 237 - 238
Copyright
Copyright © International Astronomical Union 2007

References

Alcalá, J. M. et al. 2004, A&A, 428, 339Google Scholar
Cariulo, P., Degl'Innocenti, S., & Castellani, 2004, A&A, 421, 1121Google Scholar
Cignoni, M., Ripepi, V., Marconi, M., Alcalá, J. M., Capaccioli, M., Pannella, M., & Silvotti, R. 2006, A&A, DOI: 10.1051/0004-6361:20066598CrossRefGoogle Scholar