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Resolved maps of stellar mass and SED of galaxies from optical/NIR imaging and SPS models

Published online by Cambridge University Press:  13 April 2010

Stefano Zibetti ,
Stéphane Charlot  and
Hans-Walter Rix
Stefano Zibetti
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected], [email protected]
Stéphane Charlot
Affiliation:
Institut d'Astrophysique de Paris, CNRS, Université Pierre & Marie Curie, 98 bis Boulevard Arago, 75014 Paris, France email: [email protected]
Hans-Walter Rix
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected], [email protected]
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Abstract

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We report on the method developed by Zibetti, Charlot & Rix (2009) to construct resolved stellar mass maps of galaxies from optical and NIR imaging. Accurate pixel-by-pixel colour information (specifically g – i and i – H) is converted into stellar mass-to-light ratios with typical accuracy of 30%, based on median likelihoods derived from a Monte Carlo library of 50,000 stellar population synthesis models that include dust and updated TP-AGB phase prescriptions. Hence, surface mass densities are computed. In a pilot study, we analyze 9 galaxies spanning a broad range of morphologies. Among the main results, we find that: i) galaxies appear much smoother in stellar mass maps than at any optical or NIR wavelength; ii) total stellar mass estimates based on unresolved photometry are biased low with respect to the integral of resolved stellar mass maps, by up to 40%, due to dust obscured regions being under-represented in global colours; iii) within a galaxy, on local scales colours correlate with surface stellar mass density; iv) the slope and tightness of this correlation reflect/depend on the morphology of the galaxy.

Keywords

galaxies: general – galaxies: stellar content – galaxies: structure – galaxies: fundamental parameters – galaxies: photometry – techniques: photometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 89 - 92
Copyright
Copyright © International Astronomical Union 2010

References

Bell, E. F. & de Jong, R. S. 2000, MNRAS, 312, 497CrossRefGoogle Scholar
Bell, E. F. & de Jong, R. S. 2001, ApJ, 550, 212CrossRefGoogle Scholar
Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000CrossRefGoogle Scholar
Charlot, S. & Fall, S. M. 2000, ApJ, 539, 718CrossRefGoogle Scholar
Gavazzi, G., Boselli, A., Donati, A., Franzetti, P., & Scodeggio, M. 2003, A&A, 400, 451Google Scholar
Gavazzi, G., Pierini, D., & Boselli, A. 1996, A&A, 312, 397Google Scholar
Kauffmann, G. et al. , 2003, MNRAS, 341, 54CrossRefGoogle Scholar
Kennicutt, R. C. Jr. et al. 2003, PASP, 115, 928CrossRefGoogle Scholar
Lawrence, A. et al. 2007, MNRAS, 379, 1599CrossRefGoogle Scholar
Maraston, C. 2005, MNRAS, 362, 799CrossRefGoogle Scholar
Marigo, P., Girardi, L., Bressan, A., Groenewegen, M. A. T., Silva, L., & Granato, G. L. 2008, A&A, 482, 883Google Scholar
Scodeggio, M., Gavazzi, G., Franzetti, P., Boselli, A., Zibetti, S., & Pierini, D. 2002, A&A, 384, 812Google Scholar
Zibetti, S., Charlot, S., & Rix, H.-W. 2009, MNRAS in press, ArXiv:0904.4252Google Scholar