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A method for recovering the star formation history of resolved stellar populations

Published online by Cambridge University Press:  01 December 2006

M. Cignoni ,
S. Degl'Innocenti ,
P. G. Prada Moroni  and
S. N. Shore
M. Cignoni
Affiliation:
Dipartimento di Fisica, Università di Pisa, largo Pontecorvo 3, I-56127 Pisa, Italy email: [email protected] Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, I-40127 Bologna, Italy
S. Degl'Innocenti
Affiliation:
Dipartimento di Fisica, Università di Pisa, largo Pontecorvo 3, I-56127 Pisa, Italy email: [email protected] INFN – Sezione di Pisa, largo Pontecorvo 3, I-56127 Pisa, Italy
P. G. Prada Moroni
Affiliation:
Dipartimento di Fisica, Università di Pisa, largo Pontecorvo 3, I-56127 Pisa, Italy email: [email protected] INFN – Sezione di Pisa, largo Pontecorvo 3, I-56127 Pisa, Italy
S. N. Shore
Affiliation:
Dipartimento di Fisica, Università di Pisa, largo Pontecorvo 3, I-56127 Pisa, Italy email: [email protected] INFN – Sezione di Pisa, largo Pontecorvo 3, I-56127 Pisa, Italy
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Abstract

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A new method to extract information from color-magnitude diagrams (CMDs) is presented. We employ a Richardson-Lucy (RL) algorithm to the analysis of the observational uncertainties. The resulting reconstruction is a cleaned data set with which to perform analyses of the star formation history. For this task, synthetic stellar populations are built and compared with the data CMD. As an application, the star formation rate in the solar vicinity is recovered.

Keywords

Galaxy: solar neighborhooddiskstellar content(stars:) 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. 325 - 326
Copyright
Copyright © International Astronomical Union 2007

References

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