CALIFA color/metallicity gradients connections Virtual Observatory Resource

  1. Marino R.A.
  2. Gil de Paz A.
  3. Sanchez S.F.
  4. Sanchez-Blazquez P.
  5. Cardiel N.
  6. Castillo-Morales A.
  7. Pascual S.
  8. Vilchez J.
  9. Kehrig C.
  10. Molla M.
  11. Mendez-Abreu J.
  12. Catalan-Torrecilla C.
  13. Florido E.
  14. Perez I.
  15. Ruiz-Lara T.
  16. Ellis S.
  17. Lopez-Sanchez A.R.
  18. Gonzalez Delgado R.M.
  19. De Lorenzo-Caceres A.
  20. Garcia-Benito R.
  21. Galbany L.
  22. Zibetti S.
  23. Cortijo C.
  24. Kalinova V.
  25. Mast D.
  26. Iglesias-Paramo J.
  27. Papaderos P.
  28. Walcher C.J.
  29. Bland-Hawthorn J.
  30. (the Califa Team)
  31. Published by

We study, for the first time in a statistically significant and well-defined sample, the relation between the outer-disk ionized-gas metallicity gradients and the presence of breaks in the surface brightness profiles of disk galaxies. Sloan Digital Sky Survey (SDSS) g'- and r'-band surface brightness, (g'-r') color, and ionized-gas oxygen abundance profiles for 324 galaxies within the Calar Alto Legacy Integral Field Area (CALIFA) survey are used for this purpose. We perform a detailed light-profile classification, finding that 84% of our disks show down- or up-bending profiles (Type II and Type III, respectively), while the remaining 16% are well fitted by one single exponential (Type I). The analysis of the color gradients at both sides of this break shows a U-shaped profile for most Type II galaxies with an average minimum (g'-r') color of ~0.5mag and an ionized-gas metallicity flattening associated with it only in the case of low-mass galaxies. Comparatively, more massive systems show a rather uniform negative metallicity gradient. The correlation between metallicity flattening and stellar mass for these systems results in p-values as low as 0.01. Independent of the mechanism having shaped the outer light profiles of these galaxies, stellar migration or a previous episode of star formation in a shrinking star-forming disk, it is clear that the imprint in their ionized-gas metallicity was different for low- and high-mass Type II galaxies. In the case of Type III disks, a positive correlation between the change in color and abundance gradient is found (the null hypothesis is ruled out with a p-value of 0.02), with the outer disks of Type III galaxies with masses <=10^10^M_{sun}_ showing a weak color reddening or even a bluing. This is interpreted as primarily due to a mass downsizing effect on the population of Type III galaxies that recently experienced an enhanced inside-out growth.

  1. Galaxies
  2. Photometry
  3. Optical astronomy
  4. Sloan photometry
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