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Spectral synthesis of stellar populations in the 3D era: The CALIFA experience

Published online by Cambridge University Press:  09 February 2015

R. Cid Fernandes
Affiliation:
Departamento de Física, Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil email: cid@astro.ufsc, cid@br
E. A. D. Lacerda
Affiliation:
Departamento de Física, Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil email: cid@astro.ufsc, cid@br
R. M. González Delgado
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain
N. Vale Asari
Affiliation:
Departamento de Física, Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil email: cid@astro.ufsc, cid@br
R. García-Benito
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain
E. Pérez
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain
A. L. de Amorim
Affiliation:
Departamento de Física, Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil email: cid@astro.ufsc, cid@br
C. Cortijo-Ferrero
Affiliation:
Departamento de Física, Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil email: cid@astro.ufsc, cid@br
R. López Fernández
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain
S. F. Sánchez
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain Instituto de Astronomía, Universidad Nacional Autonóma de Mexico, D. F., México
Corresponding
E-mail address:
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Abstract

Methods to recover the fossil record of galaxy evolution encoded in their optical spectra have been instrumental in processing the avalanche of data from mega-surveys along the last decade, effectively transforming observed spectra onto a long and rich list of physical properties: from stellar masses and mean ages to full star formation histories. This promoted progress in our understanding of galaxies as a whole. Yet, the lack of spatial resolution introduces undesirable aperture effects, and hampers advances on the internal physics of galaxies. This is now changing with 3D surveys. The mapping of stellar populations in data-cubes allows us to figure what comes from where, unscrambling information previously available only in integrated form. This contribution uses our starlight-based analysis of 300 CALIFA galaxies to illustrate the power of spectral synthesis applied to data-cubes. The selected results highlighted here include: (a) The evolution of the mass-metallicity and mass-density-metallicity relations, as traced by the mean stellar metallicity. (b) A comparison of star formation rates obtained from Hα to those derived from full spectral fits. (c) The relation between star formation rate and dust optical depth within galaxies, which turns out to mimic the Schmidt-Kennicutt law. (d) PCA tomography experiments.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2015 

References

Asari, N. V., Cid Fernandes, R., Stasińska, G., et al. 2007, MNRAS, 381, 263CrossRefGoogle Scholar
Chen, X. Y., Liang, Y. C., Hammer, F., et al. 2010, A&A, 515, A101Google Scholar
Cid Fernandes, R., Pérez, E., García Benito, R., et al. 2013, A&A, 557, 86Google Scholar
Cid Fernandes, R., González Delgado, R. M., Pérez, E., et al. 2014, A&A, 561, 130Google Scholar
González Delgado, R. M., Pérez, E., Cid Fernandes, R., et al. 2014a, A&A, 562, 47Google Scholar
González Delgado, R. M., Cid Fernandes, R., García-Benito, R., et al. 2014b, ApJ, 791, L16CrossRefGoogle Scholar
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