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Surface Brightness Fluctuations for constraining the chemical enrichment of massive galaxies

Published online by Cambridge University Press:  29 March 2021

A. Vazdekis Open the ORCID record for A. Vazdekis [Opens in a new window] ,
P. Rodrguez-Beltrán ,
M. Cerviño ,
M. Montes ,
I. Martn-Navarro  and
M. B. Beasley
A. Vazdekis
Affiliation:
Instituto de Astrofsica de Canarias, E-38200 La Laguna, Tenerife, Spain email: vazdekis@iac.es Departamento de Astrofsica, Universidad de La Laguna, E-38205, Tenerife, Spain
P. Rodrguez-Beltrán
Affiliation:
Instituto de Astrofsica de Canarias, E-38200 La Laguna, Tenerife, Spain email: vazdekis@iac.es Departamento de Astrofsica, Universidad de La Laguna, E-38205, Tenerife, Spain
M. Cerviño
Affiliation:
Centro de Astrobiologa (CSIC/INTA), ESAC Campus, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Spain
M. Montes
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia
I. Martn-Navarro
Affiliation:
Max-Planck Institut für Astronomie, Konigstuhl 17, D-69117 Heidelberg, Germany University of California Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA
M. B. Beasley
Affiliation:
Instituto de Astrofsica de Canarias, E-38200 La Laguna, Tenerife, Spain email: vazdekis@iac.es Departamento de Astrofsica, Universidad de La Laguna, E-38205, Tenerife, Spain
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Abstract

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Based on very deep photometry, Surface Brightness Fluctuations (SBF) have been traditionally used to determine galaxy distances. We have recently computed SBF spectra of stellar populations at moderately high resolution, which are fully based on empirical stars. We show that the SBF spectra provide an unprecedented potential for stellar population studies that, so far, have been tackled on the basis of the mean fluxes. We find that the SBFs are able to unveil metal-poor stellar components at the one percent level, which are not possible to disentangle with the standard analysis. As these metal-poor components correspond to the first stages of the chemical enrichment, the SBF analysis provides stringent constrains on the quenching epoch.

Keywords

galaxies: abundancesgalaxies: elliptical and lenticular, cDgalaxies: stellar contentgalaxies: distances and redshiftsgalaxies: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S359: Galaxy Evolution and Feedback across Different Environments , March 2019 , pp. 407 - 412
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

References

Blakeslee, J. P., Vazdekis, A., Ajhar, E. A., et al. 2001, Mnras, 320, 193 CrossRefGoogle Scholar
Blakeslee, J. P., Cantiello, M., Mei, S., et al. 2010, ApJ, 724, 657 CrossRefGoogle Scholar
Buzzoni, A. 1993, A&A, 275, 433 Google Scholar
Cenarro, A. J., Cardiel, N., Gorgas, J., et al. 2001a, Mnras, 326, 959 CrossRefGoogle Scholar
Cenarro, A. J., Moles, M., Cristóbal-Hornillos, D., et al. 2010, SPIE, 7738Google Scholar
Cantiello, M., Raimondo, G., Brocato, E., et al. 2003, AJ, 125, 2783 CrossRefGoogle Scholar
Cerviño, M. 2013, New Astron. Revs., 57, 123 CrossRefGoogle Scholar
Chabrier, G. 2001, ApJ, 554, 1274 CrossRefGoogle Scholar
Cushing, M. C., Raynier, J. T., Vacca, W. D., et al. 2005, ApJ, 623, 1115 CrossRefGoogle Scholar
Girardi, L., Bressan, A., Bertelli, G., et al. 2000, A&AS, 141, 371 Google Scholar
González Delgado, R. M., Cerviño, M., Martins, L. P., et al. 2005, Mnras, 357, 945 CrossRefGoogle Scholar
Gregg, M. D., Silva, D., Rayner, J., et al. 2006, in The 2005 HST Calibration Workshop: Hubble After the Transition to Two-Gyro Mode, ed. A. M. Koekemoer, P. Goudfrooij, & L. L. Dressel, 209–215Google Scholar
Kroupa, P. 2001, Mnras, 322, 231 CrossRefGoogle Scholar
Liu, M. C., Charlot, S., Graham, J. R., et al. 2000, ApJ, 543, 644 CrossRefGoogle Scholar
Mitzkus, M., Jakob Walcher, C. Roth, M. M., et al. 2018, Mnras, 480, 629 CrossRefGoogle Scholar
Pietrinferni, A., Cassisi, S., Salaris, M., et al. 2004, ApJ, 612, 168 CrossRefGoogle Scholar
Raynier, J. T., Cushing, M. C., Vacca, W. D., et al. 2009, ApJs, 185, 289 CrossRefGoogle Scholar
Renzini, A. 2006, ARAA, 44, 141 CrossRefGoogle Scholar
Sánchez-Blázquez, P., et al. Mnras, 371, 703 CrossRefGoogle Scholar
Tonry, J. & Schneider, D. P. 1988, AJ, 96, 807 CrossRefGoogle Scholar
Tonry, J. L., Ajhar, E. A., Luppino, G. A., et al. 1990, AJ, 100, 1416 CrossRefGoogle Scholar
Valdes, F., Gupta, R., Rose, J. A., et al. 2004, ApJs, 152, 251 CrossRefGoogle Scholar
Vazdekis, A., Casuso, E., Peletier, R. F., et al. 1996, ApJs, 106, 307 CrossRefGoogle Scholar
Vazdekis, A., Cerviño, M., Montes, M., et al. 2018, Mnras, 493, 5131 CrossRefGoogle Scholar
Worthey, G. 1994, ApJs, 95, 107 CrossRefGoogle Scholar