Marino, Raffaella Anna2023-06-192023-06-192014-08-101) Bell, E. F., de Jong, R. S., 2000, MNRAS, 312, 497. 2) Cid Fernandes, R., Asari, N. V., Sodré, L., et al., 2007, MNRAS, 375, L16. 3) Cid Fernandes, R., González Delgado, R. M., Pérez, E., et al,. 2014, A&A, 561, 130. 4) Cid Fernandes, R., Mateus, A., Sodré, L., Stasińska, G., Gomes, J. M., 2005, MNRAS, 358, 363. 5) Cid Fernandes, R., Pérez, E., García Benito, R., et al., 2013, A&A, 557, 86. 6) Faber, S. M., Jackson, R. E,. 1976, ApJ, 204, 668. 7) Fisher, D. B., Drory, N., 2011, ApJL, 733, L47. 8) Gallazzi, A., Charlot, S., Brinchmann, J., White, S. D. M., Tremonti, C. A., 2005, MNRAS, 362, 41. 9) González Delgado, R. M., Cerviño, M., Martins, L. P., Leitherer, C., Hauschildt, P. H., 2005, MNRAS, 357, 945. 10) González Delgado, R. M., Pérez, E., Cid Fernandes, R., et al., 2014, A&A, 562, 47. 11) Husemann, B., Jahnke, K., Sánchez, S. F., et al, 2013, A&A, 549, A87. 12) Iglesias-Páramo, J., Vílchez, J. M., Galbany, L., et al., 2013, A&A, 553, L7. 13) Mast, D., Rosales-Ortega, F. F., Sánchez, S. F., et al., 2014, A&A, 561, 129. 14) Panter, B., Jiménez, R., Heavens, A. F., Charlot, S., 2007, MNRAS, 378, 1550. 15) Panter, B., Jiménez, R., Heavens, A. F., Charlot, S., 2008, MNRAS, 391, 1117. 16) Pérez, E., Cid Fernandes, R., González Delgado, R. M., et al., 2013, ApJL, 764, L1. 17) Rosales-Ortega, F. F., Sánchez, S. F., Iglesias-Páramo, J., et al., 2012, ApJL, 756, L31. 18) Sánchez, S. F., Kennicutt, R. C., Gil de Paz, A., et al., 2012, A&A, 538, A8. 19) Sánchez, S. F., Rosales-Ortega, F. F., Jungwiert, B., et al,. 2013, A&A, 554, 58. 20) Schmidt, M., 1959, ApJ, 129, 243. 21) Tremonti, C. A., Heckman, T. M., Kauffmann, G., et al., 2004, ApJ, 613, 898. 22) Vazdekis, A., Sánchez-Blázquez, P., Falcón-Barroso, J., et al., 2010, MNRAS, 404, 1639. 23) Walcher, C. J., Wisotzki, L., Bekeraité, S., et al., 2014, A&A, in press (arXiv:1407.2939).2041-820510.1088/2041-8205/791/1/L16https://hdl.handle.net/20.500.14352/33910© 2014. The American Astronomical Society. This Letter is based on data obtained by the CALIFA survey (http://califa.caha.es), funded by the Spanish MINECO grants ICTS-2009-10, AYA2010-15081, and the CAHA operated jointly by the Max-Planck IfA and the IAA (CSIC). The CALIFA Collaboration thanks the CAHA staff for the dedication to this project. Support from CNPq (Brazil) through Programa Ciencia sem Fronteiras (401452 ˆ /2012-3) is duly acknowledged.We use spatially and temporally resolved maps of stellar population properties of 300 galaxies from the CALIFA integral field survey to investigate how the stellar metallicity (Z) relates to the total stellar mass (M) and the local mass surface density (μ) in both spheroidal- and disk-dominated galaxies. The galaxies are shown to follow a clear stellar mass–metallicity relation (MZR) over the hole 109–1012 M range. This relation is steeper than the one derived from nebular abundances, which is similar to the flatter stellar MZR derived when we consider only young stars. We also find a strong relation between the local values of μ and Z (the μZR), betraying the influence of local factors in determining Z. This shows that both local (μ-driven) and global (M-driven) processes are important in determining metallicity in galaxies. We find that the overall balance between local and global effects varies with the location within a galaxy. In disks, μ regulates Z, producing a strong μZR whose amplitude is modulated by M. In spheroids it is M that dominates the physics of star formation and chemical enrichment, with μ playing a minor, secondary role. These findings agree with our previous analysis of the star formation histories of CALIFA galaxies, which showed that mean stellar ages are mainly governed by surface density in galaxy disks and by total mass in spheroids.engjournal articlehttp://dx.doi.org/10.1088/2041-8205/791/1/L16http://iopscience.iop.org/open access52Digital sky surveyField area surveySpiral galaxiesEvolution.Astrofísica